Author: "Cristina Volpe" / Topic: physics - Searchworks@Jio Institute Digital Library Search Results

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52 results on '"Cristina Volpe"'

1. Radioactivity control strategy for the JUNO detector

Author: The JUNO collaboration, Angel Abusleme, Thomas Adam, Shakeel Ahmad, Rizwan Ahmed, Sebastiano Aiello, Muhammad Akram, Fengpeng An, Qi An, Giuseppe Andronico, Nikolay Anfimov, Vito Antonelli, Tatiana Antoshkina, Burin Asavapibhop, João Pedro Athayde Marcondes de André, Didier Auguste, Andrej Babic, Wander Baldini, Andrea Barresi, Davide Basilico, Eric Baussan, Marco Bellato, Antonio Bergnoli, Thilo Birkenfeld, Sylvie Blin, David Blum, Simon Blyth, Anastasia Bolshakova, Mathieu Bongrand, Clément Bordereau, Dominique Breton, Augusto Brigatti, Riccardo Brugnera, Riccardo Bruno, Antonio Budano, Mario Buscemi, Jose Busto, Ilya Butorov, Anatael Cabrera, Hao Cai, Xiao Cai, Yanke Cai, Zhiyan Cai, Antonio Cammi, Agustin Campeny, Chuanya Cao, Guofu Cao, Jun Cao, Rossella Caruso, Cédric Cerna, Jinfan Chang, Yun Chang, Pingping Chen, Po-An Chen, Shaomin Chen, Xurong Chen, Yi-Wen Chen, Yixue Chen, Yu Chen, Zhang Chen, Jie Cheng, Yaping Cheng, Alexey Chetverikov, Davide Chiesa, Pietro Chimenti, Artem Chukanov, Gérard Claverie, Catia Clementi, Barbara Clerbaux, Selma Conforti Di Lorenzo, Daniele Corti, Oliviero Cremonesi, Flavio Dal Corso, Olivia Dalager, Christophe De La Taille, Jiawei Deng, Zhi Deng, Ziyan Deng, Wilfried Depnering, Marco Diaz, Xuefeng Ding, Yayun Ding, Bayu Dirgantara, Sergey Dmitrievsky, Tadeas Dohnal, Dmitry Dolzhikov, Georgy Donchenko, Jianmeng Dong, Evgeny Doroshkevich, Marcos Dracos, Frédéric Druillole, Shuxian Du, Stefano Dusini, Martin Dvorak, Timo Enqvist, Heike Enzmann, Andrea Fabbri, Lukas Fajt, Donghua Fan, Lei Fan, Jian Fang, Wenxing Fang, Marco Fargetta, Dmitry Fedoseev, Vladko Fekete, Li-Cheng Feng, Qichun Feng, Richard Ford, Andrey Formozov, Amélie Fournier, Haonan Gan, Feng Gao, Alberto Garfagnini, Marco Giammarchi, Agnese Giaz, Nunzio Giudice, Maxim Gonchar, Guanghua Gong, Hui Gong, Yuri Gornushkin, Alexandre Göttel, Marco Grassi, Christian Grewing, Vasily Gromov, Minghao Gu, Xiaofei Gu, Yu Gu, Mengyun Guan, Nunzio Guardone, Maria Gul, Cong Guo, Jingyuan Guo, Wanlei Guo, Xinheng Guo, Yuhang Guo, Paul Hackspacher, Caren Hagner, Ran Han, Yang Han, Muhammad Sohaib Hassan, Miao He, Wei He, Tobias Heinz, Patrick Hellmuth, Yuekun Heng, Rafael Herrera, YuenKeung Hor, Shaojing Hou, Yee Hsiung, Bei-Zhen Hu, Hang Hu, Jianrun Hu, Jun Hu, Shouyang Hu, Tao Hu, Zhuojun Hu, Chunhao Huang, Guihong Huang, Hanxiong Huang, Wenhao Huang, Xin Huang, Xingtao Huang, Yongbo Huang, Jiaqi Hui, Lei Huo, Wenju Huo, Cédric Huss, Safeer Hussain, Ara Ioannisian, Roberto Isocrate, Beatrice Jelmini, Kuo-Lun Jen, Ignacio Jeria, Xiaolu Ji, Xingzhao Ji, Huihui Jia, Junji Jia, Siyu Jian, Di Jiang, Xiaoshan Jiang, Ruyi Jin, Xiaoping Jing, Cécile Jollet, Jari Joutsenvaara, Sirichok Jungthawan, Leonidas Kalousis, Philipp Kampmann, Li Kang, Rebin Karaparambil, Narine Kazarian, Waseem Khan, Khanchai Khosonthongkee, Denis Korablev, Konstantin Kouzakov, Alexey Krasnoperov, Andre Kruth, Nikolay Kutovskiy, Pasi Kuusiniemi, Tobias Lachenmaier, Cecilia Landini, Sébastien Leblanc, Victor Lebrin, Frederic Lefevre, Ruiting Lei, Rupert Leitner, Jason Leung, Demin Li, Fei Li, Fule Li, Haitao Li, Huiling Li, Jiaqi Li, Mengzhao Li, Min Li, Nan Li, Qingjiang Li, Ruhui Li, Shanfeng Li, Tao Li, Weidong Li, Weiguo Li, Xiaomei Li, Xiaonan Li, Xinglong Li, Yi Li, Yufeng Li, Zhaohan Li, Zhibing Li, Ziyuan Li, Hao Liang, Jiajun Liao, Daniel Liebau, Ayut Limphirat, Sukit Limpijumnong, Guey-Lin Lin, Shengxin Lin, Tao Lin, Jiajie Ling, Ivano Lippi, Fang Liu, Haidong Liu, Hongbang Liu, Hongjuan Liu, Hongtao Liu, Hui Liu, Jianglai Liu, Jinchang Liu, Min Liu, Qian Liu, Qin Liu, Runxuan Liu, Shuangyu Liu, Shubin Liu, Shulin Liu, Xiaowei Liu, Xiwen Liu, Yan Liu, Yunzhe Liu, Alexey Lokhov, Paolo Lombardi, Claudio Lombardo, Kai Loo, Chuan Lu, Haoqi Lu, Jingbin Lu, Junguang Lu, Shuxiang Lu, Xiaoxu Lu, Bayarto Lubsandorzhiev, Sultim Lubsandorzhiev, Livia Ludhova, Fengjiao Luo, Guang Luo, Pengwei Luo, Shu Luo, Wuming Luo, Vladimir Lyashuk, Bangzheng Ma, Qiumei Ma, Si Ma, Xiaoyan Ma, Xubo Ma, Jihane Maalmi, Yury Malyshkin, Fabio Mantovani, Francesco Manzali, Xin Mao, Yajun Mao, Stefano M. Mari, Filippo Marini, Sadia Marium, Cristina Martellini, Gisele Martin-Chassard, Agnese Martini, Matthias Mayer, Davit Mayilyan, Ints Mednieks, Yue Meng, Anselmo Meregaglia, Emanuela Meroni, David Meyhöfer, Mauro Mezzetto, Jonathan Miller, Lino Miramonti, Paolo Montini, Michele Montuschi, Axel Müller, Massimiliano Nastasi, Dmitry V. Naumov, Elena Naumova, Diana Navas-Nicolas, Igor Nemchenok, Minh Thuan Nguyen Thi, Feipeng Ning, Zhe Ning, Hiroshi Nunokawa, Lothar Oberauer, Juan Pedro Ochoa-Ricoux, Alexander Olshevskiy, Domizia Orestano, Fausto Ortica, Rainer Othegraven, Hsiao-Ru Pan, Alessandro Paoloni, Sergio Parmeggiano, Yatian Pei, Nicomede Pelliccia, Anguo Peng, Haiping Peng, Frédéric Perrot, Pierre-Alexandre Petitjean, Fabrizio Petrucci, Oliver Pilarczyk, Luis Felipe Piñeres Rico, Artyom Popov, Pascal Poussot, Wathan Pratumwan, Ezio Previtali, Fazhi Qi, Ming Qi, Sen Qian, Xiaohui Qian, Zhen Qian, Hao Qiao, Zhonghua Qin, Shoukang Qiu, Muhammad Usman Rajput, Gioacchino Ranucci, Neill Raper, Alessandra Re, Henning Rebber, Abdel Rebii, Bin Ren, Jie Ren, Barbara Ricci, Markus Robens, Mathieu Roche, Narongkiat Rodphai, Aldo Romani, Bedřich Roskovec, Christian Roth, Xiangdong Ruan, Xichao Ruan, Saroj Rujirawat, Arseniy Rybnikov, Andrey Sadovsky, Paolo Saggese, Simone Sanfilippo, Anut Sangka, Nuanwan Sanguansak, Utane Sawangwit, Julia Sawatzki, Fatma Sawy, Michaela Schever, Cédric Schwab, Konstantin Schweizer, Alexandr Selyunin, Andrea Serafini, Giulio Settanta, Mariangela Settimo, Zhuang Shao, Vladislav Sharov, Arina Shaydurova, Jingyan Shi, Yanan Shi, Vitaly Shutov, Andrey Sidorenkov, Fedor Šimkovic, Chiara Sirignano, Jaruchit Siripak, Monica Sisti, Maciej Slupecki, Mikhail Smirnov, Oleg Smirnov, Thiago Sogo-Bezerra, Sergey Sokolov, Julanan Songwadhana, Boonrucksar Soonthornthum, Albert Sotnikov, Ondřej Šrámek, Warintorn Sreethawong, Achim Stahl, Luca Stanco, Konstantin Stankevich, Dušan Štefánik, Hans Steiger, Jochen Steinmann, Tobias Sterr, Matthias Raphael Stock, Virginia Strati, Alexander Studenikin, Shifeng Sun, Xilei Sun, Yongjie Sun, Yongzhao Sun, Narumon Suwonjandee, Michal Szelezniak, Jian Tang, Qiang Tang, Quan Tang, Xiao Tang, Alexander Tietzsch, Igor Tkachev, Tomas Tmej, Konstantin Treskov, Andrea Triossi, Giancarlo Troni, Wladyslaw Trzaska, Cristina Tuve, Nikita Ushakov, Johannes van den Boom, Stefan van Waasen, Guillaume Vanroyen, Nikolaos Vassilopoulos, Vadim Vedin, Giuseppe Verde, Maxim Vialkov, Benoit Viaud, Moritz Cornelius Vollbrecht, Cristina Volpe, Vit Vorobel, Dmitriy Voronin, Lucia Votano, Pablo Walker, Caishen Wang, Chung-Hsiang Wang, En Wang, Guoli Wang, Jian Wang, Jun Wang, Kunyu Wang, Lu Wang, Meifen Wang, Meng Wang, Ruiguang Wang, Siguang Wang, Wei Wang, Wenshuai Wang, Xi Wang, Xiangyue Wang, Yangfu Wang, Yaoguang Wang, Yi Wang, Yifang Wang, Yuanqing Wang, Yuman Wang, Zhe Wang, Zheng Wang, Zhimin Wang, Zongyi Wang, Muhammad Waqas, Apimook Watcharangkool, Lianghong Wei, Wei Wei, Wenlu Wei, Yadong Wei, Liangjian Wen, Christopher Wiebusch, Steven Chan-Fai Wong, Bjoern Wonsak, Diru Wu, Fangliang Wu, Qun Wu, Zhi Wu, Michael Wurm, Jacques Wurtz, Christian Wysotzki, Yufei Xi, Dongmei Xia, Xiaochuan Xie, Yuguang Xie, Zhangquan Xie, Zhizhong Xing, Benda Xu, Cheng Xu, Donglian Xu, Fanrong Xu, Hangkun Xu, Jilei Xu, Jing Xu, Meihang Xu, Yin Xu, Yu Xu, Baojun Yan, Taylor Yan, Wenqi Yan, Xiongbo Yan, Yupeng Yan, Anbo Yang, Changgen Yang, Chengfeng Yang, Huan Yang, Jie Yang, Lei Yang, Xiaoyu Yang, Yifan Yang, Haifeng Yao, Zafar Yasin, Jiaxuan Ye, Mei Ye, Ziping Ye, Ugur Yegin, Frédéric Yermia, Peihuai Yi, Na Yin, Xiangwei Yin, Zhengyun You, Boxiang Yu, Chiye Yu, Chunxu Yu, Hongzhao Yu, Miao Yu, Xianghui Yu, Zeyuan Yu, Zezhong Yu, Chengzhuo Yuan, Ying Yuan, Zhenxiong Yuan, Ziyi Yuan, Baobiao Yue, Noman Zafar, Andre Zambanini, Vitalii Zavadskyi, Shan Zeng, Tingxuan Zeng, Yuda Zeng, Liang Zhan, Aiqiang Zhang, Feiyang Zhang, Guoqing Zhang, Haiqiong Zhang, Honghao Zhang, Jiawen Zhang, Jie Zhang, Jin Zhang, Jingbo Zhang, Jinnan Zhang, Peng Zhang, Qingmin Zhang, Shiqi Zhang, Shu Zhang, Tao Zhang, Xiaomei Zhang, Xuantong Zhang, Xueyao Zhang, Yan Zhang, Yinhong Zhang, Yiyu Zhang, Yongpeng Zhang, Yuanyuan Zhang, Yumei Zhang, Zhenyu Zhang, Zhijian Zhang, Fengyi Zhao, Jie Zhao, Rong Zhao, Shujun Zhao, Tianchi Zhao, Dongqin Zheng, Hua Zheng, Minshan Zheng, Yangheng Zheng, Weirong Zhong, Jing Zhou, Li Zhou, Nan Zhou, Shun Zhou, Tong Zhou, Xiang Zhou, Jiang Zhu, Kangfu Zhu, Kejun Zhu, Zhihang Zhu, Bo Zhuang, Honglin Zhuang, Liang Zong, Jiaheng Zou, Abusleme, A, Adam, T, Ahmad, S, Ahmed, R, Aiello, S, Akram, M, An, F, An, Q, Andronico, G, Anfimov, N, Antonelli, V, Antoshkina, T, Asavapibhop, B, de Andre, J, Auguste, D, Babic, A, Baldini, W, Barresi, A, Basilico, D, Baussan, E, Bellato, M, Bergnoli, A, Birkenfeld, T, Blin, S, Blum, D, Blyth, S, Bolshakova, A, Bongrand, M, Bordereau, C, Breton, D, Brigatti, A, Brugnera, R, Bruno, R, Budano, A, Buscemi, M, Busto, J, Butorov, I, Cabrera, A, Cai, H, Cai, X, Cai, Y, Cai, Z, Cammi, A, Campeny, A, Cao, C, Cao, G, Cao, J, Caruso, R, Cerna, C, Chang, J, Chang, Y, Chen, P, Chen, S, Chen, X, Chen, Y, Chen, Z, Cheng, J, Cheng, Y, Chetverikov, A, Chiesa, D, Chimenti, P, Chukanov, A, Claverie, G, Clementi, C, Clerbaux, B, Conforti Di Lorenzo, S, Corti, D, Cremonesi, O, Dal Corso, F, Dalager, O, De La Taille, C, Deng, J, Deng, Z, Depnering, W, Diaz, M, Ding, X, Ding, Y, Dirgantara, B, Dmitrievsky, S, Dohnal, T, Dolzhikov, D, Donchenko, G, Dong, J, Doroshkevich, E, Dracos, M, Druillole, F, Du, S, Dusini, S, Dvorak, M, Enqvist, T, Enzmann, H, Fabbri, A, Fajt, L, Fan, D, Fan, L, Fang, J, Fang, W, Fargetta, M, Fedoseev, D, Fekete, V, Feng, L, Feng, Q, Ford, R, Formozov, A, Fournier, A, Gan, H, Gao, F, Garfagnini, A, Giammarchi, M, Giaz, A, Giudice, N, Gonchar, M, Gong, G, Gong, H, Gornushkin, Y, Gottel, A, Grassi, M, Grewing, C, Gromov, V, Gu, M, Gu, X, Gu, Y, Guan, M, Guardone, N, Gul, M, Guo, C, Guo, J, Guo, W, Guo, X, Guo, Y, Hackspacher, P, Hagner, C, Han, R, Han, Y, Hassan, M, He, M, He, W, Heinz, T, Hellmuth, P, Heng, Y, Herrera, R, Hor, Y, Hou, S, Hsiung, Y, Hu, B, Hu, H, Hu, J, Hu, S, Hu, T, Hu, Z, Huang, C, Huang, G, Huang, H, Huang, W, Huang, X, Huang, Y, Hui, J, Huo, L, Huo, W, Huss, C, Hussain, S, Ioannisian, A, Isocrate, R, Jelmini, B, Jen, K, Jeria, I, Ji, X, Jia, H, Jia, J, Jian, S, Jiang, D, Jiang, X, Jin, R, Jing, X, Jollet, C, Joutsenvaara, J, Jungthawan, S, Kalousis, L, Kampmann, P, Kang, L, Karaparambil, R, Kazarian, N, Khan, W, Khosonthongkee, K, Korablev, D, Kouzakov, K, Krasnoperov, A, Kruth, A, Kutovskiy, N, Kuusiniemi, P, Lachenmaier, T, Landini, C, Leblanc, S, Lebrin, V, Lefevre, F, Lei, R, Leitner, R, Leung, J, Li, D, Li, F, Li, H, Li, J, Li, M, Li, N, Li, Q, Li, R, Li, S, Li, T, Li, W, Li, X, Li, Y, Li, Z, Liang, H, Liao, J, Liebau, D, Limphirat, A, Limpijumnong, S, Lin, G, Lin, S, Lin, T, Ling, J, Lippi, I, Liu, F, Liu, H, Liu, J, Liu, M, Liu, Q, Liu, R, Liu, S, Liu, X, Liu, Y, Lokhov, A, Lombardi, P, Lombardo, C, Loo, K, Lu, C, Lu, H, Lu, J, Lu, S, Lu, X, Lubsandorzhiev, B, Lubsandorzhiev, S, Ludhova, L, Luo, F, Luo, G, Luo, P, Luo, S, Luo, W, Lyashuk, V, Ma, B, Ma, Q, Ma, S, Ma, X, Maalmi, J, Malyshkin, Y, Mantovani, F, Manzali, F, Mao, X, Mao, Y, Mari, S, Marini, F, Marium, S, Martellini, C, Martin-Chassard, G, Martini, A, Mayer, M, Mayilyan, D, Mednieks, I, Meng, Y, Meregaglia, A, Meroni, E, Meyhofer, D, Mezzetto, M, Miller, J, Miramonti, L, Montini, P, Montuschi, M, Muller, A, Nastasi, M, Naumov, D, Naumova, E, Navas-Nicolas, D, Nemchenok, I, Nguyen Thi, M, Ning, F, Ning, Z, Nunokawa, H, Oberauer, L, Ochoa-Ricoux, J, Olshevskiy, A, Orestano, D, Ortica, F, Othegraven, R, Pan, H, Paoloni, A, Parmeggiano, S, Pei, Y, Pelliccia, N, Peng, A, Peng, H, Perrot, F, Petitjean, P, Petrucci, F, Pilarczyk, O, Pineres Rico, L, Popov, A, Poussot, P, Pratumwan, W, Previtali, E, Qi, F, Qi, M, Qian, S, Qian, X, Qian, Z, Qiao, H, Qin, Z, Qiu, S, Rajput, M, Ranucci, G, Raper, N, Re, A, Rebber, H, Rebii, A, Ren, B, Ren, J, Ricci, B, Robens, M, Roche, M, Rodphai, N, Romani, A, Roskovec, B, Roth, C, Ruan, X, Rujirawat, S, Rybnikov, A, Sadovsky, A, Saggese, P, Sanfilippo, S, Sangka, A, Sanguansak, N, Sawangwit, U, Sawatzki, J, Sawy, F, Schever, M, Schwab, C, Schweizer, K, Selyunin, A, Serafini, A, Settanta, G, Settimo, M, Shao, Z, Sharov, V, Shaydurova, A, Shi, J, Shi, Y, Shutov, V, Sidorenkov, A, Simkovic, F, Sirignano, C, Siripak, J, Sisti, M, Slupecki, M, Smirnov, M, Smirnov, O, Sogo-Bezerra, T, Sokolov, S, Songwadhana, J, Soonthornthum, B, Sotnikov, A, Sramek, O, Sreethawong, W, Stahl, A, Stanco, L, Stankevich, K, Stefanik, D, Steiger, H, Steinmann, J, Sterr, T, Stock, M, Strati, V, Studenikin, A, Sun, S, Sun, X, Sun, Y, Suwonjandee, N, Szelezniak, M, Tang, J, Tang, Q, Tang, X, Tietzsch, A, Tkachev, I, Tmej, T, Treskov, K, Triossi, A, Troni, G, Trzaska, W, Tuve, C, Ushakov, N, van den Boom, J, van Waasen, S, Vanroyen, G, Vassilopoulos, N, Vedin, V, Verde, G, Vialkov, M, Viaud, B, Vollbrecht, M, Volpe, C, Vorobel, V, Voronin, D, Votano, L, Walker, P, Wang, C, Wang, E, Wang, G, Wang, J, Wang, K, Wang, L, Wang, M, Wang, R, Wang, S, Wang, W, Wang, X, Wang, Y, Wang, Z, Waqas, M, Watcharangkool, A, Wei, L, Wei, W, Wei, Y, Wen, L, Wiebusch, C, Wong, S, Wonsak, B, Wu, D, Wu, F, Wu, Q, Wu, Z, Wurm, M, Wurtz, J, Wysotzki, C, Xi, Y, Xia, D, Xie, X, Xie, Y, Xie, Z, Xing, Z, Xu, B, Xu, C, Xu, D, Xu, F, Xu, H, Xu, J, Xu, M, Xu, Y, Yan, B, Yan, T, Yan, W, Yan, X, Yan, Y, Yang, A, Yang, C, Yang, H, Yang, J, Yang, L, Yang, X, Yang, Y, Yao, H, Yasin, Z, Ye, J, Ye, M, Ye, Z, Yegin, U, Yermia, F, Yi, P, Yin, N, Yin, X, You, Z, Yu, B, Yu, C, Yu, H, Yu, M, Yu, X, Yu, Z, Yuan, C, Yuan, Y, Yuan, Z, Yue, B, Zafar, N, Zambanini, A, Zavadskyi, V, Zeng, S, Zeng, T, Zeng, Y, Zhan, L, Zhang, A, Zhang, F, Zhang, G, Zhang, H, Zhang, J, Zhang, P, Zhang, Q, Zhang, S, Zhang, T, Zhang, X, Zhang, Y, Zhang, Z, Zhao, F, Zhao, J, Zhao, R, Zhao, S, Zhao, T, Zheng, D, Zheng, H, Zheng, M, Zheng, Y, Zhong, W, Zhou, J, Zhou, L, Zhou, N, Zhou, S, Zhou, T, Zhou, X, Zhu, J, Zhu, K, Zhu, Z, Zhuang, B, Zhuang, H, Zong, L, Zou, J, Abusleme, Angel, Adam, Thoma, Ahmad, Shakeel, Ahmed, Rizwan, Aiello, Sebastiano, Akram, Muhammad, An, Fengpeng, An, Qi, Andronico, Giuseppe, Anfimov, Nikolay, Antonelli, Vito, Antoshkina, Tatiana, Asavapibhop, Burin, de André, João Pedro Athayde Marconde, Auguste, Didier, Babic, Andrej, Baldini, Wander, Barresi, Andrea, Basilico, Davide, Baussan, Eric, Bellato, Marco, Bergnoli, Antonio, Birkenfeld, Thilo, Blin, Sylvie, Blum, David, Blyth, Simon, Bolshakova, Anastasia, Bongrand, Mathieu, Bordereau, Clément, Breton, Dominique, Brigatti, Augusto, Brugnera, Riccardo, Bruno, Riccardo, Budano, Antonio, Buscemi, Mario, Busto, Jose, Butorov, Ilya, Cabrera, Anatael, Cai, Hao, Cai, Xiao, Cai, Yanke, Cai, Zhiyan, Cammi, Antonio, Campeny, Agustin, Cao, Chuanya, Cao, Guofu, Cao, Jun, Caruso, Rossella, Cerna, Cédric, Chang, Jinfan, Chang, Yun, Chen, Pingping, Chen, Po-An, Chen, Shaomin, Chen, Xurong, Chen, Yi-Wen, Chen, Yixue, Chen, Yu, Chen, Zhang, Cheng, Jie, Cheng, Yaping, Chetverikov, Alexey, Chiesa, Davide, Chimenti, Pietro, Chukanov, Artem, Claverie, Gérard, Clementi, Catia, Clerbaux, Barbara, Conforti Di Lorenzo, Selma, Corti, Daniele, Cremonesi, Oliviero, Dal Corso, Flavio, Dalager, Olivia, De La Taille, Christophe, Deng, Jiawei, Deng, Zhi, Deng, Ziyan, Depnering, Wilfried, Diaz, Marco, Ding, Xuefeng, Ding, Yayun, Dirgantara, Bayu, Dmitrievsky, Sergey, Dohnal, Tadea, Dolzhikov, Dmitry, Donchenko, Georgy, Dong, Jianmeng, Doroshkevich, Evgeny, Dracos, Marco, Druillole, Frédéric, Du, Shuxian, Dusini, Stefano, Dvorak, Martin, Enqvist, Timo, Enzmann, Heike, Fabbri, Andrea, Fajt, Luka, Fan, Donghua, Fan, Lei, Fang, Jian, Fang, Wenxing, Fargetta, Marco, Fedoseev, Dmitry, Fekete, Vladko, Feng, Li-Cheng, Feng, Qichun, Ford, Richard, Formozov, Andrey, Fournier, Amélie, Gan, Haonan, Gao, Feng, Garfagnini, Alberto, Giammarchi, Marco, Giaz, Agnese, Giudice, Nunzio, Gonchar, Maxim, Gong, Guanghua, Gong, Hui, Gornushkin, Yuri, Göttel, Alexandre, Grassi, Marco, Grewing, Christian, Gromov, Vasily, Gu, Minghao, Gu, Xiaofei, Gu, Yu, Guan, Mengyun, Guardone, Nunzio, Gul, Maria, Guo, Cong, Guo, Jingyuan, Guo, Wanlei, Guo, Xinheng, Guo, Yuhang, Hackspacher, Paul, Hagner, Caren, Han, Ran, Han, Yang, Hassan, Muhammad Sohaib, He, Miao, He, Wei, Heinz, Tobia, Hellmuth, Patrick, Heng, Yuekun, Herrera, Rafael, Hor, Yuenkeung, Hou, Shaojing, Hsiung, Yee, Hu, Bei-Zhen, Hu, Hang, Hu, Jianrun, Hu, Jun, Hu, Shouyang, Hu, Tao, Hu, Zhuojun, Huang, Chunhao, Huang, Guihong, Huang, Hanxiong, Huang, Wenhao, Huang, Xin, Huang, Xingtao, Huang, Yongbo, Hui, Jiaqi, Huo, Lei, Huo, Wenju, Huss, Cédric, Hussain, Safeer, Ioannisian, Ara, Isocrate, Roberto, Jelmini, Beatrice, Jen, Kuo-Lun, Jeria, Ignacio, Ji, Xiaolu, Ji, Xingzhao, Jia, Huihui, Jia, Junji, Jian, Siyu, Jiang, Di, Jiang, Xiaoshan, Jin, Ruyi, Jing, Xiaoping, Jollet, Cécile, Joutsenvaara, Jari, Jungthawan, Sirichok, Kalousis, Leonida, Kampmann, Philipp, Kang, Li, Karaparambil, Rebin, Kazarian, Narine, Khan, Waseem, Khosonthongkee, Khanchai, Korablev, Deni, Kouzakov, Konstantin, Krasnoperov, Alexey, Kruth, Andre, Kutovskiy, Nikolay, Kuusiniemi, Pasi, Lachenmaier, Tobia, Landini, Cecilia, Leblanc, Sébastien, Lebrin, Victor, Lefevre, Frederic, Lei, Ruiting, Leitner, Rupert, Leung, Jason, Li, Demin, Li, Fei, Li, Fule, Li, Haitao, Li, Huiling, Li, Jiaqi, Li, Mengzhao, Li, Min, Li, Nan, Li, Qingjiang, Li, Ruhui, Li, Shanfeng, Li, Tao, Li, Weidong, Li, Weiguo, Li, Xiaomei, Li, Xiaonan, Li, Xinglong, Li, Yi, Li, Yufeng, Li, Zhaohan, Li, Zhibing, Li, Ziyuan, Liang, Hao, Liao, Jiajun, Liebau, Daniel, Limphirat, Ayut, Limpijumnong, Sukit, Lin, Guey-Lin, Lin, Shengxin, Lin, Tao, Ling, Jiajie, Lippi, Ivano, Liu, Fang, Liu, Haidong, Liu, Hongbang, Liu, Hongjuan, Liu, Hongtao, Liu, Hui, Liu, Jianglai, Liu, Jinchang, Liu, Min, Liu, Qian, Liu, Qin, Liu, Runxuan, Liu, Shuangyu, Liu, Shubin, Liu, Shulin, Liu, Xiaowei, Liu, Xiwen, Liu, Yan, Liu, Yunzhe, Lokhov, Alexey, Lombardi, Paolo, Lombardo, Claudio, Loo, Kai, Lu, Chuan, Lu, Haoqi, Lu, Jingbin, Lu, Junguang, Lu, Shuxiang, Lu, Xiaoxu, Lubsandorzhiev, Bayarto, Lubsandorzhiev, Sultim, Ludhova, Livia, Luo, Fengjiao, Luo, Guang, Luo, Pengwei, Luo, Shu, Luo, Wuming, Lyashuk, Vladimir, Ma, Bangzheng, Ma, Qiumei, Ma, Si, Ma, Xiaoyan, Ma, Xubo, Maalmi, Jihane, Malyshkin, Yury, Mantovani, Fabio, Manzali, Francesco, Mao, Xin, Mao, Yajun, Mari, Stefano M., Marini, Filippo, Marium, Sadia, Martellini, Cristina, Martin-Chassard, Gisele, Martini, Agnese, Mayer, Matthia, Mayilyan, Davit, Mednieks, Int, Meng, Yue, Meregaglia, Anselmo, Meroni, Emanuela, Meyhöfer, David, Mezzetto, Mauro, Miller, Jonathan, Miramonti, Lino, Montini, Paolo, Montuschi, Michele, Müller, Axel, Nastasi, Massimiliano, Naumov, Dmitry V., Naumova, Elena, Navas-Nicolas, Diana, Nemchenok, Igor, Nguyen Thi, Minh Thuan, Ning, Feipeng, Ning, Zhe, Nunokawa, Hiroshi, Oberauer, Lothar, Ochoa-Ricoux, Juan Pedro, Olshevskiy, Alexander, Orestano, Domizia, Ortica, Fausto, Othegraven, Rainer, Pan, Hsiao-Ru, Paoloni, Alessandro, Parmeggiano, Sergio, Pei, Yatian, Pelliccia, Nicomede, Peng, Anguo, Peng, Haiping, Perrot, Frédéric, Petitjean, Pierre-Alexandre, Petrucci, Fabrizio, Pilarczyk, Oliver, Piñeres Rico, Luis Felipe, Popov, Artyom, Poussot, Pascal, Pratumwan, Wathan, Previtali, Ezio, Qi, Fazhi, Qi, Ming, Qian, Sen, Qian, Xiaohui, Qian, Zhen, Qiao, Hao, Qin, Zhonghua, Qiu, Shoukang, Rajput, Muhammad Usman, Ranucci, Gioacchino, Raper, Neill, Re, Alessandra, Rebber, Henning, Rebii, Abdel, Ren, Bin, Ren, Jie, Ricci, Barbara, Robens, Marku, Roche, Mathieu, Rodphai, Narongkiat, Romani, Aldo, Roskovec, Bedřich, Roth, Christian, Ruan, Xiangdong, Ruan, Xichao, Rujirawat, Saroj, Rybnikov, Arseniy, Sadovsky, Andrey, Saggese, Paolo, Sanfilippo, Simone, Sangka, Anut, Sanguansak, Nuanwan, Sawangwit, Utane, Sawatzki, Julia, Sawy, Fatma, Schever, Michaela, Schwab, Cédric, Schweizer, Konstantin, Selyunin, Alexandr, Serafini, Andrea, Settanta, Giulio, Settimo, Mariangela, Shao, Zhuang, Sharov, Vladislav, Shaydurova, Arina, Shi, Jingyan, Shi, Yanan, Shutov, Vitaly, Sidorenkov, Andrey, Šimkovic, Fedor, Sirignano, Chiara, Siripak, Jaruchit, Sisti, Monica, Slupecki, Maciej, Smirnov, Mikhail, Smirnov, Oleg, Sogo-Bezerra, Thiago, Sokolov, Sergey, Songwadhana, Julanan, Soonthornthum, Boonrucksar, Sotnikov, Albert, Šrámek, Ondřej, Sreethawong, Warintorn, Stahl, Achim, Stanco, Luca, Stankevich, Konstantin, Štefánik, Dušan, Steiger, Han, Steinmann, Jochen, Sterr, Tobia, Stock, Matthias Raphael, Strati, Virginia, Studenikin, Alexander, Sun, Shifeng, Sun, Xilei, Sun, Yongjie, Sun, Yongzhao, Suwonjandee, Narumon, Szelezniak, Michal, Tang, Jian, Tang, Qiang, Tang, Quan, Tang, Xiao, Tietzsch, Alexander, Tkachev, Igor, Tmej, Toma, Treskov, Konstantin, Triossi, Andrea, Troni, Giancarlo, Trzaska, Wladyslaw, Tuve, Cristina, Ushakov, Nikita, van den Boom, Johanne, van Waasen, Stefan, Vanroyen, Guillaume, Vassilopoulos, Nikolao, Vedin, Vadim, Verde, Giuseppe, Vialkov, Maxim, Viaud, Benoit, Vollbrecht, Moritz Corneliu, Volpe, Cristina, Vorobel, Vit, Voronin, Dmitriy, Votano, Lucia, Walker, Pablo, Wang, Caishen, Wang, Chung-Hsiang, Wang, En, Wang, Guoli, Wang, Jian, Wang, Jun, Wang, Kunyu, Wang, Lu, Wang, Meifen, Wang, Meng, Wang, Ruiguang, Wang, Siguang, Wang, Wei, Wang, Wenshuai, Wang, Xi, Wang, Xiangyue, Wang, Yangfu, Wang, Yaoguang, Wang, Yi, Wang, Yifang, Wang, Yuanqing, Wang, Yuman, Wang, Zhe, Wang, Zheng, Wang, Zhimin, Wang, Zongyi, Waqas, Muhammad, Watcharangkool, Apimook, Wei, Lianghong, Wei, Wei, Wei, Wenlu, Wei, Yadong, Wen, Liangjian, Wiebusch, Christopher, Wong, Steven Chan-Fai, Wonsak, Bjoern, Wu, Diru, Wu, Fangliang, Wu, Qun, Wu, Zhi, Wurm, Michael, Wurtz, Jacque, Wysotzki, Christian, Xi, Yufei, Xia, Dongmei, Xie, Xiaochuan, Xie, Yuguang, Xie, Zhangquan, Xing, Zhizhong, Xu, Benda, Xu, Cheng, Xu, Donglian, Xu, Fanrong, Xu, Hangkun, Xu, Jilei, Xu, Jing, Xu, Meihang, Xu, Yin, Xu, Yu, Yan, Baojun, Yan, Taylor, Yan, Wenqi, Yan, Xiongbo, Yan, Yupeng, Yang, Anbo, Yang, Changgen, Yang, Chengfeng, Yang, Huan, Yang, Jie, Yang, Lei, Yang, Xiaoyu, Yang, Yifan, Yao, Haifeng, Yasin, Zafar, Ye, Jiaxuan, Ye, Mei, Ye, Ziping, Yegin, Ugur, Yermia, Frédéric, Yi, Peihuai, Yin, Na, Yin, Xiangwei, You, Zhengyun, Yu, Boxiang, Yu, Chiye, Yu, Chunxu, Yu, Hongzhao, Yu, Miao, Yu, Xianghui, Yu, Zeyuan, Yu, Zezhong, Yuan, Chengzhuo, Yuan, Ying, Yuan, Zhenxiong, Yuan, Ziyi, Yue, Baobiao, Zafar, Noman, Zambanini, Andre, Zavadskyi, Vitalii, Zeng, Shan, Zeng, Tingxuan, Zeng, Yuda, Zhan, Liang, Zhang, Aiqiang, Zhang, Feiyang, Zhang, Guoqing, Zhang, Haiqiong, Zhang, Honghao, Zhang, Jiawen, Zhang, Jie, Zhang, Jin, Zhang, Jingbo, Zhang, Jinnan, Zhang, Peng, Zhang, Qingmin, Zhang, Shiqi, Zhang, Shu, Zhang, Tao, Zhang, Xiaomei, Zhang, Xuantong, Zhang, Xueyao, Zhang, Yan, Zhang, Yinhong, Zhang, Yiyu, Zhang, Yongpeng, Zhang, Yuanyuan, Zhang, Yumei, Zhang, Zhenyu, Zhang, Zhijian, Zhao, Fengyi, Zhao, Jie, Zhao, Rong, Zhao, Shujun, Zhao, Tianchi, Zheng, Dongqin, Zheng, Hua, Zheng, Minshan, Zheng, Yangheng, Zhong, Weirong, Zhou, Jing, Zhou, Li, Zhou, Nan, Zhou, Shun, Zhou, Tong, Zhou, Xiang, Zhu, Jiang, Zhu, Kangfu, Zhu, Kejun, Zhu, Zhihang, Zhuang, Bo, Zhuang, Honglin, Zong, Liang, Zou, Jiaheng, Institut Pluridisciplinaire Hubert Curien (IPHC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Abusleme A., Adam T., Ahmad S., Ahmed R., Aiello S., Akram M., An F., An Q., Andronico G., Anfimov N., Antonelli V., Antoshkina T., Asavapibhop B., de Andre J.P.A.M., Auguste D., Babic A., Baldini W., Barresi A., Basilico D., Baussan E., Bellato M., Bergnoli A., Birkenfeld T., Blin S., Blum D., Blyth S., Bolshakova A., Bongrand M., Bordereau C., Breton D., Brigatti A., Brugnera R., Bruno R., Budano A., Buscemi M., Busto J., Butorov I., Cabrera A., Cai H., Cai X., Cai Y., Cai Z., Cammi A., Campeny A., Cao C., Cao G., Cao J., Caruso R., Cerna C., Chang J., Chang Y., Chen P., Chen P.-A., Chen S., Chen X., Chen Y.-W., Chen Y., Chen Z., Cheng J., Cheng Y., Chetverikov A., Chiesa D., Chimenti P., Chukanov A., Claverie G., Clementi C., Clerbaux B., Conforti Di Lorenzo S., Corti D., Cremonesi O., Dal Corso F., Dalager O., De La Taille C., Deng J., Deng Z., Depnering W., Diaz M., Ding X., Ding Y., Dirgantara B., Dmitrievsky S., Dohnal T., Dolzhikov D., Donchenko G., Dong J., Doroshkevich E., Dracos M., Druillole F., Du S., Dusini S., Dvorak M., Enqvist T., Enzmann H., Fabbri A., Fajt L., Fan D., Fan L., Fang J., Fang W., Fargetta M., Fedoseev D., Fekete V., Feng L.-C., Feng Q., Ford R., Formozov A., Fournier A., Gan H., Gao F., Garfagnini A., Giammarchi M., Giaz A., Giudice N., Gonchar M., Gong G., Gong H., Gornushkin Y., Gottel A., Grassi M., Grewing C., Gromov V., Gu M., Gu X., Gu Y., Guan M., Guardone N., Gul M., Guo C., Guo J., Guo W., Guo X., Guo Y., Hackspacher P., Hagner C., Han R., Han Y., Hassan M.S., He M., He W., Heinz T., Hellmuth P., Heng Y., Herrera R., Hor Y.K., Hou S., Hsiung Y., Hu B.-Z., Hu H., Hu J., Hu S., Hu T., Hu Z., Huang C., Huang G., Huang H., Huang W., Huang X., Huang Y., Hui J., Huo L., Huo W., Huss C., Hussain S., Ioannisian A., Isocrate R., Jelmini B., Jen K.-L., Jeria I., Ji X., Jia H., Jia J., Jian S., Jiang D., Jiang X., Jin R., Jing X., Jollet C., Joutsenvaara J., Jungthawan S., Kalousis L., Kampmann P., Kang L., Karaparambil R., Kazarian N., Khan W., Khosonthongkee K., Korablev D., Kouzakov K., Krasnoperov A., Kruth A., Kutovskiy N., Kuusiniemi P., Lachenmaier T., Landini C., Leblanc S., Lebrin V., Lefevre F., Lei R., Leitner R., Leung J., Li D., Li F., Li H., Li J., Li M., Li N., Li Q., Li R., Li S., Li T., Li W., Li X., Li Y., Li Z., Liang H., Liao J., Liebau D., Limphirat A., Limpijumnong S., Lin G.-L., Lin S., Lin T., Ling J., Lippi I., Liu F., Liu H., Liu J., Liu M., Liu Q., Liu R., Liu S., Liu X., Liu Y., Lokhov A., Lombardi P., Lombardo C., Loo K., Lu C., Lu H., Lu J., Lu S., Lu X., Lubsandorzhiev B., Lubsandorzhiev S., Ludhova L., Luo F., Luo G., Luo P., Luo S., Luo W., Lyashuk V., Ma B., Ma Q., Ma S., Ma X., Maalmi J., Malyshkin Y., Mantovani F., Manzali F., Mao X., Mao Y., Mari S.M., Marini F., Marium S., Martellini C., Martin-Chassard G., Martini A., Mayer M., Mayilyan D., Mednieks I., Meng Y., Meregaglia A., Meroni E., Meyhofer D., Mezzetto M., Miller J., Miramonti L., Montini P., Montuschi M., Muller A., Nastasi M., Naumov D.V., Naumova E., Navas-Nicolas D., Nemchenok I., Nguyen Thi M.T., Ning F., Ning Z., Nunokawa H., Oberauer L., Ochoa-Ricoux J.P., Olshevskiy A., Orestano D., Ortica F., Othegraven R., Pan H.-R., Paoloni A., Parmeggiano S., Pei Y., Pelliccia N., Peng A., Peng H., Perrot F., Petitjean P.-A., Petrucci F., Pilarczyk O., Pineres Rico L.F., Popov A., Poussot P., Pratumwan W., Previtali E., Qi F., Qi M., Qian S., Qian X., Qian Z., Qiao H., Qin Z., Qiu S., Rajput M.U., Ranucci G., Raper N., Re A., Rebber H., Rebii A., Ren B., Ren J., Ricci B., Robens M., Roche M., Rodphai N., Romani A., Roskovec B., Roth C., Ruan X., Rujirawat S., Rybnikov A., Sadovsky A., Saggese P., Sanfilippo S., Sangka A., Sanguansak N., Sawangwit U., Sawatzki J., Sawy F., Schever M., Schwab C., Schweizer K., Selyunin A., Serafini A., Settanta G., Settimo M., Shao Z., Sharov V., Shaydurova A., Shi J., Shi Y., Shutov V., Sidorenkov A., Simkovic F., Sirignano C., Siripak J., Sisti M., Slupecki M., Smirnov M., Smirnov O., Sogo-Bezerra T., Sokolov S., Songwadhana J., Soonthornthum B., Sotnikov A., Sramek O., Sreethawong W., Stahl A., Stanco L., Stankevich K., Stefanik D., Steiger H., Steinmann J., Sterr T., Stock M.R., Strati V., Studenikin A., Sun S., Sun X., Sun Y., Suwonjandee N., Szelezniak M., Tang J., Tang Q., Tang X., Tietzsch A., Tkachev I., Tmej T., Treskov K., Triossi A., Troni G., Trzaska W., Tuve C., Ushakov N., van den Boom J., van Waasen S., Vanroyen G., Vassilopoulos N., Vedin V., Verde G., Vialkov M., Viaud B., Vollbrecht M.C., Volpe C., Vorobel V., Voronin D., Votano L., Walker P., Wang C., Wang C.-H., Wang E., Wang G., Wang J., Wang K., Wang L., Wang M., Wang R., Wang S., Wang W., Wang X., Wang Y., Wang Z., Waqas M., Watcharangkool A., Wei L., Wei W., Wei Y., Wen L., Wiebusch C., Wong S.C.-F., Wonsak B., Wu D., Wu F., Wu Q., Wu Z., Wurm M., Wurtz J., Wysotzki C., Xi Y., Xia D., Xie X., Xie Y., Xie Z., Xing Z., Xu B., Xu C., Xu D., Xu F., Xu H., Xu J., Xu M., Xu Y., Yan B., Yan T., Yan W., Yan X., Yan Y., Yang A., Yang C., Yang H., Yang J., Yang L., Yang X., Yang Y., Yao H., Yasin Z., Ye J., Ye M., Ye Z., Yegin U., Yermia F., Yi P., Yin N., Yin X., You Z., Yu B., Yu C., Yu H., Yu M., Yu X., Yu Z., Yuan C., Yuan Y., Yuan Z., Yue B., Zafar N., Zambanini A., Zavadskyi V., Zeng S., Zeng T., Zeng Y., Zhan L., Zhang A., Zhang F., Zhang G., Zhang H., Zhang J., Zhang P., Zhang Q., Zhang S., Zhang T., Zhang X., Zhang Y., Zhang Z., Zhao F., Zhao J., Zhao R., Zhao S., Zhao T., Zheng D., Zheng H., Zheng M., Zheng Y., Zhong W., Zhou J., Zhou L., Zhou N., Zhou S., Zhou T., Zhou X., Zhu J., Zhu K., Zhu Z., Zhuang B., Zhuang H., Zong L., Zou J., Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), JUNO collaboration, The, Pedro Athayde Marcondes de André, João, Sohaib Hassan, Muhammad, Thuan Nguyen Thi, Minh, Pedro Ochoa-Ricoux, Juan, Felipe Piñeres Rico, Lui, Usman Rajput, Muhammad, Raphael Stock, Matthia, Cornelius Vollbrecht, Moritz, and Chan-Fai Wong, Steven
Subjects: Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Nuclear engineering, Monte Carlo method, Control (management), measurement methods, FOS: Physical sciences, QC770-798, Scintillator, 7. Clean energy, 01 natural sciences, NO, PE2_2, Nuclear and particle physics. Atomic energy. Radioactivity, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], ddc:530, Sensitivity (control systems), 010306 general physics, Physics, JUNO, liquid [scintillation counter], 010308 nuclear & particles physics, business.industry, Detector, Settore FIS/01 - Fisica Sperimentale, radioactivity [background], suppression [background], Instrumentation and Detectors (physics.ins-det), Monte Carlo [numerical calculations], Nuclear power, threshold [energy], sensitivity, Neutrino Detectors and Telescopes (experiments), GEANT, Neutrino, business, Energy (signal processing)
Abstract: JUNO is a massive liquid scintillator detector with a primary scientific goal of determining the neutrino mass ordering by studying the oscillated anti-neutrino flux coming from two nuclear power plants at 53 km distance. The expected signal anti-neutrino interaction rate is only 60 counts per day, therefore a careful control of the background sources due to radioactivity is critical. In particular, natural radioactivity present in all materials and in the environment represents a serious issue that could impair the sensitivity of the experiment if appropriate countermeasures were not foreseen. In this paper we discuss the background reduction strategies undertaken by the JUNO collaboration to reduce at minimum the impact of natural radioactivity. We describe our efforts for an optimized experimental design, a careful material screening and accurate detector production handling, and a constant control of the expected results through a meticulous Monte Carlo simulation program. We show that all these actions should allow us to keep the background count rate safely below the target value of 10 Hz in the default fiducial volume, above an energy threshold of 0.7 MeV., 35 pages, 12 figures
Published: 2021
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2. Neutrino decoherence in presence of strong gravitational fields

Author: Maria Cristina Volpe, Amélie Chatelain, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: High Energy Physics - Theory, Nuclear and High Energy Physics, neutrino propagation in curved spacetime, Quantum decoherence, neutrino decoherence, Physics::Instrumentation and Detectors, Wave packet, Astrophysics::High Energy Astrophysical Phenomena, Compact star, 01 natural sciences, Gravitation, General Relativity and Quantum Cosmology, Gravitational field, strong field, 0103 physical sciences, Proper time, Neutrino masses and mixings, 010306 general physics, decoherence, density matrix, Physics, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], High Energy Physics::Phenomenology, matter: effect, lcsh:QC1-999, coherence, neutrino: propagation, High Energy Physics - Phenomenology, Astrophysics - Solar and Stellar Astrophysics, space-time, gravitation, Quantum electrodynamics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino, lcsh:Physics, Coherence (physics)
Abstract: We explore the impact of strong gravitational fields on neutrino decoherence. To this aim, we employ the density matrix formalism to describe the propagation of neutrino wave packets in curved spacetime. By considering Gaussian wave packets, we determine the coherence proper time, neglecting the effect of matter outside the compact object. We show that strong gravitational fields nearby compact objects significantly influence neutrino coherence., Comment: 7 pages, 2 figures
Published: 2020
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3. Fast Neutrino Flavor Conversion Modes in Multidimensional Core-collapse Supernova Models: the Role of the Asymmetric Neutrino Distributions

Author: Tomoya Takiwaki, Sajad Abbar, Huaiyu Duan, Maria Cristina Volpe, Kohsuke Sumiyoshi, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: High Energy Physics - Theory, Particle physics, Astrophysics::High Energy Astrophysical Phenomena, protoneutron star, multipole, FOS: Physical sciences, Neutrino decoupling, 01 natural sciences, Boltzmann equation, symbols.namesake, 0103 physical sciences, 010306 general physics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, neutrino: gas, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], High Energy Physics::Phenomenology, supernova: model, crossing, Type II supernova, Supernova, collapse, High Energy Physics - Theory (hep-th), Boltzmann constant, neutrino: flavor, symbols, High Energy Physics::Experiment, Neutrino, higher-dimensional, Astrophysics - High Energy Astrophysical Phenomena, Multipole expansion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], neutrino: angular distribution, neutrino: decoupling, Astrophysics and astroparticle physics
Abstract: A dense neutrino gas, such as the one anticipated in the supernova environment, can experience fast neutrino flavor conversions on scales much shorter than those expected in vacuum probably provided that the angular distributions of $\nu_e$ and $\bar\nu_e$ cross each other. We perform a detailed investigation of the neutrino angular distributions obtained by solving the Boltzmann equations for fixed matter profiles of some representative snapshots during the post-bounce phase of core-collapse supernovae in multidimensional calculations of an $11.2\mathrm{M}_{\odot}$ and a $27\mathrm{M}_{\odot}$ progenitor models. Although the $11.2\mathrm{M}_{\odot}$ model features $\nu_e - \bar\nu_e$ angular crossings and the associated fast modes at different time snapshots, the $27\mathrm{M}_{\odot}$ model does not show any crossings within the decoupling region. We show that this can be understood by studying the multipole components of the neutrino distributions. In fact, there is a higher chance for the occurrence of $\nu_e - \bar\nu_e$ angular crossings for the zones where the multipole components of the neutrino distributions are strong enough. We also show that there can exist more than one crossings between the angular distributions of $\nu_e$ and $\bar{\nu}_e$. In addition, apart from the crossings within the neutrino decoupling region, there is a class of $\nu_e-\bar\nu_e$ angular crossings which appears very deep inside the proto-neutron star., Comment: Version accepted in PRD
Published: 2020
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4. Neutrino decoupling including flavour oscillations and primordial nucleosynthesis

Author: Julien Froustey, Maria Cristina Volpe, Cyril Pitrou, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], media_common.quotation_subject, Flavour, kinetic, FOS: Physical sciences, hierarchy, Neutrino decoupling, 01 natural sciences, Nuclear Theory (nucl-th), thermodynamics, High Energy Physics - Phenomenology (hep-ph), Big Bang nucleosynthesis, 0103 physical sciences, flavor: oscillation, Adiabatic process, media_common, Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, nucleosynthesis: primordial, Astronomy and Astrophysics, Decoupling (cosmology), quantum electrodynamics: correction, Universe, 3. Good health, Numerical integration, High Energy Physics - Phenomenology, potential: chemical, adiabatic, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Neutrino, neutrino: decoupling, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We revisit the decoupling of neutrinos in the early universe with flavour oscillations. We rederive the quantum kinetic equations which determine the neutrino evolution based on a BBGKY-like hierarchy, and include for the first time the full collision term, with both on- and off-diagonal terms for all relevant reactions. We focus on the case of zero chemical potential and solve these equations numerically. We also develop an approximate scheme based on the adiabatic evolution in the matter basis. In fact, the large difference between the oscillations and cosmological time scales allows to consider averaged flavour oscillations which can speed up the numerical integration by two orders of magnitude, when combined with a direct computation of the differential system Jacobian. The approximate numerical scheme is also useful to gain more insight into the physics of neutrino decoupling. Including the most recent results on plasma thermodynamics QED corrections, we update the effective number of neutrinos to $N_{\mathrm{eff}} = 3.0440$. Finally we study the impact of flavour oscillations during neutrino decoupling on the subsequent primordial nucleosynthesis., Comment: 38 pages, 6 figures, v2: appendix discussing the effect of a CP phase. Version published in JCAP
Published: 2020
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5. Corrigendum to 'CP violation effects on the neutrino degeneracy parameters in the Early Universe' [Nucl. Phys. B 837 (2010) 50–60]

Author: Maria Cristina Volpe, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: [PHYS]Physics [physics], Physics, Nuclear and High Energy Physics, Particle physics, 010308 nuclear & particles physics, media_common.quotation_subject, 01 natural sciences, Universe, 0103 physical sciences, lcsh:QC770-798, CP violation, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Degeneracy (biology), Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010306 general physics, ComputingMilieux_MISCELLANEOUS, media_common
Abstract: We correct for misleading statements in the text of the manuscript.
Published: 2020
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6. On Fast Neutrino Flavor Conversion Modes in the Nonlinear Regime

Author: Maria Cristina Volpe, Sajad Abbar, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Quantum decoherence, FOS: Physical sciences, 01 natural sciences, neutrino: density, 0103 physical sciences, 010306 general physics, Neutrino oscillation, Flavor, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Core-collapse supernova, density, Number density, 010308 nuclear & particles physics, Neutrino oscillations, High Energy Physics::Phenomenology, stability, Type II supernova, lcsh:QC1-999, Nonlinear system, Amplitude, oscillation: collective, neutrino: flavor, Binary neutron star mergers, nonlinear, High Energy Physics::Experiment, neutrino: oscillation, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], lcsh:Physics
Abstract: A dense neutrino medium could experience self-induced flavor conversions on relatively small scales in the presence of the so-called fast flavor conversion modes. Owing to the fact that fast conversion scales could be much smaller than the ones of the traditional collective neutrino oscillations, it has been speculated that fast modes could lead to some sort of flavor decoherence/equilibrium. We study the evolution of fast modes in the nonlinear regime and we show that not only fast modes are not guaranteed to lead to flavor equilibrium, but also they could lead to some sort of collective neutrino oscillations but on scales determined by neutrino number density. For the $\nu_e$ dominated case, we observe large amplitude collective oscillations, whereas a sort of flavor stabilization is reached for the $\bar{\nu}_e$ dominated case., Comment: Version to appear in PLB
Published: 2019
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7. On the occurrence of fast neutrino flavor conversions in multidimensional supernova models

Author: Huaiyu Duan, Sajad Abbar, Maria Cristina Volpe, Kohsuke Sumiyoshi, Tomoya Takiwaki, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)
Subjects: Particle physics, supernova: collapse, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Neutrino decoupling, 01 natural sciences, Asymmetry, transformation: flavor, Boltzmann equation, Nucleosynthesis, 0103 physical sciences, angular distribution, 010306 general physics, Neutrino oscillation, neutron star, Astrophysics::Galaxy Astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, High Energy Physics::Phenomenology, nucleosynthesis, supernova: model, crossing, Supernova, Neutron star, Automatic Keywords, Amplitude, neutrino: flavor, High Energy Physics::Experiment, neutrino: oscillation, Neutrino, higher-dimensional, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], asymmetry, neutrino: decoupling, Astrophysics and astroparticle physics
Abstract: The dense neutrino medium in a core-collapse supernova or a neutron-star merger event can experience fast flavor conversions on time/distance scales that are much smaller than those of vacuum oscillations. It is believed that fast neutrino flavor transformation occurs in the region where the angular distributions of ${\ensuremath{\nu}}_{e}$ and ${\overline{\ensuremath{\nu}}}_{e}$ cross each other. We present the first study of this crossing phenomenon and the fast neutrino flavor conversions in multidimensional (multi-D) supernova models. We examine the neutrino distributions obtained by solving the Boltzmann transport equation for several fixed profiles which are representative snapshots taken from separate 2D and 3D supernova simulations with an $11.2\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ progenitor model. Our research shows that the spherically asymmetric patterns of the ${\ensuremath{\nu}}_{e}$ and ${\overline{\ensuremath{\nu}}}_{e}$ fluxes in multi-D models can assist the appearance of the crossing between the ${\ensuremath{\nu}}_{e}$ and ${\overline{\ensuremath{\nu}}}_{e}$ angular distributions. In the models that we have studied, there exist unstable neutrino oscillation modes in and beyond the neutrino decoupling region which have amplitude growth rates as large as an $e$-fold per nanosecond. This finding can have important consequences for the explosion mechanism, nucleosynthesis, and neutrino signals of core-collapse supernovae.
Published: 2019
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8. Late time supernova neutrino signal and proto-neutron star radius

Author: Francesco Vissani, Maria Cristina Volpe, Andrea Gallo Rosso, Sajad Abbar, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Cherenkov counter: water, Astrophysics::High Energy Astrophysical Phenomena, protoneutron star, elastic scattering, FOS: Physical sciences, Astrophysics, KAMIOKANDE, 01 natural sciences, Signal, neutrino: flux, High Energy Physics - Phenomenology (hep-ph), statistical analysis, neutrino: energy, 0103 physical sciences, neutrino: supernova, numerical calculations, neutron star, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, new physics, Astronomy and Astrophysics, Radius, Supernova, Neutron star, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], black body, Astrophysics::Earth and Planetary Astrophysics, Neutrino
Abstract: We discuss the possibility of reconstructing the newly formed proto-neutron star radius from the late time neutrino signal. A black-body emission is assumed for the neutron star cooling phase. We parametrize the neutrino time-integrated fluxes based on simulations of Roberts and Reddy. A likelihood analysis of the inverse-beta decay and elastic scattering events in Hyper-Kamiokande is performed in both three flavor and an effective one flavor scenario. We show that the precision achievable in the radius reconstruction strongly depends on a correlation with the pinching parameter and therefore the corresponding prior. Although this correlation hinders the precise measurement of the newly formed neutron star radius, it could help measure the pinching parameters with good accuracy in view of the current constraints on neutron star radius, or if the neutron star radius is precisely measured., 21 pages, 11 figures, 5 tables
Published: 2018
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9. Neutrino propagation in binary neutron star mergers in presence of nonstandard interactions

Author: Maria Cristina Volpe, Amélie Chatelain, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: Particle physics, neutron star: binary, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Astrophysics::High Energy Astrophysical Phenomena, Binary number, Astrophysics, 01 natural sciences, 14.60.Pq, 13.15.+g, Accretion disc, accretion, Nucleosynthesis, 0103 physical sciences, new interaction, 010306 general physics, numerical calculations, Nuclear theory, [ PHYS.NUCL ] Physics [physics]/Nuclear Theory [nucl-th], Astrophysics::Galaxy Astrophysics, 97.60.Jd, MSW effect, Physics, flavor, 010308 nuclear & particles physics, nucleosynthesis, 3. Good health, neutrino: propagation, High Energy Physics - Phenomenology, Neutron star, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Neutrino
Abstract: We explore the impact of nonstandard interactions on neutrino propagation in accretion disks around binary neutron star mergers remnants. We show flavor evolution can be significantly modified even for values of the nonstandard couplings well below current bounds. We demonstrate the occurrence of I resonances as synchronized MSW phenomena and show that intricate conversion patterns might appear depending on the nonstandard interaction parameters. We discuss the possible implications for nucleosynthesis., Comment: 14 pages, 13 figures
Published: 2018
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10. What can we learn on supernova neutrino spectra with water Cherenkov detectors?

Author: Maria Cristina Volpe, Francesco Vissani, Andrea Gallo Rosso, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: data analysis method, Cherenkov counter: water, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, elastic scattering, FOS: Physical sciences, KAMIOKANDE, 7. Clean energy, 01 natural sciences, Nuclear physics, neutrino astronomy, High Energy Physics - Phenomenology (hep-ph), statistical analysis, neutrino: spectrum, 0103 physical sciences, neutrino: supernova, supernova neutrinos, 010303 astronomy & astrophysics, Cherenkov radiation, High Energy Astrophysical Phenomena (astro-ph.HE), Elastic scattering, Physics, neutrino muon, Muon, Luminosity (scattering theory), Neutral current, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Astronomy and Astrophysics, semileptonic decay, oxygen: target, 3. Good health, High Energy Physics - Phenomenology, antineutrino electron, efficiency, Inverse beta decay, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Electron neutrino, neutrino detectors
Abstract: We investigate the precision with which the supernova neutrino spectra can be reconstructed in water Cherenkov detectors, in particular the large scale Hyper-Kamiokande and Super-Kamiokande. To this aim, we consider quasi-thermal neutrino spectra modified by the Mikheev-Smirnov-Wolfenstein effect for the case of normal ordering. We perform three 9 degrees of freedom likelihood analyses including first inverse-beta decay only, then the combination of inverse beta decay and elastic scattering on electrons and finally a third analysis that also includes neutral scattering neutrino-oxygen events. A tenth parameter is added in the analyses to account for the theoretical uncertainty on the neutral current neutrino-oxygen cross section. By assuming a 100\% efficiency in Hyper-Kamiokande, we show that one can reconstruct the electron antineutrino average energy and pinching parameter with an accuracy of $\sim2\%$ and $\sim7\%$ percent respectively, while the antineutrino integrated luminosity can be pinned down at $\sim3\%$ percent level. As for the muon and tau neutrinos, the average energy and the integrated luminosity can be measured with $\sim7\%$ precision. These results represent a significant improvement with respect Super-Kamiokande, particularly for the pinching parameter defining the electron antineutrino spectra. As for electron neutrinos, the determination of the emission parameters requires the addition of supplementary detection channels., Comment: 22 pages, 19 figures, 7 tables
Published: 2018
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11. Neutrino astrophysics and its connections to nuclear physics

Author: Maria Cristina Volpe, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: History, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], FOS: Physical sciences, Astrophysics, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Education, Nuclear Theory (nucl-th), Nuclear physics, Physics::Popular Physics, High Energy Physics - Phenomenology (hep-ph), nuclear physics, 0103 physical sciences, [ PHYS.NEXP ] Physics [physics]/Nuclear Experiment [nucl-ex], Nuclear Experiment (nucl-ex), Nuclear Experiment, 010306 general physics, Nuclear theory, [ PHYS.NUCL ] Physics [physics]/Nuclear Theory [nucl-th], Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science::Computers and Society, Computer Science Applications, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], neutrino: cosmic radiation, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino
Abstract: We highlight recent developments in neutrino astrophysics. We discuss some of the connections with nuclear physics., Comment: 7 pages, 1 figure, Proceedings of the "Conference on Neutrino and Nuclear Physics (CNNP2017), 15-21 October, Catania
Published: 2017
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12. Open issues in neutrino astrophysics

Author: Cristina Volpe
Subjects: Physics, Sterile neutrino, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, General Physics and Astronomy, Astrophysics, Accretion (astrophysics), Black hole, Massless particle, Stars, Supernova, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Neutrino, Lepton
Abstract: Neutrinos of astrophysical origin are messengers produced in stars, in explosive phenomena like core-collapse supernovae, in the accretion disks around black holes, or in the Earth's atmosphere. Their fluxes and spectra encode information on the environments that produce them. Such fluxes are modified in characteristic ways when neutrinos traverse a medium. Here the current understanding of neutrino flavour conversion in media is summarized. The importance of this domain for astrophysical observations is emphasized. Examples are given of the fundamental properties that research into astrophysical neutrinos has uncovered, or might reveal in the future.
Published: 2013
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13. Measuring the neutron star compactness and binding energy with supernova neutrinos

Author: Francesco Vissani, Maria Cristina Volpe, Andrea Gallo Rosso, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: electron, neutral current, Cherenkov counter: water, Astrophysics::High Energy Astrophysical Phenomena, Binding energy, elastic scattering, FOS: Physical sciences, KAMIOKANDE, 01 natural sciences, neutron stars, Nuclear physics, High Energy Physics - Phenomenology (hep-ph), neutrino: spectrum, 0103 physical sciences, neutrino: supernova, numerical calculations, neutron star, supernova neutrinos, 010303 astronomy & astrophysics, Physics, Elastic scattering, 010308 nuclear & particles physics, Astronomy and Astrophysics, semileptonic decay, energy: hierarchy, binding energy, Neutron star, Supernova, High Energy Physics - Phenomenology, Neutrino detector, gravitation, Inverse beta decay, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Neutrino, Gravitational binding energy, neutrino detectors
Abstract: We investigate the precision with which a neutron star gravitational binding energy can be measured through the supernova neutrino signal, without assuming any prior such as the energy equipartition hypothesis, mean energies hierarchy or constraints on the pinching parameters that characterize the neutrino spectra. We consider water Cherenkov detectors and prove that combining inverse beta decay with elastic scattering on electrons is sufficient to reach $11\%$ precision on the neutron star gravitational binding energy already with Super-Kamiokande. The inclusion of neutral current events on oxygen in the analysis does not improve the precision further. We show that $3\%$ precision can be achieved if priors are introduced, such as energy equipartition. We discuss the implications of our findings on the properties of the newly formed neutron star, in particular concerning the assessment of the compactness or mass--radius relation., 14 pages, 3 figures. Minor corrections implemented in version 2
Published: 2017
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14. Helicity coherence in binary neutron star mergers and non-linear feedback

Author: Amélie Chatelain, Cristina Volpe, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Particle physics, neutron star: binary, Astrophysics::High Energy Astrophysical Phenomena, Binary number, feedback, anisotropy, spin, 01 natural sciences, 14.60.Pq, Nuclear physics, 13.15.+g, 0103 physical sciences, neutrino: mass, 010306 general physics, Neutrino oscillation, numerical calculations, 97.60.Jd, neutrino: interaction, Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, antineutrino, helicity, Helicity, coherence, Nonlinear system, Neutron star, MAJORANA, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], neutrino: flavor, neutrino: Majorana, nonlinear, High Energy Physics::Experiment, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Neutrino, neutrino: mixing, Coherence (physics)
Abstract: Neutrino flavor conversion studies based on astrophysical environments usually implement neutrino mixings, neutrino interactions with matter and neutrino self-interactions. In anisotropic media, the most general mean-field treatment includes neutrino mass contributions as well, that introduce a coupling between neutrinos and antineutrinos termed helicity or spin coherence. We discuss resonance conditions for helicity coherence for Dirac and Majorana neutrinos. We explore the role of these mean-field contributions on flavor evolution in the context of a binary neutron star merger remnant. We find that resonance conditions can be satisfied in neutron star merger scenarios while adiabaticity is not sufficient for efficient flavor conversion. We analyse our numerical findings by discussing general conditions to have multiple MSW-like resonances, in presence of non-linear feedback, in astrophysical environments., Comment: 21 pages, 2 tables, 9 figures. Figures (2-12) and text in the result section III have been modified (due to a numerical error), conclusion remains
Published: 2017
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15. Branch II : Neutrino Oscillations at Low Energies

Author: Cristina Volpe and Anatael Cabrera
Subjects: Physics, Nuclear and High Energy Physics, Particle physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Solar neutrino, High Energy Physics::Phenomenology, Solar neutrino problem, Atomic and Molecular Physics, and Optics, Cosmic neutrino background, Supernova, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Neutrino astronomy, Neutrino oscillation
Abstract: We summarize here briefly the experimental and theoretical results presented at the NOW2010 workshop during the parallel session Branch II “Oscillations at low energies”. The topics have covered open problems and recent advances in solar neutrinos, reactor and geo-neutrinos, as well as neutrinos from core-collapse supernovae.
Published: 2011
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16. Possible CP-violation effects in core-collapse supernovae

Author: A. B. Balantekin, Cristina Volpe, J. Gava, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Particle physics, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Physics beyond the Standard Model, FOS: Physical sciences, Astrophysics, r-process nucleosynthesis, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Phenomenology (hep-ph), core-collapse supernova, 0103 physical sciences, 010306 general physics, Physics, Muon, 010308 nuclear & particles physics, Astrophysics (astro-ph), High Energy Physics::Phenomenology, Solar neutrino problem, Type II supernova, CP-violation in neutrino sector, Massless particle, High Energy Physics - Phenomenology, Supernova, Neutron star, High Energy Physics::Experiment, Neutrino
Abstract: We study CP-violation effects when neutrinos are present in dense matter, such as outside the proto-neutron star formed in a core-collapse supernova. Using general arguments based on the Standard Model, we confirm that there are no CP-violating effects at the tree level on the electron neutrino and anti-neutrino fluxes in a core-collapse supernova. On the other hand significant effects can be obtained for muon and tau neutrinos even at the tree level. We show that CP violating effects can be present in the supernova electron (anti)neutrino fluxes as well, if muon and tau neutrinos have different fluxes at the neutrinosphere. Such differences could arise due to physics beyond the Standard Model, such as the presence of flavor-changing interactions., 11 pages, 18 figures
Published: 2008
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17. Neutrino Physics with JUNO

Author: Jilei Xu, Andre Kruth, Yuguang Xie, Wei Wang, S. M. Chen, Janet Conrad, Xingtao Huang, V. Vorobel, Jose Busto, Qi An, Alexander Olshevskiy, Jiaxing Li, Cécile Jollet, Xiangdong Ji, Ran Han, Sandra Zavatarelli, Dmitriy Taichenachev, F. Yermia, Georg G. Raffelt, R. Möllenberg, Yong Zhong Qian, Ugur Yegin, Yu Yao, Wenxiong Zhou, Siguang Wang, Zheng Wang, Zhenyu Zhang, Rupert Leitner, M. Göger-Neff, Lino Miramonti, Qun Wu, O. Drapier, Donghua Fan, Jen-Chieh Peng, D. W. Liu, Stephen T. Dye, Hao Cai, John F. Beacom, Lucia Votano, Massimiliano Clemenza, Juan Pedro Ochoa-Ricoux, Davide Chiesa, Tao Hu, Igor Tkachev, Fabio Mantovani, Hongbang Liu, Jiawen Zhang, J. G. Lu, Shulin Liu, Baojun Yan, Weili Zhong, Changgen Yang, A. Garfagnini, Antonio Cammi, Liangjian Wen, Guofu Cao, Christopher Wiebusch, Michael Wurm, Anselmo Meregaglia, Xubo Ma, Boxiang Yu, G. Meng, Damien Dornic, Vladimir Lyashuk, Björn Wonsak, Anatael Cabrera, Y. H. Zhou, Jochen Steinmann, M. Soiron, S. Dusini, Xiaomei Li, Honghao Zhang, Yajun Mao, Gang Guo, Y. B. Hsiung, Z. V. Krumshteyn, Marco Grassi, Guanghua Gong, Guang Yang, Zhi Deng, Laurent Favart, Shaomin Chen, Jun Cao, Lothar Oberauer, Xilei Sun, Herve De Kerret, Hao Liang, Ara Ioannisian, Yufei Xi, Monica Sisti, Chao Li, Yuekun Heng, Yifang Wang, Alessandro Paoloni, Stefan van Waasen, Qingmin Zhang, Meng Wang, Shouyang Hu, Jing Zhou, Dongmei Xia, Yongjie Sun, G. Salamanna, Ezio Previtali, Mengyun Guan, Thomas Mueller, Bayarto Lubsandorzhiev, Xin Heng Guo, Guorong Zhou, Xiao Cai, Guey-Lin Lin, Zhimin Wang, Margherita Buizza Avanzini, Mauro Mezzetto, Barbara Ricci, Hu Liu, Chiara Sirignano, William F. McDonough, Xichao Ruan, Dmitry V. Naumov, Jiajie Ling, Ziyan Deng, Haoqi Lu, Jianglai Liu, Paolo Lombardi, Xiang Zhou, Manfred Jeitler, Weiguo Li, Christian Grewing, Barbara Clerbaux, Jianli Liu, Jian Fang, Yi Chen, Ming Qi, Oleg Smirnov, L. B. Bezrukov, Narine Kazarian, Yangheng Zheng, Wanlei Guo, Marcos Dracos, Jinchang Liu, Hui Gong, Ivano Lippi, Michael Karagounis, Stefano Maria Mari, Vito Antonelli, Miao He, Zhengyun You, Yayun Ding, Richard Ford, Zelimir Djurcic, Qian Liu, Zhonghua Qin, Jian Tang, E. Meroni, Shubin Liu, Ruiguang Wang, Jingbo Zhang, Rong Zhou, Timo Enqvist, Zhe Wang, V. V. Sinev, Simon Blyth, Zhenghua Zhao, Yi Wang, Yumei Zhang, Yi Li, Zeyuan Yu, Tobias Lachenmaier, Marco Giammarchi, Yongbing Long, Maxim Gonchar, Wei Wei, D. D'Angelo, Sen Qian, Shu Luo, Caren Hagner, Claudia-Elisabeth Wulz, H. Peng, Jiaheng Zou, Liang Zhan, Yifan Yang, Chunxu Yu, Wei Li, Markus Robens, Fengpeng An, Xiaoshan Jiang, Yen-Hsun Lin, Pasi Kuusiniemi, Zhibing Li, Luca Stanco, Fausto Ortica, Chao Zhang, Guangpeng An, Xiangdong Ruan, R. Brugnera, Achim Stahl, Eric Baussan, Yufeng Li, Livia Ludhova, Chung Hsiang Wang, Lei Huo, Vic Guarino, Tao Lin, X. N. Li, Haonan Gan, Lei Yang, Hao Wang, M. Gonin, Ye-Ling Zhou, Yun Chang, M. H. Shaevitz, Xin Qian, Wladyslaw Henryk Trzaska, Li Zhou, C. G. Yang, Zhi-zhong Xing, Jingbin Lu, Aldo Romani, Shun Zhou, Cristina Volpe, Li Kang, Junguang Lu, Gioacchino Ranucci, Hanxiong Huang, Guo-Li Wang, Jun Hu, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), JUNO, An, F, An, G, An, Q, Antonelli, V, Baussan, E, Beacom, J, Bezrukov, L, Blyth, S, Brugnera, R, Avanzini, M, Busto, J, Cabrera, A, Cai, H, Cai, X, Cammi, A, Cao, G, Cao, J, Chang, Y, Chen, S, Chen, Y, Chiesa, D, Clemenza, M, Clerbaux, B, Conrad, J, D'Angelo, D, De Kerret, H, Deng, Z, Ding, Y, Djurcic, Z, Dornic, D, Dracos, M, Drapier, O, Dusini, S, Dye, S, Enqvist, T, Fan, D, Fang, J, Favart, L, Ford, R, Göger Neff, M, Gan, H, Garfagnini, A, Giammarchi, M, Gonchar, M, Gong, G, Gong, H, Gonin, M, Grassi, M, Grewing, C, Guan, M, Guarino, V, Guo, G, Guo, W, Guo, X, Hagner, C, Han, R, He, M, Heng, Y, Hsiung, Y, Hu, J, Hu, S, Hu, T, Huang, H, Huang, X, Huo, L, Ioannisian, A, Jeitler, M, Ji, X, Jiang, X, Jollet, C, Kang, L, Karagounis, M, Kazarian, N, Krumshteyn, Z, Kruth, A, Kuusiniemi, P, Lachenmaier, T, Leitner, R, Li, C, Li, J, Li, W, Li, X, Li, Y, Li, Z, Liang, H, Lin, G, Lin, T, Lin, Y, Ling, J, Lippi, I, Liu, D, Liu, H, Liu, J, Liu, Q, Liu, S, Lombardi, P, Long, Y, Lu, H, Lu, J, Lubsandorzhiev, B, Ludhova, L, Luo, S, Lyashuk, V, Möllenberg, R, Ma, X, Mantovani, F, Mao, Y, Mari, S, Mcdonough, W, Meng, G, Meregaglia, A, Meroni, E, Mezzetto, M, Miramonti, L, Mueller, T, Naumov, D, Oberauer, L, Ochoa Ricoux, J, Olshevskiy, A, Ortica, F, Paoloni, A, Peng, H, Peng, J, Previtali, E, Qi, M, Qian, S, Qian, X, Qian, Y, Qin, Z, Raffelt, G, Ranucci, G, Ricci, B, Robens, M, Romani, A, Ruan, X, Salamanna, G, Shaevitz, M, Sinev, V, Sirignano, C, Sisti, M, Smirnov, O, Soiron, M, Stahl, A, Stanco, L, Steinmann, J, Sun, X, Sun, Y, Taichenachev, D, Tang, J, Tkachev, I, Trzaska, W, Van Waasen, S, Volpe, C, Vorobel, V, Votano, L, Wang, C, Wang, G, Wang, H, Wang, M, Wang, R, Wang, S, Wang, W, Wang, Y, Wang, Z, Wei, W, Wen, L, Wiebusch, C, Wonsak, B, Wu, Q, Wulz, C, Wurm, M, Xi, Y, Xia, D, Xie, Y, Xing, Z, Xu, J, Yan, B, Yang, C, Yang, G, Yang, L, Yang, Y, Yao, Y, Yegin, U, Yermia, F, You, Z, Yu, B, Yu, C, Yu, Z, Zavatarelli, S, Zhan, L, Zhang, C, Zhang, H, Zhang, J, Zhang, Q, Zhang, Y, Zhang, Z, Zhao, Z, Zheng, Y, Zhong, W, Zhou, G, Zhou, J, Zhou, L, Zhou, R, Zhou, S, Zhou, W, Zhou, X, Zhou, Y, Zou, J, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), An, Fengpeng, An, Guangpeng, An, Qi, Antonelli, Vito, Baussan, Eric, Beacom, John, Bezrukov, Leonid, Blyth, Simon, Brugnera, Riccardo, Avanzini, Margherita Buizza, Busto, Jose, Cabrera, Anatael, Cai, Hao, Cai, Xiao, Cammi, Antonio, Cao, Guofu, Cao, Jun, Chang, Yun, Chen, Shaomin, Chen, Shenjian, Chen, Yixue, Chiesa, Davide, Clemenza, Massimiliano, Clerbaux, Barbara, Conrad, Janet, D’Angelo, Davide, Kerret, Hervé De, Deng, Zhi, Deng, Ziyan, Ding, Yayun, Djurcic, Zelimir, Dornic, Damien, Dracos, Marco, Drapier, Olivier, Dusini, Stefano, Dye, Stephen, Enqvist, Timo, Fan, Donghua, Fang, Jian, Favart, Laurent, Ford, Richard, Göger Neff, Marianne, Gan, Haonan, Garfagnini, Alberto, Giammarchi, Marco, Gonchar, Maxim, Gong, Guanghua, Gong, Hui, Gonin, Michel, Grassi, Marco, Grewing, Christian, Guan, Mengyun, Guarino, Vic, Guo, Gang, Guo, Wanlei, Guo, Xin Heng, Hagner, Caren, Han, Ran, He, Miao, Heng, Yuekun, Hsiung, Yee, Hu, Jun, Hu, Shouyang, Hu, Tao, Huang, Hanxiong, Huang, Xingtao, Huo, Lei, Ioannisian, Ara, Jeitler, Manfred, Ji, Xiangdong, Jiang, Xiaoshan, Jollet, Cécile, Kang, Li, Karagounis, Michael, Kazarian, Narine, Krumshteyn, Zinovy, Kruth, Andre, Kuusiniemi, Pasi, Lachenmaier, Tobia, Leitner, Rupert, Li, Chao, Li, Jiaxing, Li, Weidong, Li, Weiguo, Li, Xiaomei, Li, Xiaonan, Li, Yi, Li, Yufeng, Li, Zhi Bing, Liang, Hao, Lin, Guey Lin, Lin, Tao, Lin, Yen Hsun, Ling, Jiajie, Lippi, Ivano, Liu, Dawei, Liu, Hongbang, Liu, Hu, Liu, Jianglai, Liu, Jianli, Liu, Jinchang, Liu, Qian, Liu, Shubin, Liu, Shulin, Lombardi, Paolo, Long, Yongbing, Lu, Haoqi, Lu, Jiashu, Lu, Jingbin, Lu, Junguang, Lubsandorzhiev, Bayarto, Ludhova, Livia, Luo, Shu, Vladimir Lyashuk, Null, Möllenberg, Randolph, Ma, Xubo, Mantovani, Fabio, Mao, Yajun, Mari, Stefano Maria, Mcdonough, William F, Meng, Guang, Meregaglia, Anselmo, Meroni, Emanuela, Mezzetto, Mauro, Miramonti, Lino, Thomas Mueller, Null, Naumov, Dmitry, Oberauer, Lothar, Ochoa Ricoux, Juan Pedro, Olshevskiy, Alexander, Ortica, Fausto, Paoloni, Alessandro, Peng, Haiping, Jen Chieh Peng, Null, Previtali, Ezio, Qi, Ming, Qian, Sen, Qian, Xin, Qian, Yongzhong, Qin, Zhonghua, Raffelt, Georg, Ranucci, Gioacchino, Ricci, Barbara, Robens, Marku, Romani, Aldo, Ruan, Xiangdong, Ruan, Xichao, Salamanna, Giuseppe, Shaevitz, Mike, Valery Sinev, Null, Sirignano, Chiara, Sisti, Monica, Smirnov, Oleg, Soiron, Michael, Stahl, Achim, Stanco, Luca, Steinmann, Jochen, Sun, Xilei, Sun, Yongjie, Taichenachev, Dmitriy, Tang, Jian, Tkachev, Igor, Trzaska, Wladyslaw, Waasen, Stefan van, Volpe, Cristina, Vorobel, Vit, Votano, Lucia, Wang, Chung Hsiang, Wang, Guoli, Wang, Hao, Wang, Meng, Wang, Ruiguang, Wang, Siguang, Wang, Wei, Wang, Yi, Wang, Yifang, Wang, Zhe, Wang, Zheng, Wang, Zhigang, Wang, Zhimin, Wei, Wei, Wen, Liangjian, Wiebusch, Christopher, Wonsak, Björn, Wu, Qun, Wulz, Claudia Elisabeth, Wurm, Michael, Xi, Yufei, Xia, Dongmei, Xie, Yuguang, Zhi zhong Xing, Null, Xu, Jilei, Yan, Baojun, Yang, Changgen, Yang, Chaowen, Yang, Guang, Yang, Lei, Yang, Yifan, Yao, Yu, Yegin, Ugur, Yermia, Frédéric, You, Zhengyun, Yu, Boxiang, Yu, Chunxu, Yu, Zeyuan, Zavatarelli, Sandra, Zhan, Liang, Zhang, Chao, Zhang, Hong Hao, Zhang, Jiawen, Zhang, Jingbo, Zhang, Qingmin, Zhang, Yu Mei, Zhang, Zhenyu, Zhao, Zhenghua, Zheng, Yangheng, Zhong, Weili, Zhou, Guorong, Zhou, Jing, Zhou, Li, Zhou, Rong, Zhou, Shun, Zhou, Wenxiong, Zhou, Xiang, Zhou, Yeling, Zhou, Yufeng, Zou, Jiaheng, Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Massachusetts Institute of Technology. Department of Physics, and Conrad, Janet Marie
Subjects: Particle physics, Sterile neutrino, Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Geoneutrino, reactor neutrino experiment, Physics::Instrumentation and Detectors, Solar neutrino, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, NO, High Energy Physics - Experiment, neutrino astronomy, High Energy Physics - Experiment (hep-ex), neutrino physics, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], ddc:530, neutrino, mass hierarchy, reactor, liquid scintillator, 010306 general physics, Jiangmen Underground Neutrino Observatory, media_common, Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, neutrino physic, Instrumentation and Detectors (physics.ins-det), Universe, reactor neutrino experiments, large scintillator detectors, Supernova, 13. Climate action, Physics::Space Physics, large scintillator detector, High Energy Physics::Experiment, Neutrino
Abstract: The Jiangmen Underground Neutrino Observatory (JUNO), a 20 kton multi-purpose underground liquid scintillator detector, was proposed with the determination of the neutrino mass hierarchy as a primary physics goal. It is also capable of observing neutrinos from terrestrial and extra-terrestrial sources, including supernova burst neutrinos, diffuse supernova neutrino background, geoneutrinos, atmospheric neutrinos, solar neutrinos, as well as exotic searches such as nucleon decays, dark matter, sterile neutrinos, etc. We present the physics motivations and the anticipated performance of the JUNO detector for various proposed measurements. By detecting reactor antineutrinos from two power plants at 53-km distance, JUNO will determine the neutrino mass hierarchy at a 3-4 sigma significance with six years of running. The measurement of antineutrino spectrum will also lead to the precise determination of three out of the six oscillation parameters to an accuracy of better than 1\%. Neutrino burst from a typical core-collapse supernova at 10 kpc would lead to ~5000 inverse-beta-decay events and ~2000 all-flavor neutrino-proton elastic scattering events in JUNO. Detection of DSNB would provide valuable information on the cosmic star-formation rate and the average core-collapsed neutrino energy spectrum. Geo-neutrinos can be detected in JUNO with a rate of ~400 events per year, significantly improving the statistics of existing geoneutrino samples. The JUNO detector is sensitive to several exotic searches, e.g. proton decay via the $p\to K^++\bar\nu$ decay channel. The JUNO detector will provide a unique facility to address many outstanding crucial questions in particle and astrophysics. It holds the great potential for further advancing our quest to understanding the fundamental properties of neutrinos, one of the building blocks of our Universe., Comment: Version submitted to Journal of Physics G, with minor typo corrections. 222 Pages, 147 figures
Published: 2016
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18. Theoretical developments in supernova neutrino physics : mass corrections and pairing correlators

Author: Cristina Volpe, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: History, Particle physics, Physics::Instrumentation and Detectors, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Correlation function (quantum field theory), mass: correction, 01 natural sciences, Education, High Energy Physics - Phenomenology (hep-ph), mean field approximation, 0103 physical sciences, neutrino: supernova, neutrino: mass, correlation function, 010306 general physics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), flavor, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Computer Science Applications, neutrino: propagation, star: massive, Stars, Supernova, Automatic Keywords, High Energy Physics - Phenomenology, Mean field theory, Astrophysics - Solar and Stellar Astrophysics, Pairing, correlation, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We highlight the progress in our understanding of how neutrinos change their flavor in astrophysical environments, in particular effects from the neutrino self-interaction. We emphasize extended descriptions of neutrino propagation in massive stars that are beyond the current one based on the mean-field approximation. The extended equations include, in particular, corrections from (anti)neutrino-(anti)neutrino pairing correlations and from the neutrino mass. We underline open issues and challenges., 5 pages, Proceedings for the TAUP 2015 conference
Published: 2015
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19. Neutrino astrophysics : recent advances and open issues

Author: Cristina Volpe
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), History, Nuclear Theory, Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, FOS: Physical sciences, Astrophysics, Computer Science Applications, Education, Nuclear Theory (nucl-th), Supernova, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics - Solar and Stellar Astrophysics, High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Nuclear theory, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We highlight recent advances in neutrino astrophysics, the open issues and the interplay with neutrino properties. We emphasize the important progress in our understanding of neutrino flavor conversion in media. We discuss the case of solar neutrinos, of core-collapse supernova neutrinos and of SN1987A, and of the recently discovered ultra-high energy neutrinos whose origin is to be determined., 14 pages, 8 figures, Proceedings for "DISCRETE 2014" Symposium
Published: 2015

20. Beta-beams

Author: Cristina Volpe
Subjects: Physics, Nuclear and High Energy Physics, Particle physics, 010308 nuclear & particles physics, 7. Clean energy, 01 natural sciences, Fundamental interaction, Cosmology, 0103 physical sciences, Nuclear astrophysics, Bibliography, Physics::Accelerator Physics, CP violation, High Energy Physics::Experiment, Neutrino, 010306 general physics, Neutrino oscillation, Lepton
Abstract: Neutrino physics is traversing an exciting period, after the important discovery that neutrinos are massive particles, that has implications from high-energy physics to cosmology. A new method for the production of intense and pure neutrino beams has been proposed recently: the ``beta-beam''. It exploits boosted radioactive ions decaying through beta-decay. This novel concept has been the starting point for a new possible future facility. Its main goal is to address the crucial issue of the existence of CP violation in the lepton sector. Here we review the status and the recent developments with beta-beams. We discuss the original, the medium and high-energy scenarios as well as mono-chromatic neutrino beams produced through ion electron-capture. The issue of the degeneracies is mentioned. An overview of low energy beta-beams is also presented. These beams can be used to perform experiments of interest for nuclear structure, for the study of fundamental interactions and for nuclear astrophysics.
Published: 2006
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21. Neutrino–nucleus interactions as a probe to constrain double-beta decay predictions

Author: Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, High Energy Physics - Experiment, Nuclear Theory (nucl-th), High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), Double beta decay, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], medicine, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010306 general physics, Physics, 010308 nuclear & particles physics, 3. Good health, Interaction studies, High Energy Physics - Phenomenology, medicine.anatomical_structure, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino, Nucleus
Abstract: We propose to use charged-current neutrino-nucleus interactions as a probe of the many virtual transitions involved in neutrinoless double-beta decay. By performing neutrino and anti-neutrino interaction studies on the initial and final nucleus respectively, one can get information on the two branches involved in the double-beta decay process. The measurement of such reactions could help to further constrain double-beta decay predictions on the half-lives., 4 pages, 4 figures
Published: 2005
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22. Neutrino-antineutrino correlations in dense anisotropic media

Author: Cristina Volpe and Julien Serreau
Subjects: Physics, High Energy Physics - Theory, Nuclear and High Energy Physics, Particle physics, Sterile neutrino, Neutrino theory of light, Nuclear Theory, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, FOS: Physical sciences, Solar neutrino problem, Nuclear Theory (nucl-th), Nuclear physics, MAJORANA, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), Astrophysics - Solar and Stellar Astrophysics, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Neutrino oscillation, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We derive the most general evolution equations describing in-medium (anti)neutrino propagation in the mean-field approximation. In particular, we consider various types of neutrino-antineutrino mixing, for both Dirac and Majorana fields, resulting either from nontrivial pair correlations or from helicity coherence due to the nonvanishing neutrino masses. We show that, unless the medium is spatially homogeneous and isotropic, these correlations are sourced by the usual neutrino and antineutrino densities. This may be of importance in astrophysical environments such as core-collapse supernovae., 16 pages
Published: 2014

23. Recent advances in neutrino astrophysics

Author: Cristina Volpe, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Nuclear Theory, supernova: particle source, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Physics::Instrumentation and Detectors, media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, neutrino: flux, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Nuclear theory, [ PHYS.NUCL ] Physics [physics]/Nuclear Theory [nucl-th], Solar and Stellar Astrophysics (astro-ph.SR), media_common, Physics, 010308 nuclear & particles physics, Particle interaction, High Energy Physics::Phenomenology, Universe, neutrino: UHE, particle: interaction, Supernova, High Energy Physics - Phenomenology, Astrophysics - Solar and Stellar Astrophysics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], neutrino: cosmic radiation, neutrino: flavor, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Neutrinos are produced by a variety of sources that comprise our Sun, explosive environments such as core-collapse supernovae, the Earth and the Early Universe. The precise origin of the recently discovered ultra-high energy neutrinos is to be determined yet. These weakly interacting particles give us information on their sources, although the neutrino fluxes can be modified when neutrinos traverse an astrophysical environment. Here we highlight recent advances in neutrino astrophysics and emphasise the important progress in our understanding of neutrino flavour conversion in media., Comment: Proceedings for the Symposium "Frontiers of Fundamental Physics 2014", July 15-18, Marseille, 8 pages, 1 figure
Published: 2014
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24. Linearizing neutrino evolution equations includingνν¯pairing correlations

Author: Daavid Väänänen and Cristina Volpe
Subjects: Physics, Nuclear and High Energy Physics, High Energy Physics::Phenomenology, Many-body theory, Equations of motion, Curvature, symbols.namesake, Mean field theory, Quantum electrodynamics, Pairing, symbols, High Energy Physics::Experiment, Neutrino, Hamiltonian (quantum mechanics), Eigenvalues and eigenvectors, Mathematical physics
Abstract: We linearize the neutrino mean-field evolution equations describing the neutrino propagation in a background of matter and of neutrinos, using techniques from many-body microscopic approaches. The procedure leads to an eigenvalue equation that allows to identify instabilities in the evolution, associated with a change of the curvature of the neutrino energy-density surface. Our result includes all contributions from the neutrino Hamiltonian and is generalizable to linearize the equations of motion at an arbitrary point of the evolution. We then consider the extended equations that comprise the normal mean field as well as the abnormal mean field that is associated with neutrino-antineutrino pairing correlations. We first re-derive the extended neutrino Hamiltonian and show that such a Hamiltonian can be diagonalized by introducing a generalized Bogoliubov-Valatin transformation with quasi-particle operators that mix neutrinos and antineutrinos. We give the eigenvalue equations that determine the energies of the quasi-particles eigenstates. Finally we derive the eigenvalue equation of the extended equations of motion, valid in the small amplitude approximation. Our results apply to an arbitrary number of neutrino families.
Published: 2013
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25. Extended evolution equations for neutrino propagation in astrophysical and cosmological environments

Author: Catalina Espinoza, Daavid Väänänen, Cristina Volpe, Ministerio de Ciencia e Innovación (España), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Nuclear Theory, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Early Universe, 01 natural sciences, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Core-collapse supernovae, 010306 general physics, Nuclear theory, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Cosmological model, 3. Good health, High Energy Physics - Phenomenology, Astrophysics - Solar and Stellar Astrophysics, Evolution equation, Christian ministry, High Energy Physics::Experiment, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We derive the evolution equations for a system of neutrinos interacting among themselves and with a matter background, based upon the Bogoliubov-Born-Green-Kirkwood-Yvon hierarchy. This theoretical framework gives an (unclosed) set of first-order coupled integro-differential equations governing the evolution of the reduced density matrices. By employing the hierarchy, we first rederive the mean-field evolution equations for the neutrino one-body density matrix associated with a system of neutrinos and antineutrinos interacting with matter and with an anisotropic neutrino background. Then, we derive extended evolution equations to determine neutrino flavor conversion beyond the commonly used mean-field approximation. To this aim we include neutrino-antineutrino pairing correlations to the two-body density matrix. The inclusion of these new contributions leads to an extended evolution equation for the normal neutrino density and to an equation for the abnormal one involving the pairing mean field. We discuss the possible impact of neutrino-antineutrino correlations on neutrino flavor conversion in the astrophysical and cosmological environments, and possibly upon the supernova dynamics. Our results can be easily generalized to an arbitrary number of neutrino families., C. V. thanks J. Serreau for useful discussions and careful reading of this manuscript. C. E. thanks CNRS/IN2P3 for financial support during an early stage of the project, and the Spanish Grant No. FPA 2008/02878 of Spanish Ministry MICINN. C. E. thanks IPN Orsay for the hospitality during the realization of the project.
Published: 2013
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26. Neutrino flavour conversion and supernovae

Author: Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], High Energy Physics::Lattice, Astrophysics::High Energy Astrophysical Phenomena, Flavour, High Energy Physics::Phenomenology, FOS: Physical sciences, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Supernova, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics - Solar and Stellar Astrophysics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 0103 physical sciences, High Energy Physics::Experiment, Neutrino, 010306 general physics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We summarize the recent developments in our understanding of neutrino flavour conversion in core-collapse supernovae and discuss open questions., Comment: Proceedings to the "Eleventh Conference on the Intersections of Particle and Nuclear Physics (CIPANP2012)", May 29 to June 3, Florida, 8 pages, 2 figures
Published: 2012
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27. Search for new physics with neutrinos at Radioactive Ion Beam facilities

Author: Rimantas Lazauskas, Cristina Volpe, and Catalina Espinoza
Subjects: Physics, Nuclear and High Energy Physics, Sterile neutrino, Particle physics, Ion beam, Physics::Instrumentation and Detectors, Solar neutrino, High Energy Physics::Phenomenology, FOS: Physical sciences, Solar neutrino problem, Nuclear physics, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Neutrino detector, Double beta decay, High Energy Physics::Experiment, Neutrino, Neutrino oscillation
Abstract: We propose applications of Radioactive Ion Beam facilities to investigate physics beyond the Standard Model. In particular, we focus on the possible measurement of coherent neutrino-nucleus scattering and on a search for sterile neutrinos, by means of a low energy beta-beam with a Lorentz boost factor $\gamma \approx 1$. In the considered setup the collected radioactive ions are sent inside a 4$\pi$ detector. For the first application we provide the number of events associated with neutrino-nucleus coherent scattering, when the detector is filled in with a noble liquid. For the sterile search we consider that the spherical detector is filled in with a liquid scintillator, and that the neutrino detection channel is inverse-beta decay. We provide the exclusion curves for the sterile neutrino mixing parameters, based upon the 3+1 formalism, depending upon the achievable ion intensity. Our results are obtained both from total rates, and including spectral information with binning in energy and in distance. The proposed experiment represents a possible alternative to clarify the current anomalies observed in neutrino experiments., Comment: 9 pages, 6 figures. v2 - added 2 figures
Published: 2012

28. The neutrino-neutrino interaction effects in supernovae: the point of view from the 'matter' basis

Author: Sebastien Galais, James P. Kneller, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Diagonal, FOS: Physical sciences, 01 natural sciences, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Neutrino oscillation, Eigenvalues and eigenvectors, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Phase derivative, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], High Energy Physics::Phenomenology, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Supernova, High Energy Physics - Phenomenology, Astrophysics - Solar and Stellar Astrophysics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], symbols, High Energy Physics::Experiment, Neutrino, Hamiltonian (quantum mechanics)
Abstract: We consider the Hamiltonian for neutrino oscillations in matter in the case of arbitrary potentials including off-diagonal complex terms. We derive the 'matter basis' Hamiltonian in terms of quantities one can derive from the flavor basis Hamiltonian and its derivative, for an arbitrary number of neutrino flavors. We make our expressions explicit for the two-neutrino flavor case and apply our results to the situation where the Hamiltonian includes both coupling to matter and to neutrinos, which describes neutrino propagation in core-collapse supernovae. We show that the neutrino flavour evolution depends on the mixing matrix derivatives involving not only the derivative of the matter mixing angles but also of the phases. In particular, we point out the important role of the phase derivatives, that appear due to the neutrino-neutrino interaction, and show how it can cause an oscillating degeneracy between the diagonal elements of the matter basis Hamiltonian. Our results also reveal, that the end of the synchronization regime is due to a rapid increase of the phase derivative, and identify the condition to be fulfilled for the onset of bipolar oscillations involving both the off-diagonal neutrino-neutrino interaction contributions and the vacuum terms., 11 pages, 5 figures, text and manuscript structure improved
Published: 2011
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29. The neutrino spectral split in core-collapse supernovae: a magnetic resonance phenomenon

Author: Sebastien Galais, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Elementary particle, Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Binary star, 010306 general physics, Neutrino oscillation, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], High Energy Physics::Phenomenology, Fermion, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Massless particle, High Energy Physics - Phenomenology, Supernova, Astrophysics - Solar and Stellar Astrophysics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Neutrino, Lepton
Abstract: A variety of neutrino flavour conversion phenomena occur in core-collapse supernova, due to the large neutrino density close to the neutrinosphere, and the importance of the neutrino-neutrino interaction. Three different regimes have been identified so far, usually called the synchronization, the bipolar oscillations and the spectral split. Using the formalism of polarization vectors, within two-flavours, we focus on the spectral split phenomenon and we show for the first time that the physical mechanism underlying the neutrino spectral split is a magnetic resonance phenomenon. In particular, we show that the precession frequencies fulfill the magnetic resonance conditions. Our numerical calculations show that the neutrino energies and the location at which the resonance takes place in the supernova coincide well with the neutrino energies at which a spectral swap occurs. The corresponding adiabaticity parameters present spikes at the resonance location., Comment: 11 pages, 9 figures, text and references added
Published: 2011
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30. Shock waves in supernovae: New implications on the diffuse supernova neutrino background

Author: James P. Kneller, Jerome Gava, Cristina Volpe, Sebastien Galais, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Shock wave, Physics, Nuclear and High Energy Physics, Particle physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Elementary particle, Fermion, Astrophysics, CHOOZ, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Massless particle, High Energy Physics - Phenomenology, Supernova, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Neutrino, 010306 general physics, Lepton
Abstract: We investigate shock wave effects upon the diffuse supernova neutrino background using dynamic profiles taken from hydrodynamical simulations and calculating the neutrino evolution in three flavors with the S-matrix formalism. We show that the shock wave impact is significant and introduces modifications of the relic fluxes by about $20 \%$ and of the associated event rates at the level of $10-20 \%$. Such an effect is important since it is of the same order as the rate variation introduced when different oscillation scenarios (i.e. hierarchy or $\theta_{13}$) are considered. In addition, due to the shock wave, the rates become less sensitive to collective effects, in the inverted hierarchy and when $\sin^2 2 \theta_{13}$ is between the Chooz limit and $10^{-5}$. We propose a simplified model to account for shock wave effects in future predictions., Comment: 8 pages, 9 figures
Published: 2010
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31. CP violation effects on the neutrino degeneracy parameters in the Early Universe

Author: Jerome Gava, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Nuclear and High Energy Physics, Particle physics, Neutrino theory of light, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], 010308 nuclear & particles physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, FOS: Physical sciences, Neutrino decoupling, 01 natural sciences, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Tau neutrino, 0103 physical sciences, Measurements of neutrino speed, CP violation, Degeneracy (biology), High Energy Physics::Experiment, Neutrino, 010306 general physics, Neutrino oscillation
Abstract: We explore possible CP violating effects, coming from the Dirac phase of the Maki-Nakagawa-Sakata-Pontecorvo matrix, on the neutrino degeneracy parameters, at the epoch of Big-Bang nucleosynthesis. We first demonstrate the conditions under which such effects can arise. In particular it requires that the initial muon and tau neutrino degeneracy parameters differ. Then we solve numerically the kinetic equations for the three flavour neutrino density matrix with the goal of quantifying the impact of the Dirac phase on the electron neutrino degeneracy parameter. The calculations include the vacuum term, the coupling to matter, the neutrino-neutrino interaction and the collisions. Effects on electron neutrino degeneracy parameter up to almost 1.% and on Yp of about 0.1% are found, depending on the initial conditions., 15 pages, 4 figures
Published: 2010
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32. Low-energy neutrino scattering measurements at future spallation source facilities

Author: R Lazauskas, Cristina Volpe, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Louis Pasteur - Strasbourg I, Institut de Physique Nucléaire, and Université Paris-Sud - Paris 11 (UP11)
Subjects: Nuclear and High Energy Physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 25.30.Pt, 01 natural sciences, 7. Clean energy, Nuclear physics, Nuclear Theory (nucl-th), 26.30.Jk, 26.30.Hj, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Spallation, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Muon, 010308 nuclear & particles physics, Electroweak interaction, High Energy Physics::Phenomenology, Weinberg angle, Massless particle, High Energy Physics - Phenomenology, Supernova, Astrophysics - Solar and Stellar Astrophysics, Physics::Accelerator Physics, High Energy Physics::Experiment, 97.60.Bw, Neutrino, Lepton
Abstract: In the future several Spallation Source facilities will be available worldwide. Spallation Sources produce large amount of neutrinos from decay-at-rest muons and thus can be well adapted to accommodate state-of-the-art neutrino experiments. In this paper low energy neutrino scattering experiments that can be performed at such facilities are reviewed. Estimation of expected event rates are given for several nuclei, electrons and protons at a detector located close to the source. A neutrino program at Spallation Sources comprises neutrino-nucleus cross section measurements relevant for neutrino and core-collapse supernova physics, electroweak tests and lepton-flavor violation searches., Comment: 12 pages, 4 figures, 5 tables
Published: 2010
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33. Turbulence effects on supernova neutrinos

Author: James P. Kneller, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nuclear and High Energy Physics, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], 010308 nuclear & particles physics, Turbulence, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, Resonance, FOS: Physical sciences, Astrophysics, 01 natural sciences, Mantle (geology), Computational physics, Physics::Fluid Dynamics, High Energy Physics - Phenomenology, Supernova, Amplitude, High Energy Physics - Phenomenology (hep-ph), Factorization, 13. Climate action, 0103 physical sciences, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics
Abstract: Multi-dimensional core-collapse supernova simulations exhibit turbulence of large amplitude and over large scales. As neutrinos pass through the supernova mantle the turbulence is expected to modify their evolution compared to the case where the explosion is free of turbulence. In this paper we study this turbulence effect upon the neutrinos modelling the turbulence expected from multi-dimensional simulations by adding matter density fluctuations to density profiles taken from one-dimensional hydrodynamical simulations. We investigate the impact upon the supernova neutrino transition probabilities as a function of the neutrino mixing angle theta_13 and turbulence amplitude. In the high (H) resonant channel and with large theta_13 values we find that turbulence is effectively two flavor for fluctuation amplitudes, Comment: New figure added
Published: 2010
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34. Dynamical Collective Calculation of Supernova Neutrino Signals

Author: Gail C. McLaughlin, Jerome Gava, James P. Kneller, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Particle physics, Nuclear Theory, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, 01 natural sciences, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Neutrino oscillation, Solar and Stellar Astrophysics (astro-ph.SR), Cherenkov radiation, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Solar neutrino problem, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], High Energy Physics - Phenomenology, Supernova, Astrophysics - Solar and Stellar Astrophysics, Neutrino detector, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Lepton
Abstract: We present the first calculations with three flavors of collective and shock wave effects for neutrino propagation in core-collapse supernovae using hydroynamical density profiles and the S matrix formalism. We explore the interplay between the neutrino-neutrino interaction and the effects of multiple resonances upon the time signal of positrons in supernova observatories. A specific signature is found for the inverted hierarchy and a large third neutrino mixing angle and we predict, in this case, a dearth of lower energy positrons in Cherenkov detectors midway through the neutrino signal and the simultaneous revelation of valuable information about the original fluxes. We show that this feature is also observable with current generation neutrino detectors at the level of several sigmas., Comment: 4 pages, 5 figures
Published: 2009
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35. Untangling supernova-neutrino oscillations with beta-beam data

Author: Gail C. McLaughlin, Natalie Jachowicz, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Nuclear and High Energy Physics, Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, Nuclear Theory (nucl-th), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Phenomenology (hep-ph), Nucleosynthesis, 0103 physical sciences, 010306 general physics, Neutrino oscillation, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), High Energy Physics::Phenomenology, Detector, Cosmic neutrino background, High Energy Physics - Phenomenology, Neutron star, Supernova, Physics and Astronomy, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Beta (plasma physics), Measurements of neutrino speed, 25.30Pt, High Energy Physics::Experiment, Supernova nucleosynthesis, Neutrino, Beam (structure)
Abstract: Recently, we suggested that low-energy beta-beam neutrinos can be very useful for the study of supernova neutrino interactions. In this paper, we examine the use of a such experiment for the analysis of a supernova neutrino signal. Since supernova neutrinos are oscillating, it is very likely that the terrestrial spectrum of supernova neutrinos of a given flavor will not be the same as the energy distribution with which these neutrinos were first emitted. We demonstrate the efficacy of the proposed method for untangling multiple neutrino spectra. This is an essential feature of any model aiming at gaining information about the supernova mechanism, probing proto-neutron star physics, and understanding supernova nucleosynthesis, such as the neutrino process and the r-process. We also consider the efficacy of different experimental approaches including measurements at multiple beam energies and detector configurations., Comment: 13 pages, 11 figures, accepted for publication in Phys. Rev. C
Published: 2009
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36. Search for CP violation in the lepton sector

Author: Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), 01 natural sciences, 7. Clean energy, Cosmology, High Energy Physics - Phenomenology (hep-ph), Nucleosynthesis, 0103 physical sciences, 010306 general physics, Baseline (configuration management), Physics, Core-collapse supernova, 010308 nuclear & particles physics, r-process, High Energy Physics::Phenomenology, Leptonic CP violation, Supernova, High Energy Physics - Phenomenology, Neutrinos masses and mixings, CP violation, High Energy Physics::Experiment, Neutrino, Beta-beams, Lepton
Abstract: One of the major open issues in neutrino physics is the possible existence of CP violation in the neutrino sector. Such an observation would have an important impact in various domains of physics, from high energy physics to cosmology. Its search requires future accelerator neutrino facilities producing intense and pure neutrino beams such as "beta-beams". Here we review the different beta-beam scenarios proposed so far and discuss the present status, with a particular emphasis on the original baseline scenario and its feasibility. Alternative strategies for the CP violation search are to be pursued as well. A possibility is to search for CP violation effects in astrophysical environments. Here we present recent analytical and numerical results obtained in the context of core-collapse supernovae. In particular, we point out the conditions under which there can be CP violating effects in dense media and show numerical results on the supernova (anti-)neutrino fluxes and on the electron fraction, relevant for the r-process nucleosynthesis., Comment: 12 pages
Published: 2009
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37. An 'archaeological' quest for galactic supernova neutrinos

Author: Cecilia Lunardini, Rimantas Lazauskas, Cristina Volpe, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Electron, Astrophysics, 7. Clean energy, 01 natural sciences, star formation, High Energy Physics - Phenomenology (hep-ph), Comparable size, 0103 physical sciences, 010306 general physics, Neutrino oscillation, supernova neutrinos, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], High Energy Physics::Phenomenology, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Supernova, High Energy Physics - Phenomenology, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, core-collapse supernovas, High Energy Physics::Experiment, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Neutrino
Abstract: We explore the possibility to observe the effects of electron neutrinos from past galactic supernovae, through a geochemical measurement of the amount of Technetium 97 produced by neutrino-induced reactions in a Molybdenum ore. The calculations we present take into account the recent advances in our knowledge of neutrino interactions, of neutrino oscillations inside a supernova, of the solar neutrino flux at Earth and of possible failed supernovae. The predicted Technetium 97 abundance is of the order of 10^7 atoms per 10 kilotons of ore, which is close to the current geochemical experimental sensitivity. Of this, 10-20% is from supernovae. Considering the comparable size of uncertainties, more precision in the modeling of neutrino fluxes as well as of neutrino cross sections is required for a meaningful measurement., Comment: PDFLateX, 22 pages, 2 Tables, 6 figures
Published: 2009
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38. Collective neutrino oscillations in matter and CP violation

Author: Jerome Gava, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Physics::Instrumentation and Detectors, Physics beyond the Standard Model, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, Standard Model, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Neutrino oscillation, Physics, Muon, 010308 nuclear & particles physics, Astrophysics (astro-ph), High Energy Physics::Phenomenology, High Energy Physics - Phenomenology, CP violation, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Lepton
Abstract: We explore CP violation effects on the neutrino propagation in dense environments, such as in core-collapse supernovae, where the neutrino self-interaction induces non-linear evolution equations. We demonstrate that the electron (anti)neutrino fluxes are not sensitive to the CP violating phase if the muon and tau neutrinos interact similarly with matter. On the other hand, we numerically show that new features arise, because of the non-linearity and the flux dependence of the evolution equations, when the muon and tau neutrinos have different fluxes at the neutrinosphere (due to loop corrections or of physics beyond the Standard Model). In particular, the electron (anti)neutrino probabilities and fluxes depend upon the CP violating phase. We also discuss the CP effects induced by radiative corrections to the neutrino refractive index., Comment: 8 pages and 9 figures
Published: 2008
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39. Low-energy neutrinos at off-axis from a standard beta-beam

Author: J. H. de Jesus, R. Lazauskas, Cristina Volpe, A. B. Balantekin, Institut de Physique Nucléaire d'Orsay (IPNO), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Nuclear and High Energy Physics, Particle physics, Nuclear Theory, Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, off-axis neutrino fluxes, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, Nuclear Theory (nucl-th), High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Neutrino oscillation, Nuclear Experiment, Physics, 010308 nuclear & particles physics, Detector, beta-beams, Solar neutrino problem, 13.15.+g,14.60.Lm,23.40.Bw,29.90.+r, High Energy Physics - Phenomenology, Neutrino detector, Low-energy neutrino interactions, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Measurements of neutrino speed, Physics::Accelerator Physics, High Energy Physics::Experiment, Neutrino, Beam (structure)
Abstract: We discuss a scenario to extract up to 150 MeV neutrinos at a standard beta-beam facility using one and two detectors off-axis. In particular we show that the high-energy component of the neutrino fluxes can be subtracted through a specific combination of the response of two off-axis detectors. A systematic analysis of the neutrino fluxes using different detector geometries is presented, as well as a comparison with the expected fluxes at a low-energy beta-beam facility. The presented option could offer an alternative way to perform low-energy neutrino experiments., Comment: 9 pages, 6 figures
Published: 2007
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40. Neutrino quantum kinetic equations

Author: Cristina Volpe
Subjects: Physics, Nuclear and High Energy Physics, Nuclear Theory, Many-body theory, FOS: Physical sciences, General Physics and Astronomy, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology, symbols.namesake, Supernova, Theoretical physics, High Energy Physics - Phenomenology (hep-ph), Astrophysics - Solar and Stellar Astrophysics, Mean field theory, Kinetic equations, Salient, Boltzmann constant, symbols, High Energy Physics::Experiment, Neutrino, Quantum, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Neutrinos propagate in astrophysical and cosmological environments modifying their flavor in intriguing ways. The study of neutrino propagation in media is based on the mean-field, extended mean-field and Boltzmann equations. We summarise salient features of these evolution equations and the methods employed so far to derive them. We emphasize applications to situations of observational interest., Comment: 19 pages, 1 figure, review for the special issue "Collective motion in nuclei, neutrinos, and neutron stars"
Published: 2015
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41. Conserved vector current test using low energy beta beams

Author: Cristina Volpe, A. B. Balantekin, J. H. de Jesus, R. Lazauskas, Institut de Physique Nucléaire d'Orsay (IPNO), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Physics, Nuclear and High Energy Physics, 13.15.+g, 23.40.Bw, 25.30.Pt, Current (mathematics), 010308 nuclear & particles physics, Magnetism, Detector, Current algebra, Form factor (quantum field theory), FOS: Physical sciences, form factors (elementary particles), 01 natural sciences, Nuclear physics, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Positron, neutrino-proton interactions, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 0103 physical sciences, current algebra, Beta (velocity), Sensitivity (control systems), 010306 general physics
Abstract: We discuss the possibility of testing the weak currents and, in particular, the weak magnetism term through the measurement of the electron anti-neutrinos capture by protons at a low energy beta-beam facility. We analyze the sensitivity using both the total number of events and the angular distribution of the positrons emitted in a water Cerenkov detector. We show that the weak magnetism form factor might be determined with better than several percent accuracy using the angular distribution. This offers a new way of testing the Conserved Vector Current hypothesis., 8 pages, 5 figures
Published: 2006
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42. Physics with a very first low-energy beta-beam

Author: Cristina Volpe, Girod, Dominique, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.NUCL] Physics [physics]/Nuclear Theory [nucl-th], Nuclear and High Energy Physics, Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], [PHYS.NEXP] Physics [physics]/Nuclear Experiment [nucl-ex], FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Astrophysics, 7. Clean energy, 01 natural sciences, Ion, Nuclear Theory (nucl-th), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Low energy, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Atomic and Molecular Physics, and Optics, 3. Good health, Interaction studies, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics - Phenomenology, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Beta (plasma physics), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Physics::Accelerator Physics, High Energy Physics::Experiment, Neutrino, Beam (structure)
Abstract: We describe the importance of having low-energy (10-100 MeV) neutrino beams produced through the decay of boosted radioactive ions (``beta-beams''). We focus on the interest for neutrino-nucleus interaction studies and their impact for astrophysics, nuclear and particle physics. In particular, we discuss the relation to neutrinoless double-beta decay. Finally, we mention the status as far as the feasibility of low-energy beta-beams is concerned., Comment: 5 pages, 2 figures, Proceedings to NUFACT05, June 21-26, 2005
Published: 2005

43. Neutrino-nucleus interactions: open questions and future projects

Author: Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Astrophysics, 01 natural sciences, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, medicine, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Physics, Focus (computing), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Atomic and Molecular Physics, and Optics, High Energy Physics - Phenomenology, medicine.anatomical_structure, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Physics::Accelerator Physics, Neutrino, Nucleus
Abstract: We discuss various issues concerning the interactions of nuclei with neutrinos of low impinging energies (i.e. having several tens of MeV to a few hundred MeV) of interest for particle physics, nuclear physics and astrophysics. We focus, in particular, on open questions as well as possible strategies to obtain more experimental information. The option of a low-energy beta-beam facility is extensively discussed. We also mention its potential concerning the neutrino magnetic moment., Comment: 8 pages, 4 figures, Proceedings to "Neutrino2004", 14-19 June 2004, Paris
Published: 2004
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44. What about a beta-beam facility for low energy neutrinos?

Author: Cristina Volpe, Arxiv, Import, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.NUCL] Physics [physics]/Nuclear Theory [nucl-th], Nuclear and High Energy Physics, Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], [PHYS.NEXP] Physics [physics]/Nuclear Experiment [nucl-ex], FOS: Physical sciences, Neutrino beam, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 7. Clean energy, 01 natural sciences, Collimated light, High Energy Physics - Experiment, Nuclear Theory (nucl-th), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), Low energy, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Interaction studies, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics - Phenomenology, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Physics::Accelerator Physics, Neutrino, Beam (structure)
Abstract: A novel method to produce neutrino beams has recently been proposed : the beta-beams. This method consists in using the beta-decay of boosted radioactive nuclei to obtain an intense, collimated and pure neutrino beam. Here we propose to exploit the beta-beam concept to produce neutrino beams of low energy. We discuss the applications of such a facility as well as its importance for different domains of physics. We focus, in particular, on neutrino-nucleus interaction studies of interest for various open issues in astrophysics, nuclear and particle physics. We suggest possible sites for a low energy beta-beam facility., 4 pages, 1 figure
Published: 2004

45. Neutrino-nucleus interaction rates at a low-energy beta-beam facility

Author: Cristina Volpe, Julien Serreau, Institut de Physique Nucléaire d'Orsay (IPNO), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Nuclear and High Energy Physics, Particle physics, Nuclear Theory, Physics::Instrumentation and Detectors, FOS: Physical sciences, Elementary particle, Astrophysics, 01 natural sciences, Nuclear physics, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 25.30.Pt, 26.50.+x, 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Charged current, Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Astrophysics (astro-ph), Fermion, Massless particle, High Energy Physics - Phenomenology, Neutrino detector, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Physics::Accelerator Physics, High Energy Physics::Experiment, Neutrino, Storage ring, Lepton
Abstract: We compute the neutrino detection rates to be expected at a low-energy beta-beam facility. We consider various nuclei as neutrino detectors and compare the case of a small versus large storage ring., Comment: 6 pages, 3 figures
Published: 2004
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46. Prospects for Detecting a Neutrino Magnetic Moment with a Tritium Source and Beta-beams

Author: Gail C. McLaughlin, Cristina Volpe, Institut de Physique Nucléaire d'Orsay (IPNO), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Physics::Instrumentation and Detectors, Solar neutrino, FOS: Physical sciences, Electron, 7. Clean energy, 01 natural sciences, Ion, Nuclear physics, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Physics, Magnetic moment, 010308 nuclear & particles physics, Scattering, 3. Good health, Bohr model, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Beta (plasma physics), symbols, High Energy Physics::Experiment, Neutrino
Abstract: We compare the prospects for detecting a neutrino magnetic moment by the measurement of neutrinos from a tritium source, reactors and low-energy beta-beams. In all cases the neutrinos or antineutrinos are detected by scattering of electrons. We find that a large (20 MCurie) tritium source could improve the limit on the neutrino magnetic moment significantly, down to the level of a few $\times 10^{-12}$ while low-energy beta-beams with sufficiently rapid production of ions could improve the limits to the level of a few $\times 10^{-11}$. The latter would require ion production at the rate of at least $10^{15}$ s$^{-1}$., Comment: 6 pages, 3 figures
Published: 2003
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47. Nucleosynthesis and the role of neutrinos: state of the art and open issues

Author: Cristina Volpe and A Baha Balantekin
Subjects: Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astronomy, Astrophysics, Universe, p-process, Neutron star, Stellar nucleosynthesis, Big Bang nucleosynthesis, Nucleosynthesis, Astrophysics::Solar and Stellar Astrophysics, r-process, Neutrino, Astrophysics::Galaxy Astrophysics, media_common
Abstract: Understanding the origin of the elements around us is one of the main quests of modern science. Realizing that only a few of the lightest elements can have been produced in the early Universe because of the lack of stable nuclei with A = 5 and A = 8, and that stars need to be producing some of the heavier nuclei up to iron so they may shine were triumphs of nuclear physics in the first part of the 20th century. For the synthesis of heavier elements the situation is more complicated. In particular, the site of r-process nucleosynthesis is still an open question. Suggested sites for r-process nucleosynthesis include the high-temperature, high-entropy region outside the newly formed neutron star in a core-collapse supernova, 4He mantles of the metal-poor (i.e. early) supernova progenitors, neutron-star mergers and accretion discs around black holes. The nucleosynthetic outcomes in such sites depend on their neutron- or proton-richness, which is determined by the astrophysical conditions as well as the properties of exotic nuclei, far from the valley of stability. A key development during the last few decades has been the appreciation of the close relationship between neutrinos and nucleosynthesis as physicists and astronomers ascertained the fact that neutrino properties figure prominently in many astrophysical environments. Neutrinos are involved in different types of stellar nucleosynthesis processes: the v-process, the v p process and the r-process. These developments have occurred in parallel with the impressive progress in our understanding of neutrino masses and mixings as well as neutrino flavour conversion in astrophysical (and cosmological) environments. Neutrino interactions with protons and neutrons impact the conditions for proton or neutron richness of a given site. Further investigations are necessary in order to fully unravel neutrino flavour conversion phenomena in these environments and to establish how much these finally impact the nucleosynthesis outcomes. To address the problem of nucleosynthesis one needs a three-pronged approach using experimental, observational and theoretical tools. The articles in this special issue, by renowned experts in the field, have been chosen to present the state-of-the-art in these three venues and show the intimate connection between the fundamental properties of neutrinos and nucleosynthesis.
Published: 2014
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48. Search for sterile neutrinos at radioactive ion beam facilities

Author: Cristina Volpe, Catalina Espinoza, and Rimantas Lazauskas
Subjects: Physics, History, Particle physics, Sterile neutrino, Ion beam, Physics::Instrumentation and Detectors, Physics beyond the Standard Model, High Energy Physics::Phenomenology, Scintillator, Computer Science Applications, Education, Ion, Nuclear physics, Neutrino detector, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino
Abstract: We propose applications of Radioactive Ion Beam facilities to investigate physics beyond the Standard Model. In particular, we focus upon the search for sterile neutrinos by means of a low energy beta-beam with a Lorentz boost factor of 1. In the considered setup, collected 8Li radioactive ions are sent inside a 4? detector filled with a liquid scintillator, with inverse-beta decay as neutrino detection channel. We provide exclusion curves for the sterile neutrino mixing parameters, based upon the 3+1 formalism, depending upon the achievable ion intensity. The proposed experiment represents a possible alternative to clarify the current anomalies observed in neutrino experiments.
Published: 2013
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49. Large underground, liquid based detectors for astro-particle physics in Europe: scientific case and prospects

Author: U. Moser, A. Meregaglia, T. Patzak, Jukka Maalampi, Michael Wurm, Michele Maltoni, A. de Bellefon, Matts Roos, L. Chaussard, A. Marchionni, Caren Hagner, J. Ebert, Manfred Lindner, D. Stefan, J. Busto, D. Autiero, L. B. Bezrukov, Georg G. Raffelt, N. Savvinov, R. Zimmermann, M. Hess, N. J. C. Spooner, I. Kreslo, G. Natterer, W. Gruber, C. Pistillo, L. Mosca, Juha Äystö, Mauro Mezzetto, L. Knecht, Wladyslaw Henryk Trzaska, V. A. Kudryavtsev, Ch. Cavata, T. Marrodán Undagoitia, Jan T. Sobczyk, J. Bouchez, A. Badertscher, André Rubbia, L. Oberauer, M. Laffranchi, Pasi Kuusiniemi, S. N. Gninenko, Biagio Rossi, J. E. Campagne, J. Winter, Arnold Milenko Müller, M. Messina, M. Göger-Neff, J. Marteau, J. Peltoniemi, Alessandro Mirizzi, P. K. Lightfoot, Y. Déclais, T. Schwetz, Antonio Ereditato, Antonio Bueno, J. Ulbricht, W. Potzel, P. Otiougova, J. Kisiel, Tobias Lachenmaier, F. von Feilitzsch, B. Lefievre, A. Zalewska, Cristina Volpe, J. Dumarchez, K. A. Hochmuth, A. Tonazzo, Timo Enqvist, P. Fileviez Perez, E. Rondio, Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Neutrinos, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), AstroParticule et Cosmologie (APC (UMR_7164)), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)-AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU)
Subjects: Physics, Particle physics, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Detector, Active detection, FOS: Physical sciences, Astronomy and Astrophysics, Scintillator, 01 natural sciences, Critical discussion, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 0103 physical sciences, Liquid argon, Liquid based, High Energy Physics::Experiment, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Neutrino, 010306 general physics, Particle Physics - Phenomenology
Abstract: This document reports on a series of experimental and theoretical studies conducted to assess the astro-particle physics potential of three future large-scale particle detectors proposed in Europe as next generation underground observatories. The proposed apparatus employ three different and, to some extent, complementary detection techniques: GLACIER (liquid Argon TPC), LENA (liquid scintillator) and MEMPHYS (\WC), based on the use of large mass of liquids as active detection media. The results of these studies are presented along with a critical discussion of the performance attainable by the three proposed approaches coupled to existing or planned underground laboratories, in relation to open and outstanding physics issues such as the search for matter instability, the detection of astrophysical- and geo-neutrinos and to the possible use of these detectors in future high-intensity neutrino beams., Comment: 50 pages, 26 figures
Published: 2007
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50. SN1987A and neutrino non-radiative decay

Author: Pilar Iváñez-Ballesteros and Maria Cristina Volpe
Subjects: Neutrino non-radiative decay, SN1987A, Core-collapse supernova neutrinos, Neutrino masses and mixings, Physics, QC1-999
Abstract: We investigate neutrino non-radiative two-body decay in vacuum, in relation to SN1987A. In a full 3ν decay framework, we perform a detailed likelihood analysis of the 24 neutrino events from SN1987A observed by Kamiokande-II, IMB, and Baksan. We consider both normal and inverted neutrino mass orderings, and the possibility of strongly hierarchical and quasi-degenerate neutrino mass patterns. The results of the likelihood analysis show that the sensitivity is too low to derive bounds in the case of normal mass ordering. On the contrary, in the case of inverted mass ordering we obtain the bound τ/m≥2.4×105 s/eV (1.2×105) s/eV at 68% (90%) CL on the lifetime-to-mass ratio of the mass eigenstates ν2 and ν1.
Published: 2023
Full Text: View/download PDF

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