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1. A technique for studying (n,p) reactions of astrophysical interest using radioactive beams with SECAR

Author

Tsintari Pelagia, Berg Georg P. A., Blackmon Jeff, Chipps Kelly, Couder Manoel, Deibel Catherine, Dimitrakopoulos Nikolaos, Garg Ruchi, Greife Uwe, Hermansen Kirby, Hood Ashley, Jain Rahul, Maher Cavan, Marshall Caleb, Meisel Zach, Miskovich Sara, Montes Fernando, Perdikakis Georgios, Pereira Jorge, Ruland Thomas, Schatz Hendrik, Setoodehnia Kiana, Smith Michael, Wagner Louis, and Zegers Remco G. T.

Subjects
Physics, QC1-999
Abstract

The formation of nuclei in slightly proton-rich regions of the neutrino-driven wind of core-collapse supernovae could be attributed to the neutrino-p process (νp-process). As it proceeds via a sequence of (p,γ) and (n,p) reactions, it may produce elements in the range of Ni and Sn, considering adequate conditions. Recent studies identify a number of decisive (n,p) reactions that control the efficiency of the νp-process. The study of one such (n,p) reaction via the measurement of the reverse (p,n) in inverse kinematics was performed with SECAR at NSCL/FRIB. Proton-induced reaction measurements, especially at the mass region of interest, are notably difficult since the recoils have nearly identical masses as the unreacted projectiles. Such measurements are feasible with the adequate separation level achieved with SECAR, and the in-coincidence neutron detection. Adjustments of the SECAR system for the first (p,n) reaction measurement included the development of new ion beam optics, and the installation of the neutron detection system. The aforementioned developments along with a discussion on the preliminary results of the p(58Fe,n)58Co reaction measurement are presented.

Published
2023
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2. Constraining nucleosythesis in neutrino-driven winds using the impact of (α, xn) reaction rates

Author

Psaltis Athanasios, Arcones Almudena, Avila Melina L., Jacobi Maximilian, Hansen Camilla Juul, Lombardo Linda, Meisel Zach, Mohr Peter, Montes Fernando, Ong Wei Jia, and Schatz Hendrik

Subjects
Physics, QC1-999
Abstract

The lighter heavy elements of the first r-process peak, between strontium and silver, can be synthesized in the moderately neutron-rich neutrino–driven ejecta of either core–collapse supernovae or neutron star mergers via the weak r–process. This nucleosynthesis scenario exhibits uncertainties from the absence of experimental data from (α, xn) reactions on neutron–rich nuclei, which are currently based on statistical model estimates. We have performed a new impact study to identify the most important (α, xn) reactions that can affect the production of the lighter heavy elements under different astrophysical conditions using new, constrained (α, xn) reaction rates based on the Atomki-V2 αOMP. Our results show how when reducing the nuclear physics uncertainties, we can use abundance ratios to constrain the astrophysical conditions/environment. This can be achieved in the near future, when the key (α, xn) reaction rates will be measured experimentally in radioactive beam facilities.

Published
2023
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3. First (p,n) reaction measurement in inverse kinematics with SECAR

Author

Tsintari Pelagia, Berg Georg, Blackmon Jeff, Chipps Kelly, Couder Manoel, Deibel Catherine, Dimitrakopoulos Nikolaos, Garg Ruchi, Greife Uwe, Hermansen Kirby, Hood Ashley, Jain Rahul, Maher Cavan, Marshall Caleb, Meisel Zach, Miskovich Sara, Montes Fernando, Perdikakis Georgios, Pereira Jorge, Ruland Thomas, Schatz Hendrik, Setoodehnia Kiana, Smith Michael, Wagner Louis, and Zegers Remco G.T.

Subjects
Physics, QC1-999
Abstract

Nucleosynthesis in the νp-process occurs in regions of slightly proton-rich nuclei in the neutrino-driven wind of core-collapse supernovae. The process proceeds via a sequence of (p,γ) and (n,p) reactions, and depending on the conditions, may produce elements between Ni and Sn. Recent studies show that a few key (n,p) reactions regulate the efficiency of the neutrino-p process (νp-process). We performed a study of one of such (n,p) reactions via the measurement of the reverse (p,n) in inverse kinematics with SECAR at NSCL/FRIB.Such proton-induced reaction measurements are particularly challenging, as the recoils and the unreacted projectiles have nearly identical masses. An appropriate separation level can be achieved with SECAR, and along with the incoincidence detection of neutrons these measurements become attainable. The preparation of the SECAR system for accommodating its first (p,n) reaction measurement, including the development of alternative ion beam optics, and the setup of the in-coincidence neutron detection, along with discussion on preliminary results from the p(58Fe,n)58Co reaction measurement are presented and discussed.

Published
2023
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5. SECAR: A recoil separator for nuclear astrophysics

Author

Tsintari Pelagia, Garg Ruchi, Berg Georg, Blackmon Jeff, Chipps Kelly, Couder Manoel, Deibel Catherine, Dimitrakopoulos Nikolaos, Greife Uwe, Hood Ashley, Jain Rahul, Marshall Caleb, Meisel Zach, Miskovich Sara, Montes Fernando, Perdikakis Georgios, Ruland Thomas, Schatz Hendrik, Setoodehnia Kiana, Smith Michael, and Wagner Louis

Subjects
Physics, QC1-999
Abstract

Proton-and alpha-capture reactions on unstable proton-rich nuclei power astrophysical explosions like novae and X-ray bursts. Direct measurements of these reactions are crucial for understanding the mechanisms behind these explosions and the nucleosynthesis at such sites. The recoil mass separator, SECAR (SEparator for CApture Reactions) at the National Superconducting Cyclotron Laboratory (NSCL) and the Facility for Rare Isotope Beams (FRIB), has been designed with the required sensitivity to study (p,γ) and (α,γ) reactions, directly at astrophysical energies in inverse kinematics, with radioactive beams of masses up to about A = 65. The complete SECAR system, including two Wien Filters for high mass resolution, has been installed at Michigan State University and is currently being commissioned. The present article introduces the SECAR concept, its scientific goals, and provides an update of the current status of the project.

Published
2022
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6. Sensitivity Study of Type-I X-ray Bursts to Nuclear Reaction Rates

Author

Sultana Irin, Estradé Alfredo, Borowiak Jessica, Elliott Jacob, Meyer Bradley S., and Schatz Hendrik

Subjects
Physics, QC1-999
Abstract

Type-I X-ray bursts are frequently occurring thermonuclear runaways on the surface of an accreting neutron star. The different nuclear reactions that empower the cataclysmic event play a key role in accurately comparing theoretical models and observations. We investigate the effect of the uncertainties in the nuclear reactions using a ONEZONE model for a set of different compositions and accretion rates that are within the range of the standard observed burst sources. A combination of a full-reaction network and a semi-analytic model is used to obtain the conditions at the time of X-ray burst ignition via simulating the settling process of the accreted material. We then evaluate the sensitivity of the X-ray burst model by varying the proton and alpha-induced reaction rates in JINA REACLIBV2.2 within representative nuclear physics uncertainties.

Published
2022
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7. Observatory science with eXTP

Author

in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael

Published
2018
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8. Dense matter with eXTP

Author

Watts, Anna L., Yu, WenFei, Poutanen, Juri, Zhang, Shu, Bhattacharyya, Sudip, Bogdanov, Slavko, Ji, Long, Patruno, Alessandro, Riley, Thomas E., Bakala, Pavel, Baykal, Altan, Bernardini, Federico, Bombaci, Ignazio, Brown, Edward, Cavecchi, Yuri, Chakrabarty, Deepto, Chenevez, Jérôme, Degenaar, Nathalie, Del Santo, Melania, Di Salvo, Tiziana, Doroshenko, Victor, Falanga, Maurizio, Ferdman, Robert D., Feroci, Marco, Gambino, Angelo F., Ge, MingYu, Greif, Svenja K., Guillot, Sebastien, Gungor, Can, Hartmann, Dieter H., Hebeler, Kai, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Zand, Jean in’t, Kargaltsev, Oleg, Kurkela, Aleksi, Lai, XiaoYu, Li, Ang, Li, XiangDong, Li, ZhaoSheng, Linares, Manuel, Lu, FangJun, Mahmoodifar, Simin, Méndez, Mariano, Coleman Miller, M., Morsink, Sharon, Nättilä, Joonas, Possenti, Andrea, Prescod-Weinstein, Chanda, Qu, JinLu, Riggio, Alessandro, Salmi, Tuomo, Sanna, Andrea, Santangelo, Andrea, Schatz, Hendrik, Schwenk, Achim, Song, LiMing, Šrámková, Eva, Stappers, Benjamin, Stiele, Holger, Strohmayer, Tod, Tews, Ingo, Tolos, Laura, Török, Gabriel, Tsang, David, Urbanec, Martin, Vacchi, Andrea, Xu, RenXin, Xu, YuPeng, Zane, Silvia, Zhang, GuoBao, Zhang, ShuangNan, Zhang, WenDa, Zheng, ShiJie, and Zhou, Xia

Published
2018
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9. X-ray burst studies with the JENSA gas jet target

Author

Schmidt Konrad, Chipps Kelly A., Ahn Sunghoon, Allen Jacob M., Ayoub Sara, Bardayan Daniel W., Blackmon Jeffrey C., Blankstein Drew, Browne Justin, Cha Soomi, Chae Kyung YUK, Cizewski Jolie, Deibel Catherine M., Deleeuw Eric, Gomez Orlando, Greife Uwe, Hager Ulrike, Hall Matthew R., Jones Katherine L., Kontos Antonios, Kozub Raymond L., Lee Eunji, Lepailleur Alex, Linhardt Laura E., Matos Milan, Meisel Zach, Montes Fernando, O’Malley Patrick D., Ong Wei Jia, Pain Steven D., Sachs Alison, Schatz Hendrik, Schmitt Kyle T., Smith Karl, Smith Michael S., Soares de Bem Natã F., Thompson Paul J., Toomey Rebecca, and Walter David

Subjects
Physics, QC1-999
Abstract

When a neutron star accretes hydrogen and helium from the outer layers of its companion star, thermonuclear burning enables the αp-process as a break out mechanism from the hot CNO cycle. Model calculations predict (α, p) reaction rates significantly affect both the light curves and elemental abundances in the burst ashes. The Jet Experiments in Nuclear Structure and Astrophysics (JENSA) gas jet target enables the direct measurement of previously inaccessible (α,p) reactions with radioactive beams provided by the rare isotope re-accelerator ReA3 at the National Superconducting Cyclotron Laboratory (NSCL), USA. JENSA is going to be the main target for the Recoil Separator for Capture Reactions (SECAR) at the Facility for Rare Isotope Beams (FRIB). Commissioning of JENSA and first experiments at Oak Ridge National Laboratory (ORNL) showed a highly localized, pure gas target with a density of ∼1019 atoms per square centimeter. Preliminary results are presented from the first direct cross section measurement of the 34Ar(α, p)37 K reaction at NSCL.

Published
2017
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10. Constraining the rp-process by measuring 23Al(d,n)24Si with GRETINA and LENDA at NSCL

Author

Wolf Clemens, Langer Christoph, Montes Fernando, Pereira Jorge, Ahn Sunghoon, Ayoub Sara, Bazin Daniel, Bender Peter, Brown Alex, Browne Justin, Crawford Heather, Deleeuw Eric, Elman Brandon, Fiebiger Stefan, Gade Alexandra, Gastis Panagiotis, Lipschutz Samuel, Longfellow Brenden, Nunes Filomena, Ong Wei-Jia, Poxon-Pearson Terri, Perdikakis Georgios, Reifarth René, Schatz Hendrik, Schmidt Konrad, Schmitt Jaclyn, Sullivan Chris, Titus Rachel, Weisshaar Dirk, Woods Philip, Zamora Juan Carlos, and G.T. Zegers Remco

Subjects
Physics, QC1-999
Abstract

The 23Al(p, γ)24Si stellar reaction rate has a significant impact on the light-curve emitted in X-ray bursts. Theoretical calculations show that the reaction rate is mainly determined by the properties of direct capture as well as low-lying 2+ states and a possible 4+ state in 24Si. Currently, there is little experimental information on the properties of these states. In this proceeding we will present a new experimental study to investigate this reaction, using the surrogate reaction 23Al(d,n) at 47 AMeV at the National Superconducting Cyclotron Laboratory (NSCL). We will discuss our new experimental setup which allows us to use full kinematics employing the Gamma-Ray Energy Tracking In-beam Nuclear Array (GRETINA) to detect the γ-rays following the de-excitation of excited states of the reaction products and the Low Energy Neutron Detector Array (LENDA) to detect the recoiling neutrons. The S800 was used for identification of the 24Si recoils. As a proof of principle to show the feasibility of this concept the Q-value spectrum of 22Mg(d,n)23Al is reconstructed.

Published
2017
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11. White Paper on Nuclear Astrophysics and Low Energy Nuclear Physics Part 1: Nuclear Astrophysics

Author

Arcones, Almudena, Bardayan, Dan W, Beers, Timothy C, Bernstein, Lee A, Blackmon, Jeffrey C, Messer, Bronson, Brown, B. Alex, Brown, Edward F, Brune, Carl R, Champagne, Art E, Chieffi, Alessandro, Couture, Aaron J, Danielewicz, Pawel, Diehl, Roland, El-Eid, Mounib, Escher, Jutta E, Fields, Brian D, Frohlich, Carla, Herwig, Falk, Hix, William Raphael, Iliadis, Christian, Lynch, William G, McLaughlin, Gail C, Meyer, Bradley S, Mezzacappa, Anthony, Nunes, Filomena, O’Shea, Brian W, Prakash, Madappa, Pritychenko, Boris, Reddy, Sanjay, Rehm, Ernst, Rogachev, Grigory, Rutledge, Robert E, Schatz, Hendrik, Smith, Michael S, Stairs, Ingrid H, Steiner, Andrew W, Strohmayey, Tod E, Timmes, F. X, Townsley, Dean M, Wiescher, Michael, Zegers, Remco G. T, and Zingale, Michael

Subjects
Astrophysics, Nuclear Physics
Abstract

This white paper informs the nuclear astrophysics community and funding agencies about the scientific directions and priorities of the field and provides input from this community for the 2015 Nuclear Science Long Range Plan. It summarizes the outcome of the nuclear astrophysics town meeting that was held on August 21-23, 2014 in College Station at the campus of Texas AM University in preparation of the NSAC Nuclear Science Long Range Plan. It also reflects the outcome of an earlier town meeting of the nuclear astrophysics community organized by the Joint Institute for Nuclear Astrophysics (JINA) on October 9-10, 2012 Detroit, Michigan, with the purpose of developing a vision for nuclear astrophysics in light of the recent NRC decadal surveys in nuclear physics (NP2010) and astronomy (ASTRO2010). The white paper is furthermore informed by the town meeting of the Association of Research at University Nuclear Accelerators (ARUNA) that took place at the University of Notre Dame on June 12-13, 2014. In summary we find that nuclear astrophysics is a modern and vibrant field addressing fundamental science questions at the intersection of nuclear physics and astrophysics. These questions relate to the origin of the elements, the nuclear engines that drive life and death of stars, and the properties of dense matter. A broad range of nuclear accelerator facilities, astronomical observatories, theory efforts, and computational capabilities are needed. With the developments outlined in this white paper, answers to long standing key questions are well within reach in the coming decade.

Published
2015
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12. Observatory science with eXTP

Author

in't Zand, Jean J. M., Bozzo, Enrico, Qu, Jinlu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, De Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, Xuefeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, Joao, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, Chichuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aì, Antonino, Dai, Zi-Gao, D'Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D'Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, Xilong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, Mingyu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, Fangjun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, Yunpeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O'Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, Lijing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, Junfeng, Watts, Anna L., Weng, Shanshan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, Shaolin, Xu, Yupeng, Yan, Zhen, Younes, George, Yu, Wenfei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean, Drake, Stephen, Jenke, Peter, Maccarone, Thomas, Rossi, Elena, Tauris, Thomas, Andersson, Nils, Ballantyne, David, Brown, Edward, Cackett, Edward, D’Aì, Antonino, D’Ammando, Filippo, D’Elia, Valerio, Ferdman, Robert, Galloway, Duncan, Gambino, Angelo, Heinke, Craig, Jonker, Peter, Kaastra, Jelle, Lutovinov, Alexander, Mignani, Roberto, O’Brien, Paul, Osborne, Julian, Papadakis, Iossif, Pérez Torres, Miguel, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Torres, Diego, Watts, Anna, Weinberg, Nevin, Wheatley, Peter, Woods, Tyrone, Woosley, Stan, Zdziarski, Andrzej, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Lauren, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Deny, Malzac, Julien, Manousakis, Antonio, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joona, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuoma, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jirí, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), eXTP, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherche en Information Biomédicale sino-français (CRIBS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Southeast University [Jiangsu]-Institut National de la Santé et de la Recherche Médicale (INSERM), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), ASI Science Data Center (ASDC), Italian Space Agency, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Anthropobiologie (LA), École des hautes études en sciences sociales (EHESS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), SRON Netherlands Institute for Space Research (SRON), Istituto di Radioastronomia [Bologna] (IRA), KAUST Catalysis Center (KCC), King Abdullah University of Sciences & Technologie, IASF, Area di Ricerca di Tor Vergata, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-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), School of Physics and Astronomy [Southampton], University of Southampton, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut für Astrophysik [Wien], Universität Wien, Sabanci University [Istanbul], The George Washington University (GW), Department of Physics, Tokyo Institute of Technology [Tokyo] (TITECH), Deakin University [Burwood], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), University of New Hampshire (UNH), Department of Mechanical and Industrial Engineering [Trondheim] (MTP NTNU), Norwegian University of Science and Technology [Trondheim] (NTNU), Norwegian University of Science and Technology (NTNU)-Norwegian University of Science and Technology (NTNU), Ethoikos, Radicondoli, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Sichuan University [Chengdu] (SCU), University of Warwick [Coventry], U.S. Department of Energy [Washington] (DOE), University College of London [London] (UCL), Medical School (University of Nanjing), Nanjing University (NJU), Beijing Municipal Climate Center, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Informática [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), NLD, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, National Natural Science Foundation of China (NSFC), European Research Council (ERC), National Aeronautics and Space Administration (NASA), Agencia Estatal de Investigación (AEI), Royal Society, Strategic Priority Research Program of the Chinese Academy of Sciences, National Science Centre, Poland (NCN), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, Astronomy, Discrete Technology and Production Automation, in't Zand, Jean J. M., Qu, Jinlu, Tauris, Thomas M., Wilm, Joern, Wu, Xuefeng, Jin, Chichuan, D'Aì, Antonino, D'Ammando, Filippo, D'Elia, Valerio, Fan, Xilong, Ge, Mingyu, Lu, Fangjun, Mchardy, Ian, Men, Yunpeng, O'Brien, Paul T., Shao, Lijing, Svoboda, Jir̆í, Thielemann, F. -K., Wang, Junfeng, Weng, Shanshan, Xiong, Shaolin, Xu, Yupeng, Yu, Wenfei, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Osservatorio Astronomico di Brera, Istituto di Radioastronomia (IRA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), George Washington University (GW), Department of Mechanical and Industrial Engineering [Trondheim], Sichuan University, U.S. Department of Energy (DOE), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), SRON Netherlands Institute for Space Research, University of Geneva, CAS - Institute of High Energy Physics, Nanjing University, INAF/IASF Bologna, National Institute for Astrophysics, University of Tübingen, NASA Goddard Space Flight Center, ICREA, University of Alabama in Huntsville, Texas Tech University, Osservatorio Astronomico di Capodimonte, Leiden University, University of Amsterdam, Polytechnic University of Catalonia, University of Urbino, Max Planck Institute for Radio Astronomy, Friedrich-Alexander University Erlangen-Nürnberg, CAS - Purple Mountain Observatory, CSIC, IRAP, New York University Abu Dhabi, Georgia Institute of Technology, Middle East Technical University, Technion-Israel Institute of Technology, Tata Institute of Fundamental Research, Roma Tre University, Instituto de Astrofísica de Canarias, Instituto Nacional de Pesquisas Espaciais, Danmarks Tekniske Universitet, Michigan State University, Osservatorio Astrofisico Di Arcetri, Florence, University of Cagliari, Wayne State University, Osservatorio Astronomico Roma, CAS - Shanghai Astronomical Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University

Subjects
cataclysmic binaries, Astronomy, FIELD CAMERAS OBSERVATIONS, space research instruments nuclear astrophysics flare stars accretion and accretion disks mass loss and stellar winds cataclysmic binaries X-ray binaries supernova remnants active galactic nuclei X-ray bursts gamma-ray bursts gravitational waves, General Physics and Astronomy, gamma-ray burst, space research instrument, 01 natural sciences, Gamma ray bursts, Observatory, Accretion and accretion disks, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, gravitational wave, accretion and accretion disk, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], flare stars, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, accretion and accretion disks, active galactic nuclei, gravitational waves, mass loss and stellar winds, nuclear astrophysics, space research instruments, X-ray binaries, X-ray bursts, Physics and Astronomy (all), Space research instruments, X ray burst, Supernova, QUIET, High mass, X-ray binarie, Mass loss and stellar winds, Nuclear astrophysics, Gamma-ray bursts, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, FAST RADIO-BURSTS, Astrofísica nuclear, Active galactic nucleus, TIDAL DISRUPTION, Supernova remnants, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, ACCRETING NEUTRON-STARS, Gravitational waves, cataclysmic binarie, Settore FIS/05 - Astronomia e Astrofisica, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, 010306 general physics, X-ray burst, Astrophysics::Galaxy Astrophysics, Cataclysmic binaries, Active galactic nuclei, flare star, White dwarf, Flare stars, Stars, supernova remnant, QB460-466 Astrophysics, [SDU]Sciences of the Universe [physics], mass loss and stellar wind, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], X-RAY, Supernova remmants, X ray binaries, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SEYFERT 1 GALAXY, nuclear astrophysic
Abstract

Disponible preprint en: arXiv:1812.04023v1 [astro-ph.HE] [v1] Mon, 10 Dec 2018 19:00:52 UTC (4,376 KB), In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.© 2018, Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature., This work was supported by the Royal Society, ERC Starting (Grant No. 639217), the European Union Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Global Fellowship (Grant No. 703916), the National Natural Science Foundation of China (Grant Nos. 11233001, 11773014, 11633007, 11403074, 11333005, 11503008, and 11590781), the National Basic Research Program of China (Grant No. 2015CB857100), NASA (Grant No. NNX13AD28A), an ARC Future Fellowship (Grant No. FT120100363), the National Science Foundation (Grant No. PHY-1430152), the Spanish MINECO (Grant No. AYA2016-76012-C3-1-P), the ICCUB (Unidad de Excelencia 'Maria de Maeztu') (Grant No. MDM-2014-0369), EU's Horizon Programme through a Marie Sklodowska-Curie Fellowship (Grant No. 702638), the Polish National Science Center (Grant Nos. 2015/17/B/ST9/03422, 2015/18/M/ST9/00541, 2013/10/M/ST9/00729, and 2015/18/A/ST9/00746), the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA15020100), and the NWO Veni Fellowship (Grant No. 639.041.647).

Published
2019
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14. Catching Element Formation In The Act. The Case for a New MeV Gamma-Ray Mission: Radionuclide Astronomy in the 2020s. A White Paper for the 2020 Decadal Survey

Author

Fryer, Chris L., Timmes, Frank, Hungerford, Aimee L., Couture, Aaron, Adams, Fred, Aoki, Wako, Arcones, Almudena, Arnett, David, Auchettl, Katie, Avila, Melina, Badenes, Carles, Baron, Eddie, Bauswein, Andreas, John Beacom, Blackmon, Jeff, Blondin, Stéphane, Bloser, Peter, Boggs, Steve, Boss, Alan, Brandt, Terri, Bravo, Eduardo, Brown, E., Brown, Peter, Bruenn, Steve, Budtz-Jørgensen, Carl, Burns, Eric, Calder, Alan, Caputo, Regina, Champagne, Art, Chevalier, Roger, Chieffi, Alessandro, Chipps, Kelly, Cinabro, David, Clarkson, Ondrea, Clayton, Don, Coc, Alain, Connolly, Devin, Conroy, Charlie, Côté, Benoit, Couch, Sean, Dauphas, Nicolas, Deboer, Richard James, Deibel, Catherine, Denisenkov, Pavel, Desch, Steve, Dessart, Luc, Diehl, Roland, Doherty, Carolyn, Domínguez, Inma, Dong, Subo, Dwarkadas, Vikram, Fan, Doreen, Fields, Brian, Fields, Carl, Filippenko, Alex, Fisher, Robert, Foucart, Francois, Fransson, Claes, Fröhlich, Carla, Fuller, George, Gibson, Brad, Giryanskaya, Viktoriya, Görres, Joachim, Goriely, Stéphane, Grebenev, Sergei, Grefenstette, Brian, Grohs, Evan, Guillochon, James, Harpole, Alice, Harris, Chelsea, Austin Harris, J., Harrison, Fiona, Hartmann, Dieter, Hashimoto, Masa-Aki, Heger, Alexander, Hernanz, Margarita, Herwig, Falk, Hirschi, Raphael, Hix, Raphael William, Höflich, Peter, Hoffman, Robert, Holcomb, Cole, Hsiao, Eric, Iliadis, Christian, Janiuk, Agnieszka, Janka, Thomas, Jerkstrand, Anders, Johns, Lucas, Jones, Samuel, José, Jordi, Kajino, Toshitaka, Karakas, Amanda, Karpov, Platon, Kasen, Dan, Kierans, Carolyn, Kippen, Marc, Korobkin, Oleg, Kobayashi, Chiaki, Kozma, Cecilia, Krot, Saha, Kumar, Pawan, Kuvvetli, Irfan, Laird, Alison, Laming, Martin, Larsson, Josefin, Lattanzio, John, Lattimer, James, Leising, Mark, Lennarz, Annika, Lentz, Eric, Limongi, Marco, Lippuner, Jonas, Livne, Eli, Lloyd-Ronning, Nicole, Longland, Richard, Lopez, Laura A., Lugaro, Maria, Lutovinov, Alexander, Madsen, Kristin, Malone, Chris, Matteucci, Francesca, Mcenery, Julie, Meisel, Zach, Messer, Bronson, Metzger, Brian, Meyer, Bradley, Meynet, Georges, Mezzacappa, Anthony, Miller, Jonah, Miller, Richard, Milne, Peter, Misch, Wendell, Mitchell, Lee, Mösta, Philipp, Motizuki, Yuko, Müller, Bernhard, Mumpower, Matthew, Murphy, Jeremiah, Nagataki, Shigehiro, Nakar, Ehud, Nomoto, Ken Ichi, Nugent, Peter, Nunes, Filomena, O Shea, Brian, Oberlack, Uwe, Pain, Steven, Parker, Lucas, Perego, Albino, Pignatari, Marco, Pinedo, Gabriel Martínez, Plewa, Tomasz, Poznanski, Dovi, Priedhorsky, William, Pritychenko, Boris, Radice, David, Ramirez-Ruiz, Enrico, Rauscher, Thomas, Reddy, Sanjay, Rehm, Ernst, Reifarth, Rene, Richman, Debra, Ricker, Paul, Rijal, Nabin, Roberts, Luke, Röpke, Friedrich, Rosswog, Stephan, Ruiter, Ashley J., Ruiz, Chris, Savin, Daniel Wolf, Schatz, Hendrik, Schneider, Dieter, Schwab, Josiah, Seitenzahl, Ivo, Shen, Ken, Siegert, Thomas, Sim, Stuart, Smith, David, Smith, Karl, Smith, Michael, Sollerman, Jesper, Sprouse, Trevor, Spyrou, Artemis, Starrfield, Sumner, Steiner, Andrew, Strong, Andrew W., Sukhbold, Tuguldur, Suntzeff, Nick, Surman, Rebecca, Tanimori, Toru, The, Lih-Sin, Thielemann, Friedrich-Karl, Tolstov, Alexey, Tominaga, Nozomu, Tomsick, John, Townsley, Dean, Tsintari, Pelagia, Tsygankov, Sergey, Vartanyan, David, Venters, Tonia, Vestrand, Tom, Vink, Jacco, Waldman, Roni, Wang, Lifang, Wang, Xilu, Warren, Mackenzie, West, Christopher, Craig Wheeler, J., Wiescher, Michael, Winkler, Christoph, Winter, Lisa, Wolf, Bill, Woolf, Richard, Woosley, Stan, Wu, Jin, Wrede, Chris, Yamada, Shoichi, Young, Patrick, Zegers, Remco, Zingale, Michael, Portegies Zwart, Simon, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), 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), European Space Agency (ESA), HEP, INSPIRE, 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
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

Gamma-ray astronomy explores the most energetic photons in nature to address some of the most pressing puzzles in contemporary astrophysics. It encompasses a wide range of objects and phenomena: stars, supernovae, novae, neutron stars, stellar-mass black holes, nucleosynthesis, the interstellar medium, cosmic rays and relativistic-particle acceleration, and the evolution of galaxies. MeV gamma-rays provide a unique probe of nuclear processes in astronomy, directly measuring radioactive decay, nuclear de-excitation, and positron annihilation. The substantial information carried by gamma-ray photons allows us to see deeper into these objects, the bulk of the power is often emitted at gamma-ray energies, and radioactivity provides a natural physical clock that adds unique information. New science will be driven by time-domain population studies at gamma-ray energies. This science is enabled by next-generation gamma-ray instruments with one to two orders of magnitude better sensitivity, larger sky coverage, and faster cadence than all previous gamma-ray instruments. This transformative capability permits: (a) the accurate identification of the gamma-ray emitting objects and correlations with observations taken at other wavelengths and with other messengers; (b) construction of new gamma-ray maps of the Milky Way and other nearby galaxies where extended regions are distinguished from point sources; and (c) considerable serendipitous science of scarce events -- nearby neutron star mergers, for example. Advances in technology push the performance of new gamma-ray instruments to address a wide set of astrophysical questions.

Published
2019

15. Catching Element Formation In The Act.:The Case for a New MeV Gamma-Ray Mission: Radionuclide Astronomy in the 2020s. A White Paper for the 2020 Decadal Survey

Author

Fryer, Chris L., Timmes, Frank, Hungerford, Aimee L., Couture, Aaron, Adams, Fred, Aoki, Wako, Arcones, Almudena, Arnett, David, Auchettl, Katie, Avila, Melina, Badenes, Carles, Baron, Eddie, Bauswein, Andreas, Beacom, John, Blackmon, Jeff, Blondin, Stephane, Bloser, Peter, Boggs, Steve, Boss, Alan, Brandt, Terri, Bravo, Eduardo, Brown, Ed, Brown, Peter, Budtz-Jorgensen, Steve Bruenn. Carl, Burns, Eric, Calder, Alan, Caputo, Regina, Champagne, Art, Chevalier, Roger, Chieffi, Alessandro, Chipps, Kelly, Cinabro, David, Clarkson, Ondrea, Clayton, Don, Coc, Alain, Connolly, Devin, Conroy, Charlie, Cote, Benoit, Couch, Sean, Dauphas, Nicolas, deBoer, Richard James, Deibel, Catherine, Denisenkov, Pavel, Desch, Steve, Dessart, Luc, Diehl, Roland, Doherty, Carolyn, Dominguez, Inma, Dong, Subo, Dwarkadas, Vikram, Fan, Doreen, Fields, Brian, Fields, Carl, Filippenko, Alex, Fisher, Robert, Foucart, Francois, Fransson, Claes, Frohlich, Carla, Fuller, George, Gibson, Brad, Giryanskaya, Viktoriya, Gorres, Joachim, Goriely, Stephane, Grebenev, Sergei, Grefenstette, Brian, Grohs, Evan, Guillochon, James, Harpole, Alice, Harris, Chelsea, Harris, J. Austin, Harrison, Fiona, Hartmann, Dieter, Hashimoto, Masa-aki, Heger, Alexander, Hernanz, Margarita, Herwig, Falk, Hirschi, Raphael, Hix, Raphael William, Hoflich, Peter, Hoffman, Robert, Holcomb, Cole, Hsiao, Eric, Iliadis, Christian, Janiuk, Agnieszka, Janka, Thomas, Jerkstrand, Anders, Johns, Lucas, Jones, Samuel, Jose, Jordi, Kajino, Toshitaka, Karakas, Amanda, Karpov, Platon, Kasen, Dan, Kierans, Carolyn, Kippen, Marc, Korobkin, Oleg, Kobayashi, Chiaki, Kozma, Cecilia, Krot, Saha, Kumar, Pawan, Kuvvetli, Irfan, Laird, Alison, Laming, Martin, Larsson, Josefin, Lattanzio, John, Lattimer, James, Leising, Mark, Lennarz, Annika, Lentz, Eric, Limongi, Marco, Lippuner, Jonas, Livne, Eli, Lloyd-Ronning, Nicole, Longland, Richard, Lopez, Laura A., Lugaro, Maria, Lutovinov, Alexander, Madsen, Kristin, Malone, Chris, Matteucci, Francesca, McEnery, Julie, Meisel, Zach, Messer, Bronson, Metzger, Brian, Meyer, Bradley, Meynet, Georges, Mezzacappa, Anthony, Miller, Jonah, Miller, Richard, Milne, Peter, Misch, Wendell, Mitchell, Lee, Mosta, Philipp, Motizuki, Yuko, Muller, Bernhard, Mumpower, Matthew, Murphy, Jeremiah, Nagataki, Shigehiro, Nakar, Ehud, Nomoto, Ken'ichi, Nugent, Peter, Nunes, Filomena, O'Shea, Brian, Oberlack, Uwe, Pain, Steven, Parker, Lucas, Perego, Albino, Pignatari, Marco, Pinedo, Gabriel Martinez, Plewa, Tomasz, Poznanski, Dovi, Priedhorsky, William, Pritychenko, Boris, Radice, David, Ramirez-Ruiz, Enrico, Rauscher, Thomas, Reddy, Sanjay, Rehm, Ernst, Reifarth, Rene, Richman, Debra, Ricker, Paul, Rijal, Nabin, Roberts, Luke, Ropke, Friedrich, Rosswog, Stephan, Ruiter, Ashley J., Ruiz, Chris, Savin, Daniel Wolf, Schatz, Hendrik, Schneider, Dieter, Schwab, Josiah, Seitenzahl, Ivo, Shen, Ken, Siegert, Thomas, Sim, Stuart, Smith, David, Smith, Karl, Smith, Michael, Sollerman, Jesper, Sprouse, Trevor, Spyrou, Artemis, Starrfield, Sumner, Steiner, Andrew, Strong, Andrew W., Sukhbold, Tuguldur, Suntzeff, Nick, Surman, Rebecca, Tanimori, Toru, The, Lih-Sin, Thielemann, Friedrich-Karl, Tolstov, Alexey, Tominaga, Nozomu, Tomsick, John, Townsley, Dean, Tsintari, Pelagia, Tsygankov, Sergey, Vartanyan, David, Venters, Tonia, Vestrand, Tom, Vink, Jacco, Waldman, Roni, Wang, Lifang, Wang, Xilu, Warren, MacKenzie, West, Christopher, Wheeler, J. Craig, Wiescher, Michael, Winkler, Christoph, Winter, Lisa, Wolf, Bill, Woolf, Richard, Woosley, Stan, Wu, Jin, Wrede, Chris, Yamada, Shoichi, Young, Patrick, Zegers, Remco, Zingale, Michael, and Zwart, Simon Portegies

Abstract

Gamma-ray astronomy explores the most energetic photons in nature to address some of the most pressing puzzles in contemporary astrophysics. The unique information provided by MeV gamma-ray astronomy to help address frontiers makes now a compelling time for the community to advocate for a new mission to be operational in the 2020s and beyond.

Published
2019
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16. The impact of (n,γ) reaction rate uncertainties of unstable isotopes on the i-process nucleosynthesis of the elements from Ba to W.

Author

Denissenkov, Pavel A, Herwig, Falk, Perdikakis, Georgios, and Schatz, Hendrik

Subjects
MONTE Carlo method, NUCLEOSYNTHESIS, PEARSON correlation (Statistics), ISOTOPES, UNCERTAINTY, CESIUM isotopes
Abstract

The abundances of neutron (n)-capture elements in the carbon-enhanced metal-poor (CEMP)-r/s stars agree with predictions of intermediate n-density nucleosynthesis, at N n ∼ 1013–1015 cm−3, in rapidly accreting white dwarfs (RAWDs). We have performed Monte Carlo simulations of this intermediate-process (i -process) nucleosynthesis to determine the impact of (n,γ) reaction rate uncertainties of 164 unstable isotopes, from 131I to 189Hf, on the predicted abundances of 18 elements from Ba to W. The impact study is based on two representative one-zone models with constant values of N n = 3.16 × 1014 and 3.16 × 1013 cm−3 and on a multizone model based on a realistic stellar evolution simulation of He-shell convection entraining H in a RAWD model with [Fe/H] = −2.6. For each of the selected elements, we have identified up to two (n,γ) reactions having the strongest correlations between their rate variations constrained by Hauser–Feshbach computations and the predicted abundances, with the Pearson product–moment correlation coefficients | r P| > 0.15. We find that the discrepancies between the predicted and observed abundances of Ba and Pr in the CEMP-i star CS 31062−050 are significantly diminished if the rate of 137Cs(n,γ)138Cs is reduced and the rates of 141Ba(n,γ)142Ba or 141La(n,γ)142La increased. The uncertainties of temperature-dependent β-decay rates of the same unstable isotopes have a negligible effect on the predicted abundances. One-zone Monte Carlo simulations can be used instead of computationally time-consuming multizone Monte Carlo simulations in reaction rate uncertainty studies if they use comparable values of N n. We discuss the key challenges that RAWD simulations of i process for CEMP-i stars meet by contrasting them with recently published low- Z asymptotic giant branch (AGB) i process. [ABSTRACT FROM AUTHOR]

Published
2021
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18. Magnets and Wien Filters for SECAR

Author

BøDker, Franz, Berg, Georg, Couder, Manoel, Hauge, Nils, Kristensen, Jesper, and Schatz, Hendrik

Subjects
04 Hadron Accelerators, Accelerator Physics
Abstract

The Separator for Capture Reactions, SECAR, is being built at Michigan State University for the study of low-energy capture reactions. The high performance magnets and two large Wien filters required to reach the very high recoil mass separation factor are being designed and produced at Danfysik to the SECAR specifications. The 2.4 m long Wien filters with a weight of 35 ton each including a large vacuum tank have high electrode voltages of ±300 kV combined with a magnetic field of 0.12 T. Challenging design requirements for integrated magnetic and electrostatic field homogeneity combined with tight tolerance on the effective lengths have been meet. The dipole magnets for this facility are special in having stringent ±0.5 mm effective magnetic length specifications in a wide excitation range and the transverse field boundary variation is described by a 4th order polynomial. Most of the dipoles are made with variable segmented field clamps in order to keep the deviation of the magnetic fringe field boundary within the required ±0.1 mm. The wide range of different quadrupole, sextupole and octupole magnets are required to meet the specified magnetic length with a tight tolerance., Proceedings of the 8th Int. Particle Accelerator Conf., IPAC2017, Copenhagen, Denmark

Published
2017
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19. Reaction Rate Sensitivity of the Production of γ-Ray Emitting Isotopes in Core-collapse Supernovae.

Author

Hermansen, Kirby, Couch, Sean M., Roberts, Luke F., Schatz, Hendrik, and Warren, MacKenzie L.

Subjects
NUCLEOSYNTHESIS, RADIOISOTOPES, NUCLEAR reactions, ISOTOPES, SUPERNOVAE, SILICON isotopes, CHROMIUM isotopes
Abstract

Radioactive isotopes produced in core-collapse supernovae (CCSNe) provide useful insights into the underlying processes driving the collapse mechanism and the origins of elemental abundances. Their study generates a confluence of major physics research, including experimental measurements of nuclear reaction rates, astrophysical modeling, and γ-ray observations. Here we identify the key nuclear reaction rates to the nucleosynthesis of observable radioactive isotopes in explosive silicon burning during CCSNe. Using the nuclear reaction network calculator SkyNet and current REACLIB reaction rates, we evolve temperature–density–time profiles of the innermost 0.45 M⊙ ejecta from the core collapse and explosion of a 12 M⊙ star. Individually varying 3403 reaction rates by factors of 100, we identify 141 reactions that cause significant differences in the isotopes of interest, namely, 43K, 47Ca, 44,47Sc, 44Ti, 48,51Cr, 48,49V, 52,53Mn, 55,59Fe, 56,57Co, and 56,57,59Ni. For each of these reactions, we present a novel method to extract the temperature range pertinent to the nucleosynthesis of the relevant isotope; the resulting temperatures lie within the range T = 0.47–6.15 GK. Limiting the variations to within 1σ of STARLIB reaction rate uncertainties further reduces the identified reactions to 48 key rates, which can be used to guide future experimental research. Complete results are presented in tabular form. [ABSTRACT FROM AUTHOR]

Published
2020
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20. The impact of (n,γ) reaction rate uncertainties on the predicted abundances of i-process elements with 32 ≤ Z ≤ 48 in the metal-poor star HD94028.

Author

McKay, John E, Denissenkov, Pavel A, Herwig, Falk, Perdikakis, Georgios, and Schatz, Hendrik

Subjects
MONTE Carlo method, INTEGRAL field spectroscopy, PEARSON correlation (Statistics), NUCLEAR physics, NUCLEOSYNTHESIS, NUCLEAR reactions
Abstract

Several anomalous elemental abundance ratios have been observed in the metal-poor star HD94028. We assume that its high [As/Ge] ratio is a product of a weak intermediate (i) neutron-capture process. Given that observational errors are usually smaller than predicted nuclear physics uncertainties, we have first set-up a benchmark one-zone i-process nucleosynthesis simulation results of which provide the best fit to the observed abundances. We have then performed Monte Carlo simulations in which 113 relevant (n,γ) reaction rates of unstable species were randomly varied within Hauser–Feshbach model uncertainty ranges for each reaction to estimate the impact on the predicted stellar abundances. One of the interesting results of these simulations is a double-peaked distribution of the As abundance, which is caused by the variation of the 75Ga (n,γ) cross-section. This variation strongly anticorrelates with the predicted As abundance, confirming the necessity for improved theoretical or experimental bounds on this cross-section. The 66Ni (n,γ) reaction is found to behave as a major bottleneck for the i-process nucleosynthesis. Our analysis finds the Pearson product–moment correlation coefficient r P > 0.2 for all of the i-process elements with 32 ≤ Z ≤ 42, with significant changes in their predicted abundances showing up when the rate of this reaction is reduced to its theoretically constrained lower bound. Our results are applicable to any other stellar nucleosynthesis site with the similar i-process conditions, such as Sakurai's object (V4334 Sagittarii) or rapidly accreting white dwarfs. [ABSTRACT FROM AUTHOR]

Published
2020
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21. Rare isotopes in the cosmos

Author

Schatz, Hendrik

Subjects
Astrophysics -- Research, Heavy elements (Cosmochemistry) -- Atomic properties, Isotopes -- Observations, Universe -- Composition, Physics
Published
2008

22. Constraining the rp-process by measuring 23Al(d,n)24Si with GRETINA and LENDA at NSCL.

Author

Wolf, Clemens, Langer, Christoph, Fiebiger, Stefan, Reifarth, René, Bazin, Daniel, Bender, Peter, Brown, Alex, Sullivan, Chris, Weisshaar, Dirk, Carlos Zamora, Juan, Montes, Fernando, Pereira, Jorge, Sunghoon Ahn, Schmidt, Konrad, Schmitt, Jaclyn, Titus, Rachel, Schatz, Hendrik, Ayoub, Sara, Browne, Justin, and Deleeuw, Eric

Subjects
ALUMINUM isotopes, NUCLEAR reactions, PROTON capture, SILICON isotopes, X-ray bursts, NUCLEAR physics experiments, KINEMATICS
Abstract

The 23Al(p, γ)24Si stellar reaction rate has a significant impact on the light-curve emitted in X-ray bursts. Theoretical calculations show that the reaction rate is mainly determined by the properties of direct capture as well as low-lying 2+ states and a possible 4+ state in 24Si. Currently, there is little experimental information on the properties of these states. In this proceeding we will present a new experimental study to investigate this reaction, using the surrogate reaction 23Al(d,n) at 47 AMeV at the National Superconducting Cyclotron Laboratory (NSCL). We will discuss our new experimental setup which allows us to use full kinematics employing the Gamma-Ray Energy Tracking In-beam Nuclear Array (GRETINA) to detect the γ-rays following the de-excitation of excited states of the reaction products and the Low Energy Neutron Detector Array (LENDA) to detect the recoiling neutrons. The S800 was used for identification of the 24Si recoils. As a proof of principle to show the feasibility of this concept the Q-value spectrum of 22Mg(d,n)23Al is reconstructed. [ABSTRACT FROM AUTHOR]

Published
2017
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23. X-ray burst studies with the JENSA gas jet target.

Author

Linhardt, Laura E., Schmidt, Konrad, Sunghoon Ahn, Montes, Fernando, Ayoub, Sara, Browne, Justin, Deleeuw, Eric, Wei Jia Ong, Schatz, Hendrik, Hager, Ulrike, Greife, Uwe, Jones, Katherine L., Sachs, Alison, Schmitt, Kyle T., Smith, Karl, Thompson, Paul J., Kontos, Antonios, Kozub, Raymond L., Soares de Bem, Natã F., and Matos, Milan

Subjects
X-ray bursts, TARGETS (Nuclear physics), NUCLEAR reactions, NEUTRON stars, HELIUM isotopes, HYDROGEN isotopes, THERMONUCLEAR reactions in stars
Abstract

When a neutron star accretes hydrogen and helium from the outer layers of its companion star, thermonuclear burning enables the αp-process as a break out mechanism from the hot CNO cycle. Model calculations predict (α, p) reaction rates significantly affect both the light curves and elemental abundances in the burst ashes. The Jet Experiments in Nuclear Structure and Astrophysics (JENSA) gas jet target enables the direct measurement of previously inaccessible (α,p) reactions with radioactive beams provided by the rare isotope re-accelerator ReA3 at the National Superconducting Cyclotron Laboratory (NSCL), USA. JENSA is going to be the main target for the Recoil Separator for Capture Reactions (SECAR) at the Facility for Rare Isotope Beams (FRIB). Commissioning of JENSA and first experiments at Oak Ridge National Laboratory (ORNL) showed a highly localized, pure gas target with a density of ∼1019 atoms per square centimeter. Preliminary results are presented from the first direct cross section measurement of the 34Ar(α, p)37 K reaction at NSCL. [ABSTRACT FROM AUTHOR]

Published
2017
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24. TOF-Bρ Mass Measurement of Neutron Rich Nuclei at the NSCL.

Author

Estradé, Alfredo, Matoš, Milan, Amthor, Matthew A., Bazin, Daniel, Becerril, Ana D., Elliot, Thom J., Gade, Alexandra, Galaviz, Daniel, Lorusso, Giuseppe, Pereira, Jorge, Portillo, Mauricio, Rogers, Andrew, Schatz, Hendrik, Shapira, Dan, Smith, Edward, Stolz, Andreas, and Wallace, Mark S.

Subjects
NUCLEAR physics, PARTICLES (Nuclear physics), NEUTRON stars, STARS, CHEMICAL elements, COSMOCHEMISTRY
Abstract

Experimental knowledge of nuclear masses of exotic nuclei is important for understanding nuclear structure far from the valley of β-stability, and as a direct input into astrophysical models. In the case of astrophysical processes involving neutron rich nuclei, such as nucleosynthesis during the r-process and the evolution of matter in the crust of an accreting neutron star, we are mostly limited to using theoretical mass models. The time of flight (TOF) mass measurement technique allows measuring very short-lived nuclei. It has been effectively applied using the fast fragment beams produced at the A1900 fragment separator at the National Superconducting Cyclotron Lab (NSCL) to reach masses very far from stability. We describe a recent mass measurement experiment in the neutron rich Fe region performed at the NSCL, and present preliminary results. [ABSTRACT FROM AUTHOR]

Published
2007
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26. Design of a New Recoil Separator for Measurements of Radiative Capture Reactions in Astrophysics.

Author

Berg, Georg P. A., Blackmon, Jeff C., Couder, Manoel, Greife, U., Montes, F., Rehm, K. Ernst, Schatz, Hendrik, Smith, Michael S., Wiescher, Michael, and Zeller, Al

Subjects
ASTROPHYSICS, PROTONS, NUCLEAR reactions, X-rays, COLLISIONS (Nuclear physics)
Abstract

The rates of proton- and alpha-capture reactions on unstable proton-rich nuclei are needed to understand the energy generation and element synthesis occurring in novae, X-ray bursts, and other explosions. Direct measurements of the cross sections of some of these reactions are now possible with radioactive beams and a recoil separator. A new device for such measurements, the Separator for CApture Reactions [SECAR], is being designed for use at the Facility for Rare Isotope Beams (FRIB). The specifications and preliminary conceptual design will be discussed along with plans for the first set of measurements. [ABSTRACT FROM AUTHOR]

Published
2010
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27. Thermonuclear Reaction Rate Libraries and Software Tools for Nuclear Astrophysics Research.

Author

Smith, Michael S., Cyburt, Richard, Schatz, Hendrik, Wiescher, Michael, Smith, Karl, Warren, Scott, Ferguson, Ryan, Lingerfelt, Eric, Buckner, Kim, and Nesaraja, Caroline D.

Subjects
NUCLEAR astrophysics, CHEMICAL kinetics, ASTROPHYSICS, NUCLEAR reactions, NUCLEAR physics
Abstract

Thermonuclear reaction rates are a crucial input for simulating a wide variety of astrophysical environments. A new collaboration has been formed to ensure that astrophysical modelers have access to reaction rates based on the most recent experimental and theoretical nuclear physics information. To reach this goal, a new version of the REACLIB library has been created by the Joint Institute for Nuclear Astrophysics (JINA), now available online at http://www.nscl.msu.edu/∼nero/db. A complementary effort is the development of software tools in the Computational Infrastructure for Nuclear Astrophysics, online at nucastrodata.org, to streamline, manage, and access the workflow of the reaction evaluations from their initiation to peer review to incorporation into the library. Details of these new projects will be described. [ABSTRACT FROM AUTHOR]

Published
2008
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28. Astrophysics at RIA (ARIA) Working Group.

Author

Smith, Michael S., Schatz, Hendrik, Timmes, Frank X., Wiescher, Michael, and Greife, Uwe

Subjects
*SUPERNOVAE, *ASTROPHYSICS, *ASTRONOMY, *RESEARCH teams
Abstract

The Astrophysics at RIA (ARIA) Working Group has been established to develop and promote the nuclear astrophysics research anticipated at the Rare Isotope Accelerator (RIA). RIA is a proposed next-generation nuclear science facility in the U.S. that will enable significant progress in studies of core collapse supernovae, thermonuclear supernovae, X-ray bursts, novae, and other astrophysical sites. Many of the topics addressed by the Working Group are relevant for the RIKEN RI Beam Factory, the planned GSI-Fair facility, and other advanced radioactive beam facilities. © 2006 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2006
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29. PREFACE.

Author

Yong-Zhong Qian, Rehm, Ernst, Schatz, Hendrik, and Thielemann, Friedrich-Karl

Subjects
RADIOACTIVE nuclear beams, NUCLEAR astrophysics, NEUTRON capture, URANIUM
Published
2004

30. CARBON SYNTHESIS IN STEADY-STATE HYDROGEN AND HELIUM BURNING ON ACCRETING NEUTRON STARS.

Author

Stevens, Jeremy, Brown, Edward F., Cumming, Andrew, Cyburt, Richard, and Schatz, Hendrik

Subjects
ACCRETION (Astrophysics), NUCLEAR reactions, NUCLEOSYNTHESIS, STARS, NEUTRON stars, X-ray bursts
Abstract

Superbursts from accreting neutron stars probe nuclear reactions at extreme densities (ρ ≈ 109 g cm–3) and temperatures (T > 109 K). These bursts (∼1000 times more energetic than type I X-ray bursts) are most likely triggered by unstable ignition of carbon in a sea of heavy nuclei made during the rapid proton capture process (rp-process) of regular type I X-ray bursts (where the accumulated hydrogen and helium are burned). An open question is the origin of sufficient amounts of carbon, which is largely destroyed during the rp-process in X-ray bursts. We explore carbon production in steady-state burning via the rp-process, which might occur together with unstable burning in systems showing superbursts. We find that for a wide range of accretion rates and accreted helium mass fractions large amounts of carbon are produced, even for systems that accrete solar composition. This makes stable hydrogen and helium burning a viable source of carbon to trigger superbursts. We also investigate the sensitivity of the results to nuclear reactions. We find that the 14O(α, p)17F reaction rate introduces by far the largest uncertainties in the 12C yield. [ABSTRACT FROM AUTHOR]

Published
2014
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31. NEW DETECTIONS OF ARSENIC, SELENIUM, AND OTHER HEAVY ELEMENTS IN TWO METAL-POOR STARS.

Author

Roederer, Ian U., Schatz, Hendrik, Lawler, James E., Beers, Timothy C., Cowan, John J., Frebel, Anna, Ivans, Inese I., Sneden, Christopher, and Sobeck, Jennifer S.

Subjects
*SPECTROGRAPHS, *WAVELENGTHS, *DENSITY of stars, *THERMODYNAMICS
Abstract

We use the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope to obtain new high-quality spectra covering the 1900 ⩽λ ⩽ 2360 Å wavelength range for two metal-poor stars, HD 108317 and HD 128279. We derive abundances of Cu II, Zn II, As I, Se I, Mo II, and Cd II, which have not been detected previously in either star. Abundances derived for Ge I, Te I, Os II, and Pt I confirm those derived from lines at longer wavelengths. We also derive upper limits from the non-detection of W II, Hg II, Pb II, and Bi I. The mean [As/Fe] ratio derived from these two stars and five others in the literature is unchanged over the metallicity range –2.8 < [Fe/H] <–0.6, 〈 [As/Fe]〉 = +0.28 ± 0.14 (σ = 0.36 dex). The mean [Se/Fe] ratio derived from these two stars and six others in the literature is also constant, 〈 [Se/Fe]〉 = +0.16 ± 0.09 (σ = 0.26 dex). The As and Se abundances are enhanced relative to a simple extrapolation of the iron-peak abundances to higher masses, suggesting that this mass region (75 ⩽A ⩽ 82) may be the point at which a different nucleosynthetic mechanism begins to dominate the quasi-equilibrium α-rich freezeout of the iron peak. 〈 [Cu II/Cu I]〉 = +0.56 ± 0.23 in HD 108317 and HD 128279, and we infer that lines of Cu I may not be formed in local thermodynamic equilibrium in these stars. The [Zn/Fe], [Mo/Fe], [Cd/Fe], and [Os/Fe] ratios are also derived from neutral and ionized species, and each ratio pair agrees within the mutual uncertainties, which range from 0.15 to 0.52 dex. [ABSTRACT FROM AUTHOR]

Published
2014
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32. HUBBLE SPACE TELESCOPE NEAR-ULTRAVIOLET SPECTROSCOPY OF THE BRIGHT CEMP-NO STAR BD+44°493.

Author

Placco, Vinicius M., Beers, Timothy C., Roederer, Ian U., Cowan, John J., Frebel, Anna, Filler, Dan, Ivans, Inese I., Lawler, James E., Schatz, Hendrik, Sneden, Christopher, Sobeck, Jennifer S., Aoki, Wako, and Smith, Verne V.

Subjects
ULTRAVIOLET radiation, NEUTRONS, HEAVY elements, BERYLLIUM
Abstract

We present an elemental-abundance analysis, in the near-ultraviolet (NUV) spectral range, for the extremely metal-poor star BD+44°493 a ninth magnitude subgiant with [Fe/H] =–3.8 and enhanced carbon, based on data acquired with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. This star is the brightest example of a class of objects that, unlike the great majority of carbon-enhanced metal-poor (CEMP) stars, does not exhibit over-abundances of heavy neutron-capture elements (CEMP-no). In this paper, we validate the abundance determinations for a number of species that were previously studied in the optical region, and obtain strong upper limits for beryllium and boron, as well as for neutron-capture elements from zirconium to platinum, many of which are not accessible from ground-based spectra. The boron upper limit we obtain for BD+44°493, log ε (B) <–0.70, the first such measurement for a CEMP star, is the lowest yet found for very and extremely metal-poor stars. In addition, we obtain even lower upper limits on the abundances of beryllium, log ε (Be) <–2.3, and lead, log ε (Pb) <–0.23 ([Pb/Fe] <+1.90), than those reported by previous analyses in the optical range. Taken together with the previously measured low abundance of lithium, the very low upper limits on Be and B suggest that BD+44°493 was formed at a very early time, and that it could well be a bona-fide second-generation star. Finally, the Pb upper limit strengthens the argument for non-s-process production of the heavy-element abundance patterns in CEMP-no stars. [ABSTRACT FROM AUTHOR]

Published
2014
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39. The Virtual Journals of the Joint Institute for Nuclear Astrophysics.

Author

Cyburt, Richard H., Austin, Sam M., Beers, Timothy C., Estrade, Alfredo, Ferguson, Ryan M., Sakharuk, Alexander, Schatz, Hendrik, Smith, Karl, and Warren, Scott

Subjects
NUCLEAR astrophysics, NUCLEAR physics, TRITONS (Nuclear physics), DATABASE security, COMPUTER security
Abstract

The research area of nuclear astrophysics is characterized by a need for information published in tens of journals in several fields and an extremely dilute distribution of researchers. For these reasons it is difficult for researchers, especially students, to be adequately informed of the relevant published research. In an attempt to address this problem, we have developed a virtual journal (VJ), a process for collecting and distributing a weekly compendium of articles of interest to researchers in nuclear astrophysics. Subscribers are notified of each VJ issue using an email-list server or an RSS feed. The VJ data base is searchable by topics assigned by the editors, or by keywords. There are two related VJs: the Virtual Journal of Nuclear Astrophysics (JINA VJ), and the SEGUE Virtual Journal (SEGUE VJ). [ABSTRACT FROM AUTHOR]

Published
2010
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40. Dense matter with eXTP

Author

Xiang-Dong Li, Jean in 't Zand, B. W. Stappers, Sudip Bhattacharyya, Slavko Bogdanov, Holger Stiele, Sharon M. Morsink, Tiziana Di Salvo, Zhaosheng Li, Robert D. Ferdman, Alessandro Riggio, Jin-Lu Qu, Wenfei Yu, Oleg Kargaltsev, R. Iaria, Xia Zhou, Joonas Nättilä, Gabriel Török, David Tsang, Aleksi Kurkela, Laura Tolos, Achim Schwenk, Ingo Tews, Ypeng Xu, Andrea Vacchi, Martin Urbanec, Andrea Santangelo, Xiao Yu Lai, Manuel Linares, Pavel Bakala, Altan Baykal, Anna L. Watts, Alexander Heger, Eva Šrámková, Andrea Sanna, Maurizio Falanga, Ang Li, M. Coleman Miller, Federico Bernardini, Edward F. Brown, Yuri Cavecchi, Jérôme Chenevez, Long Ji, Dieter H. Hartmann, Hendrik Schatz, Ignazio Bombaci, Shuang-Nan Zhang, Silvia Zane, Chanda Prescod-Weinstein, Victor Doroshenko, Kai Hebeler, Guobao Zhang, Tuomo Salmi, Fangjun Lu, Ming-Yu Ge, Melania Del Santo, Deepto Chakrabarty, Mariano Mendez, ShiJie Zheng, Wenda Zhang, S. K. Greif, Alessandro Patruno, Angelo Gambino, Nathalie Degenaar, Simin Mahmoodifar, Juri Poutanen, Marco Feroci, Thomas E. Riley, Shu Zhang, Andrea Possenti, Sebastien Guillot, Tod E. Strohmayer, Jeroen Homan, Can Güngör, Li-Ming Song, Renxin Xu, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, High Energy Astrophys. & Astropart. Phys (API, FNWI), Astronomy, Watts, Anna L., Yu, WenFei, Poutanen, Juri, Zhang, Shu, Bhattacharyya, Sudip, Bogdanov, Slavko, Ji, Long, Patruno, Alessandro, Riley, Thomas E., Bakala, Pavel, Baykal, Altan, Bernardini, Federico, Bombaci, Ignazio, Brown, Edward, Cavecchi, Yuri, Chakrabarty, Deepto, Chenevez, Jérôme, Degenaar, Nathalie, Del Santo, Melania, Di Salvo, Tiziana, Doroshenko, Victor, Falanga, Maurizio, Ferdman, Robert D., Feroci, Marco, Gambino, Angelo F., Ge, MingYu, Greif, Svenja K., Guillot, Sebastien, Gungor, Can, Hartmann, Dieter H., Hebeler, Kai, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Zand, Jean in’t, Kargaltsev, Oleg, Kurkela, Aleksi, Lai, XiaoYu, Li, Ang, Li, XiangDong, Li, ZhaoSheng, Linares, Manuel, Lu, FangJun, Mahmoodifar, Simin, Méndez, Mariano, Coleman Miller, M., Morsink, Sharon, Nättilä, Joona, Possenti, Andrea, Prescod-Weinstein, Chanda, Qu, JinLu, Riggio, Alessandro, Salmi, Tuomo, Sanna, Andrea, Santangelo, Andrea, Schatz, Hendrik, Schwenk, Achim, Song, LiMing, Šrámková, Eva, Stappers, Benjamin, Stiele, Holger, Strohmayer, Tod, Tews, Ingo, Tolos, Laura, Török, Gabriel, Tsang, David, Urbanec, Martin, Vacchi, Andrea, Xu, RenXin, Xu, YuPeng, Zane, Silvia, Zhang, GuoBao, Zhang, ShuangNan, Zhang, WenDa, Zheng, ShiJie, and Zhou, Xia

Subjects
GAMMA-RAY PULSARS, dense matter, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Neutron, BRIGHTNESS OSCILLATIONS, 7. Clean energy, 01 natural sciences, INNER ACCRETION DISKS, Spectral line, X-ray, equation of state, neutron, X-rays, Physics and Astronomy (all), Equacions d'estat, Pulsar, 0103 physical sciences, MILLISECOND PULSARS, NEUTRON-STAR, RADIUS CONSTRAINTS, 010306 general physics, 010303 astronomy & astrophysics, RELATIVISTIC IRON LINE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), LIGHT CURVES, Neutrons, Equation of state, QUASI-PERIODIC OSCILLATIONS, X-Rays, Starke Wechselwirkung und exotische Kerne – Abteilung Blaum, Astrophysics::Instrumentation and Methods for Astrophysics, EQUATION-OF-STATE, Accretion (astrophysics), Neutron star, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Raigs X, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Dense matter
Abstract

In this White Paper we present the potential of the Enhanced X-ray Timing and Polarimetry (eXTP) mission for determining the nature of dense matter; neutron star cores host an extreme density regime which cannot be replicated in a terrestrial laboratory. The tightest statistical constraints on the dense matter equation of state will come from pulse profile modelling of accretion-powered pulsars, burst oscillation sources, and rotation-powered pulsars. Additional constraints will derive from spin measurements, burst spectra, and properties of the accretion flows in the vicinity of the neutron star. Under development by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)

Published
2019

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