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1,215 results on '"Lefèvre, F"'

1. Probing Earth's Missing Potassium using the Unique Antimatter Signature of Geoneutrinos

Author

Consortium, LiquidO, Cabrera, A., Chen, M., Mantovani, F., Serafini, A., Strati, V., Apilluelo, J., Asquith, L., Beney, J. L., Bezerra, T. J. C., Bongrand, M., Bourgeois, C., Breton, D., Briere, M., Busto, J., Cadiou, A., Calvo, E., Chaumat, V., Chauveau, E., Cattermole, B. J., Chimenti, P., Delafosse, C., de Kerret, H., Dusini, S., Earle, A., Frigerio-Martins, C., Galán, J., García, J. A., Gazzini, R., Gibson-Foster, A., Gallas, A., Girard-Carillo, C., Griffith, W. C., Haddad, F., Hartnell, J., Hourlier, A., Hull, G., Irastorza, I. G., Koch, L., Laniéce, P., Du, J. F. Le, Lefebvre, C., Lefevre, F., Legrand, F., Loaiza, P., Lock, J. A., Luzón, G., Maalmi, J., Marquet, C., Martínez, M., Mathon, B., Ménard, L., Navas-Nicolás, D., Nunokawa, H., Ochoa-Ricoux, J. P., Obolensky, M., Palomares, C., Pillot, P., Porter, J. C. C., Pravikoff, M. S., Ramarijaona, H., Roche, M., Rosier, P., Roskovec, B., Sarsa, M. L., Schoppmann, S., Shorrock, W., Simard, L., Steiger, H. Th. J., Stocco, D., Stutzmann, J. S., Suekane, F., Tunc, A., Verdier, M. -A., Verdugo, A., Viaud, B., Wakely, S. M., Weber, A., and Yermia, F.

Subjects
Physics - Geophysics, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

The formation of the Earth remains an epoch with mysterious puzzles extending to our still incomplete understanding of the planet's potential origin and bulk composition. Direct confirmation of the Earth's internal heat engine was accomplished by the successful observation of geoneutrinos originating from uranium (U) and thorium (Th) progenies, manifestations of the planet's natural radioactivity dominated by potassium (40K) and the decay chains of uranium (238U) and thorium (232Th). This radiogenic energy output is critical to planetary dynamics and must be accurately measured for a complete understanding of the overall heat budget and thermal history of the Earth. Detecting geoneutrinos remains the only direct probe to do so and constitutes a challenging objective in modern neutrino physics. In particular, the intriguing potassium geoneutrinos have never been observed and thus far have been considered impractical to measure. We propose here a novel approach for potassium geoneutrino detection using the unique antimatter signature of antineutrinos to reduce the otherwise overwhelming backgrounds to observing this rarest signal. The proposed detection framework relies on the innovative LiquidO detection technique to enable positron (e+) identification and antineutrino interactions with ideal isotope targets identified here for the first time. We also provide the complete experimental methodology to yield the first potassium geoneutrino discovery.

Published
2023

2. Characterization of a radiation detector based on opaque water-based liquid scintillator

Author

Apilluelo, J., Asquith, L., Bannister, E.F., Beney, J.L., de La Bernardie, X., Bezerra, T.J.C., Bongrand, M., Bourgeois, C., Boutalha, H., Breton, D., Briere, M., Cabrera, A., Cadiou, A., Calvo, E., Chaumat, V., Chauveau, E., Cattermole, B.J., Chen, M., Chimenti, P., Ċornet, T., Cowen, D.F., Delafosse, C., Dusini, S., Earle, A., Frigerio-Martins, C., Galán, J., Gallas, A., García, J.A., Gazzini, R., Gibson-Foster, A., Girard-Carillo, C., Griffith, W.C., Gómez-Cadenas, J.J., Guittière, M., Haddad, F., Hartnell, J., Holin, A., Hull, G., Irastorza, I.G., Jovanovic, I., Koch, L., Du, J.F. Le, Lefebvre, C., Lefevre, F., Legrand, F., Loaiza, P., Lock, J.A., Luzón, G., Maalmi, J., Malhado, J.P., Mantovani, F., Marquet, C., Martínez, M., Mathon, B., Navas-Nicolás, D., Nunokawa, H., Ochoa-Ricoux, J.P., Palomares, C., Petyt, D., Pillot, P., Porter, J.C.C., Pravikoff, M.S., Ramarijaona, H., Roche, M., Rosero, R., Rosier, P., Roskovec, B., Sarsa, M.L., Schoppmann, S., Serafini, A., Shepherd-Themistocleous, C., Shorrock, W., Simard, L., Soleti, S.R., Steiger, H.Th.J., Stocco, D., Strati, V., Stutzmann, J.S., Suekane, F., Tunc, A., Tuccori, N., Verdugo, A., Viaud, B., Wakely, S.M., Weber, A., Wendel, G., Wilhelm, A.S., Yeh, M., and Yermia, F.

Published
2025
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3. No detection of SO2, H2S, or OCS in the atmosphere of Mars from the first two Martian years of observations from TGO/ACS

Author

Braude, Ashwin S., Montmessin, F., Olsen, K. S., Trokhimovskiy, A., Korablev, O. I., Lefèvre, F., Fedorova, A. A., Alday, J., Baggio, L., Irbah, A., Lacombe, G., Forget, F., Millour, E., Wilson, C. F., Patrakeev, A., and Shakun, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The detection of sulphur species in the Martian atmosphere would be a strong indicator of volcanic outgassing from the surface of Mars. We wish to establish the presence of SO2, H2S, or OCS in the Martian atmosphere or determine upper limits on their concentration in the absence of a detection. We perform a comprehensive analysis of solar occultation data from the mid-infrared channel of the Atmospheric Chemistry Suite instrument, on board the ExoMars Trace Gas Orbiter, obtained during Martian years 34 and 35. For the most optimal sensitivity conditions, we determine 1-sigma upper limits of SO2 at 20 ppbv, H2S at 15 ppbv, and OCS at 0.4 ppbv; the last value is lower than any previous upper limits imposed on OCS in the literature. We find no evidence of any of these species above a 3-sigma confidence threshold. We therefore infer that passive volcanic outgassing of SO2 must be below 2 ktons/day., Comment: 13 pages, 12 figures, received for production in A&A on the 19th of November 2021

Published
2021
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6. Metallization of Shock-Compressed Liquid Ammonia

Author

Ravasio, A., Bethkenhagen, M., Hernandez, J. -A., Benuzzi-Mounaix, A., Datchi, F., French, M., Guarguaglini, M., Lefevre, F., Ninet, S., Redmer, R., and Vinci, T.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Chemical Physics, Physics - Plasma Physics
Abstract

Ammonia is predicted to be one of the major components in the depths of the ice giant planets Uranus and Neptune. Their dynamics, evolution, and interior structure are insufficiently understood and models rely imperatively on data for equation of state and transport properties. Despite its great significance, the experimentally accessed region of the ammonia phase diagram today is still very limited in pressure and temperature. Here we push the probed regime to unprecedented conditions, up to $\sim$350 GPa and $\sim$40000 K. Along the Hugoniot, the temperature measured as a function of pressure shows a subtle change in slope at $\sim$7000 K and $\sim$90 GPa, in agreement with ab initio simulations we have performed. This feature coincides with the gradual transition from a molecular liquid to a plasma state. Additionally, we performed reflectivity measurements, providing the first experimental evidence of electronic conduction in high-pressure ammonia. Shock reflectance continuously rises with pressure above 50 GPa and reaches saturation values above 120 GPa. Corresponding electrical conductivity values are up to 1 order of magnitude higher than in water in the 100 GPa regime, with possible significant contributions of the predicted ammonia-rich layers to the generation of magnetic dynamos in ice giant interiors., Comment: Please visit publisher's website for supplementary information

Published
2021
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7. Optimization of the JUNO liquid scintillator composition using a Daya Bay antineutrino detector

Author

Bay, Daya, collaborations, JUNO, Abusleme, A., Adam, T., Ahmad, S., Aiello, S., Akram, M., Ali, N., An, F. P., An, G. P., An, Q., Andronico, G., Anfimov, N., Antonelli, V., Antoshkina, T., Asavapibhop, B., de André, J. P. A. M., Babic, A., Balantekin, A. B., Baldini, W., Baldoncini, M., Band, H. R., Barresi, A., Baussan, E., Bellato, M., Bernieri, E., Biare, D., Birkenfeld, T., Bishai, M., Blin, S., Blum, D., Blyth, S., Bordereau, C., Brigatti, A., Brugnera, R., Budano, A., Burgbacher, P., Buscemi, M., Bussino, S., Busto, J., Butorov, I., Cabrera, A., Cai, H., Cai, X., Cai, Y. K., Cai, Z. Y., Cammi, A., Campeny, A., Cao, C. Y., Cao, G. F., Cao, J., Caruso, R., Cerna, C., Chakaberia, I., Chang, J. F., Chang, Y., Chen, H. S., Chen, P. A., Chen, P. P., Chen, S. M., Chen, S. J., Chen, X. R., Chen, Y. W., Chen, Y. X., Chen, Y., Chen, Z., Cheng, J., Cheng, Y. P., Cheng, Z. K., Chepurnov, A., Cherwinka, J. J., Chiarello, F., Chiesa, D., Chimenti, P., Chu, M. C., Chukanov, A., Chuvashova, A., Clementi, ., Clerbaux, B., Di Lorenzo, S. Conforti, Corti, D., Costa, S., Corso, F. D., Cummings, J. P., Dalager, O., De La Taille, C., Deng, F. S., Deng, J. W., Deng, Z., Deng, Z. Y., Depnering, W., Diaz, M., Ding, X. F., Ding, Y. Y., Dirgantara, B., Dmitrievsky, S., Diwan, M. V., Dohnal, T., Donchenko, G., Dong, J. M., Dornic, D., Doroshkevich, E., Dove, J., Dracos, M., Druillole, F., Du, S. X., Dusini, S., Dvorak, M., Dwyer, D. A., Enqvist, T., Enzmann, H., Fabbri, A., Fajt, L., Fan, D. H., Fan, L., Fang, C., Fang, J., Fatkina, A., Fedoseev, D., Fekete, V., Feng, L. C., Feng, Q. C., Fiorentini, G., Ford, R., Formozov, A., Fournier, A., Franke, S., Gallo, J. P., Gan, H. N., Gao, F., Garfagnini, A., Göttel, A., Genster, C., Giammarchi, M., Giaz, A., Giudice, N., Giuliani, F., Gonchar, M., Gong, G. H., Gong, H., Gorchakov, O., Gornushkin, Y., Grassi, M., Grewing, C., Gromov, M., Gromov, V., Gu, M. H., Gu, W. Q., Gu, X. F., Gu, Y., Guan, M. Y., Guardone, N., Gul, M., Guo, C., Guo, J. Y., Guo, L., Guo, W. L., Guo, X. H., Guo, Y. H., Guo, Z., Haacke, M., Hackenburg, R. W., Hackspacher, P., Hagner, C., Han, R., Han, Y., Hans, S., He, M., He, W., Heeger, K. M., Heinz, T., Heng, Y. K., Herrera, R., Higuera, A., Hong, D. J., Hor, Y. K., Hou, S. J., Hsiung, Y. B., Hu, B. Z., Hu, H., Hu, J. R., Hu, J., Hu, S. Y., Hu, T., Hu, Z. J., Huang, C. H., Huang, G. H., Huang, H. X., Huang, Q. H., Huang, W. H., Huang, X. T., Huang, Y. B., Huber, P., Hui, J. Q., Huo, L., Huo, W. J., Huss, C., Hussain, S., Insolia, A., Ioannisian, A., Ioannisyan, D., Isocrate, R., Jaffe, D. E., Jen, K. L., Ji, X. L., Ji, X. P., Ji, X. Z., Jia, H. H., Jia, J. J., Jian, S. Y., Jiang, D., Jiang, X. S., Jin, R. Y., Jing, X. P., Johnson, R. A., Jollet, C., Jones, D., Joutsenvaara, J., Jungthawan, S., Kalousis, L., Kampmann, P., Kang, L., Karagounis, M., Kazarian, N., Kettell, S. H., Khan, A., Khan, W., Khosonthongkee, K., Kinz, P., Kohn, S., Korablev, D., Kouzakov, K., Kramer, M., Krasnoperov, A., Krokhaleva, S., Krumshteyn, Z., Kruth, A., Kutovskiy, N., Kuusiniemi, P., Lachacinski, B., Lachenmaier, T., Langford, T. J., Lee, J., Lee, J. H. C., Lefevre, F., Lei, L., Lei, R., Leitner, R., Leung, J., Li, C., Li, D. M., Li, F., Li, H. T., Li, H. L., Li, J., Li, J. J., Li, J. Q., Li, K. J., Li, M. Z., Li, N., Li, Q. J., Li, R. H., Li, S. C., Li, S. F., Li, S. J., Li, T., Li, W. D., Li, W. G., Li, X. M., Li, X. N., Li, X. L., Li, X. Q., Li, Y., Li, Y. F., Li, Z. B., Li, Z. Y., Liang, H., Liang, J. J., Liebau, D., Limphirat, A., Limpijumnong, S., Lin, C. J., Lin, G. L., Lin, S. X., Lin, T., Lin, Y. H., Ling, J. J., Link, J. M., Lippi, I., Littenberg, L., Littlejohn, B. R., Liu, F., Liu, H., Liu, H. B., Liu, H. D., Liu, H. J., Liu, H. T., Liu, J. C., Liu, J. L., Liu, M., Liu, Q., Liu, R. X., Liu, S. Y., Liu, S. B., Liu, S. L., Liu, X. W., Liu, Y., Lokhov, A., Lombardi, P., Loo, K., Lorenz, S., Lu, C., Lu, H. Q., Lu, J. B., Lu, J. G., Lu, S. X., Lu, X. X., Lubsandorzhiev, B., Lubsandorzhiev, S., Ludhova, L., Luk, K. B., Luo, F. J., Luo, G., Luo, P. W., Luo, S., Luo, W. M., Lyashuk, V., Ma, Q. M., Ma, S., Ma, X. B., Ma, X. Y., Ma, Y. Q., Malyshkin, Y., Mantovani, F., Mao, Y. J., Mari, S. M., Marini, F., Marium, S., Marshall, C., Martellini, C., Martin-Chassard, G., Caicedo, D. A. Martinez, Martini, A., Martino, J., Mayilyan, D., McDonald, K. T., McKeown, R. D., Müller, A., Meng, G., Meng, Y., Meregaglia, A., Meroni, E., Meyhöfer, D., Mezzetto, M., Miller, J., Miramonti, L., Monforte, S., Montini, P., Montuschi, M., Morozov, N., Muralidharan, P., Napolitano, J., Nastasi, M., Naumov, D. V., Naumova, E., Nemchenok, I., Nikolaev, A., Ning, F. P., Ning, Z., Nunokawa, H., Oberauer, L., Ochoa-Ricoux, J. P., Olshevskiy, A., Ortica, F., Pan, H. R., Paoloni, A., Park, J., Parkalian, N., Parmeggiano, S., Patton, S., Payupol, T., Pec, V., Pedretti, D., Pei, Y. T., Pelliccia, N., Peng, A. G., Peng, H. P., Peng, J. C., Perrot, F., Petitjean, P. A., Rico, L. F. Pineres, Popov, A., Poussot, P., Pratumwan, W., Previtali, E., Pun, C. S. J., Qi, F. Z., Qi, M., Qian, S., Qian, X., Qian, X. H., Qiao, H., Qin, Z. H., Qiu, S. K., Rajput, M., Ranucci, G., Raper, N., Re, A., Rebber, H., Rebii, A., Ren, B., Ren, J., Reveco, C. M., Rezinko, T., Ricci, B., Robens, M., Roche, M., Rodphai, N., Rohwer, L., Romani, A., Rosero, R., Roskovec, B., Roth, C., Ruan, X. C., Ruan, X. D., Rujirawat, S., Rybnikov, A., Sadovsky, A., Saggese, P., Salamanna, G., Sangka, A., Sanguansak, N., Sawangwit, U., Sawatzki, J., Sawy, F., Schever, M., Schuler, J., Schwab, C., Schweizer, K., Selivanov, D., Selyunin, A., Serafini, A., Settanta, G., Settimo, M., Shahzad, M., Shi, G., Shi, J. Y., Shi, Y. J., Shutov, V., Sidorenkov, A., Simkovic, F., Sirignano, C., Siripak, J., Sisti, M., Slupecki, M., Smirnov, M., Smirnov, O., Sogo-Bezerra, T., Songwadhana, J., Soonthornthum, B., Sotnikov, A., Sramek, O., Sreethawong, W., Stahl, A., Stanco, L., Stankevich, K., Stefanik, D., Steiger, H., Steiner, H., Steinmann, J., Stender, M., Strati, V., Studenikin, A., Sun, G. X., Sun, L. T., Sun, J. L., Sun, S. F., Sun, X. L., Sun, Y. J., Sun, Y. Z., Suwonjandee, N., Szelezniak, M., Tang, J., Tang, Q., Tang, X., Tietzsch, A., Tkachev, I., Tmej, T., Treskov, K., Troni, G., Trzaska, W., Tse, W. -H., Tull, C. E., Tuve, C., van Waasen, S., Boom, J. Vanden, Vassilopoulos, N., Vedin, V., Verde, G., Vialkov, M., Viaud, B., Viren, B., Volpe, C., Vorobel, V., Votano, L., Walker, P., Wang, C., Wang, C. H., Wang, E., Wang, G. L., Wang, J., Wang, K. Y., Wang, L., Wang, M. F., Wang, M., Wang, N. Y., Wang, R. G., Wang, S. G., Wang, W., Wang, W. S., Wang, X., Wang, X. Y., Wang, Y., Wang, Y. F., Wang, Y. G., Wang, Y. M., Wang, Y. Q., Wang, Z., Wang, Z. M., Wang, Z. Y., Watcharangkool, A., Wei, H. Y., Wei, L. H., Wei, W., Wei, Y. D., Wen, L. J., Whisnant, K., White, C. G., Wiebusch, C., Wong, S. C. F., Wong, H. L. H., Wonsak, B., Worcester, E., Wu, C. H., Wu, D. R., Wu, F. L., Wu, Q., Wu, W. J., Wu, Z., Wurm, M., Wurtz, J., Wysotzki, C., Xi, Y. F., Xia, D. M., Xie, Y. G., Xie, Z. Q., Xing, Z. Z., Xu, D. L., Xu, F. R., Xu, H. K., Xu, J. L., Xu, J., Xu, M. H., Xu, T., Xu, Y., Xue, T., Yan, B. J., Yan, X. B., Yan, Y. P., Yang, A. B., Yang, C. G., Yang, H., Yang, J., Yang, L., Yang, X. Y., Yang, Y. F., Yang, Y. Z., Yao, H. F., Yasin, Z., Ye, J. X., Ye, M., Yegin, U., Yeh, M., Yermia, F., Yi, P. H., You, Z. Y., Young, B. L., Yu, B. X., Yu, C. X., Yu, C. Y., Yu, H. Z., Yu, M., Yu, X. H., Yu, Z. Y., Yuan, C. Z., Yuan, Y., Yuan, Z. X., Yuan, Z. Y., Yue, B. B., Zafar, N., Zambanini, A., Zeng, P., Zeng, S., Zeng, T. X., Zeng, Y. D., Zhan, L., Zhang, C., Zhang, F. Y., Zhang, G. Q., Zhang, H. H., Zhang, H. Q., Zhang, J., Zhang, J. B., Zhang, J. W., Zhang, P., Zhang, Q. M., Zhang, T., Zhang, X. M., Zhang, X. T., Zhang, Y., Zhang, Y. H., Zhang, Y. M., Zhang, Y. P., Zhang, Y. X., Zhang, Y. Y., Zhang, Z. J., Zhang, Z. P., Zhang, Z. Y., Zhao, F. Y., Zhao, J., Zhao, R., Zhao, S. J., Zhao, T. C., Zheng, D. Q., Zheng, H., Zheng, M. S., Zheng, Y. H., Zhong, W. R., Zhou, J., Zhou, L., Zhou, N., Zhou, S., Zhou, X., Zhu, J., Zhu, K. J., Zhuang, H. L., Zong, L., and Zou, J. H.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

To maximize the light yield of the liquid scintillator (LS) for the Jiangmen Underground Neutrino Observatory (JUNO), a 20 t LS sample was produced in a pilot plant at Daya Bay. The optical properties of the new LS in various compositions were studied by replacing the gadolinium-loaded LS in one antineutrino detector. The concentrations of the fluor, PPO, and the wavelength shifter, bis-MSB, were increased in 12 steps from 0.5 g/L and <0.01 mg/L to 4 g/L and 13 mg/L, respectively. The numbers of total detected photoelectrons suggest that, with the optically purified solvent, the bis-MSB concentration does not need to be more than 4 mg/L. To bridge the one order of magnitude in the detector size difference between Daya Bay and JUNO, the Daya Bay data were used to tune the parameters of a newly developed optical model. Then, the model and tuned parameters were used in the JUNO simulation. This enabled to determine the optimal composition for the JUNO LS: purified solvent LAB with 2.5 g/L PPO, and 1 to 4 mg/L bis-MSB., Comment: 13 pages, 8 figures

Published
2020

10. Studies and optimization of scintillation light measurements for the development of the 3-gamma medical imaging XEMIS2 liquid xenon Compton camera

Author

Zhu, Y., Acounis, S., Beaupère, N., Beney, J.L., Bert, J., Bouvier, S., Cai, D., Canot, C., Carlier, T., Cherel, M., Cussonneau, J.P., Diglio, S., Giovagnoli, D., Idier, J., Kraeber-Bodéré, F., Le Ray, P., Lefèvre, F., Masbou, J., Morteau, E., Stutzmann, J.S., Visvikis, D., Xing, Y., and Thers, D.

Published
2023
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11. Equation of state and optical properties of shock-compressed C:H:N:O molecular mixtures

Author

Guarguaglini, M., Hernandez, J. -A., Okuchi, T., Barroso, P., Benuzzi-Mounaix, A., Bolis, R., Brambrink, E., Fujimoto, Y., Kodama, R., Koenig, M., Lefevre, F., Miyanishi, K., Ozaki, N., Sano, T., Umeda, Y., Vinci, T., and Ravasio, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Water, ethanol, and ammonia are the key components of the mantles of Uranus and Neptune. To improve structure and evolution models and give an explanation of the magnetic fields and luminosities of the icy giants, those components need to be characterised at planetary conditions (some Mbar and a few $10^3$ K). Those conditions are typical of the Warm Dense Matter regime, which exhibits a rich phase diagram, with the coexistence of many states of matter and a large variety of chemical processes. H$_2$O, C:H:O, and C:H:N:O mixtures have been compressed up to 2.8 Mbar along the principal Hugoniot using laser-driven decaying shocks. The experiments were performed at the GEKKO XII and LULI 2000 laser facilities using standard optical diagnostics (Doppler velocimetry and pyrometry) to characterise equation of state and optical reflectivity of the shocked states. The results show that H$_2$O and the C:H:N:O mixture share the same equation of state with a density scaling, while the reflectivity behaves differently by what concerns both the onset pressures and the saturation values. The reflectivity measurement at two frequencies allows to estimate the conductivity and the complex refractive index using a Drude model.

Published
2018
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12. Laboratory radiative accretion shocks on GEKKO XII laser facility for POLAR project

Author

Som, L. Van Box, Falize, E., Koenig, M., Sakawa, Y., Albertazzi, B., Barroso, P., Bonnet-Bidaud, J. -M., Busschaert, C., Ciardi, A., Hara, Y., Katsuki, N., Kumar, R., Lefevre, F., Michaut, C., Michel, Th., Miura, T., Morita, T., Mouchet, M., Rigon, G., Sano, T., Shiiba, S., Shimogawara, H., and Tomiya, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

A new target design is presented to model high-energy radiative accretion shocks in polars. In this paper, we present the experimental results obtained on the GEKKO XII laser facility for the POLAR project. The experimental results are compared with 2D FCI2 simulations to characterize the dynamics and the structure of plasma flow before and after the collision. The good agreement between simulations and experimental data confirm the formation of a reverse shock where cooling losses start modifying the post-shock region. With the multi-material structure of the target, a hydrodynamic collimation is exhibited and a radiative structure coupled with the reverse shock is highlighted in both experimental data and simulations. The flexibility on the laser energy produced on GEKKO XII, allowed us to produce high-velocity flows and study new and interesting radiation hydrodynamic regimes between those obtained on the LULI2000 and Orion laser facilities., Comment: 8 pages, 11 figures, accepted in High Power Laser Science and Engineering journal

Published
2018

16. Ultraviolet NO and Visible O2 Nightglow in the Mars Southern Winter Polar Region: Statistical Study and Model Comparison.

Author

Soret, L., González‐Galindo, F., Gérard, J.‐C., Thomas, I. R., Ristic, B., Willame, Y., Vandaele, A. C., Hubert, B., Lefèvre, F., Daerden, F., and Patel, M. R.

Subjects
MARTIAN atmosphere, ATMOSPHERIC circulation, ATMOSPHERIC models, UPPER atmosphere, OXYGEN
Abstract

The Mars NO and the O2 nightglow are produced by the recombination of atoms produced on the dayside by photodissociation and transported to the nightside. These emissions are tracers of the summer to winter pole dynamics in the upper Mars atmosphere. The UV‐visible (UVIS) channel of the Nadir and Occultation for MArs Discovery (NOMAD) spectrometer onboard Trace Gas Orbiter (TGO) is the first instrument able to simultaneously monitor both nightglow emissions. Observations by NOMAD/UVIS during the first part of the Martian year show that both the NO and O2 nightglow emissions are enhanced near the southern winter pole. Their mean brightnesses are 15 and 108 kR, respectively. These nightglow emissions generally occur between 30 and 60 km, the NO emitting layer being consistently located ∼10 km higher than the O2 nightglow layer. Numerical simulations with the Mars Planetary Climate Model (MPCM, v6.1) properly reproduce the nightglow brightness but tend to overestimate the NO peak altitude by ∼10 km. These results suggest that the atomic oxygen density is correctly predicted by the model but that the nitrogen density altitude distribution might not be properly modeled. Plain Language Summary: Nightside emissions of the Martian upper atmosphere are excited by the recombination of atoms created on the dayside. For the first time, the NO ultraviolet emission and the O2 visible emission have been observed simultaneously with the UV‐visible (UVIS) channel of the Nadir and Occultation for MArs Discovery (NOMAD) spectrometer onboard Trace Gas Orbiter (TGO). They are used as tracers of the atmospheric dynamics to demonstrate the summer to winter pole circulation that governs the Mars upper atmosphere. We show that the two nightglow layers occur between 30 and 60 km and that they are separated by ∼10 km. We compare our results with simulations from the Mars Planetary Climate Model. Simulations manage to properly reproduce the nightglow brightness but tend to overestimate the NO peak altitude by ∼10 km. These results suggest that the atomic oxygen density is correctly predicted by the model but that the altitude distribution of the nitrogen density might not be properly modeled. Key Points: For the first time, NOMAD/UVIS simultaneously monitors both the NO UV and O2 visible nightglow in the Mars southern winter atmosphereThe NO emitting layer is consistently located ∼10 km above the O2 nightglow layer (∼55 and ∼45 km, respectively)Brightness is overall well predicted but the altitude difference between the two polar emission layers is overestimated by the MPCM v6.1 model [ABSTRACT FROM AUTHOR]

Published
2024
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19. Review: Quality of animal-source foods

Author

Prache, S., Adamiec, C., Astruc, T., Baéza-Campone, E., Bouillot, P.E., Clinquart, A., Feidt, C., Fourat, E., Gautron, J., Girard, A., Guillier, L., Kesse-Guyot, E., Lebret, B., Lefèvre, F., Le Perchec, S., Martin, B., Mirade, P.S., Pierre, F., Raulet, M., Rémond, D., Sans, P., Souchon, I., Donnars, C., and Santé-Lhoutellier, V.

Published
2022
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21. Optimization of the JUNO liquid scintillator composition using a Daya Bay antineutrino detector

Author

Abusleme, A., Adam, T., Ahmad, S., Aiello, S., Akram, M., Ali, N., An, F.P., An, G.P., An, Q., Andronico, G., Anfimov, N., Antonelli, V., Antoshkina, T., Asavapibhop, B., de André, J.P.A.M., Babic, A., Balantekin, A.B., Baldini, W., Baldoncini, M., Band, H.R., Barresi, A., Baussan, E., Bellato, M., Bernieri, E., Biare, D., Birkenfeld, T., Bishai, M., Blin, S., Blum, D., Blyth, S., Bordereau, C., Brigatti, A., Brugnera, R., Budano, A., Burgbacher, P., Buscemi, M., Bussino, S., Busto, J., Butorov, I., Cabrera, A., Cai, H., Cai, X., Cai, Y.K., Cai, Z.Y., Cammi, A., Campeny, A., Cao, C.Y., Cao, G.F., Cao, J., Caruso, R., Cerna, C., Chang, J.F., Chang, Y., Chen, H.S., Chen, P.A., Chen, P.P., Chen, S.M., Chen, S.J., Chen, X.R., Chen, Y.W., Chen, Y.X., Chen, Y., Chen, Z., Cheng, J., Cheng, Y.P., Cheng, Z.K., Chepurnov, A., Cherwinka, J.J., Chiarello, F., Chiesa, D., Chimenti, P., Chu, M.C., Chukanov, A., Chuvashova, A., Clementi, C., Clerbaux, B., Di Lorenzo, S. Conforti, Corti, D., Costa, S., Dal Corso, F., Cummings, J.P., Dalager, O., De La Taille, C., Deng, F.S., Deng, J.W., Deng, Z., Deng, Z.Y., Depnering, W., Diaz, M., Ding, X.F., Ding, Y.Y., Dirgantara, B., Dmitrievsky, S., Diwan, M.V., Dohnal, T., Donchenko, G., Dong, J.M., Dornic, D., Doroshkevich, E., Dove, J., Dracos, M., Druillole, F., Du, S.X., Dusini, S., Dvorak, M., Dwyer, D.A., Enqvist, T., Enzmann, H., Fabbri, A., Fajt, L., Fan, D.H., Fan, L., Fang, C., Fang, J., Fatkina, A., Fedoseev, D., Fekete, V., Feng, L.C., Feng, Q.C., Fiorentini, G., Ford, R., Formozov, A., Fournier, A., Franke, S., Gallo, J.P., Gan, H.N., Gao, F., Garfagnini, A., Göttel, A., Genster, C., Giammarchi, M., Giaz, A., Giudice, N., Giuliani, F., Gonchar, M., Gong, G.H., Gong, H., Gorchakov, O., Gornushkin, Y., Grassi, M., Grewing, C., Gromov, M., Gromov, V., Gu, M.H., Gu, W.Q., Gu, X.F., Gu, Y., Guan, M.Y., Guardone, N., Gul, M., Guo, C., Guo, J.Y., Guo, L., Guo, W.L., Guo, X.H., Guo, Y.H., Guo, Z., Haacke, M., Hackenburg, R.W., Hackspacher, P., Hagner, C., Han, R., Han, Y., Hans, S., He, M., He, W., Heeger, K.M., Heinz, T., Heng, Y.K., Herrera, R., Higuera, A., Hong, D.J., Hor, Y.K., Hou, S.J., Hsiung, Y.B., Hu, B.Z., Hu, H., Hu, J.R., Hu, J., Hu, S.Y., Hu, T., Hu, Z.J., Huang, C.H., Huang, G.H., Huang, H.X., Huang, Q.H., Huang, W.H., Huang, X.T., Huang, Y.B., Huber, P., Hui, J.Q., Huo, L., Huo, W.J., Huss, C., Hussain, S., Insolia, A., Ioannisian, A., Ioannisyan, D., Isocrate, R., Jaffe, D.E., Jen, K.L., Ji, X.L., Ji, X.P., Ji, X.Z., Jia, H.H., Jia, J.J., Jian, S.Y., Jiang, D., Jiang, X.S., Jin, R.Y., Jing, X.P., Johnson, R.A., Jollet, C., Jones, D., Joutsenvaara, J., Jungthawan, S., Kalousis, L., Kampmann, P., Kang, L., Karagounis, M., Kazarian, N., Kettell, S.H., Khan, A., Khan, W., Khosonthongkee, K., Kinz, P., Kohn, S., Korablev, D., Kouzakov, K., Kramer, M., Krasnoperov, A., Krokhaleva, S., Krumshteyn, Z., Kruth, A., Kutovskiy, N., Kuusiniemi, P., Lachacinski, B., Lachenmaier, T., Landini, C., Langford, T.J., Lee, J., Lee, J.H.C., Lefevre, F., Lei, L., Lei, R., Leitner, R., Leung, J., Li, D.M., Li, F., Li, H.T., Li, H.L., Li, J., Li, J.J., Li, J.Q., Li, K.J., Li, M.Z., Li, N., Li, Q.J., Li, R.H., Li, S.C., Li, S.F., Li, S.J., Li, T., Li, W.D., Li, W.G., Li, X.M., Li, X.N., Li, X.L., Li, X.Q., Li, Y., Li, Y.F., Li, Z.B., Li, Z.Y., Liang, H., Liang, J.J., Liebau, D., Limphirat, A., Limpijumnong, S., Lin, C.J., Lin, G.L., Lin, S.X., Lin, T., Lin, Y.H., Ling, J.J., Link, J.M., Lippi, I., Littenberg, L., Littlejohn, B.R., Liu, F., Liu, H., Liu, H.B., Liu, H.D., Liu, H.J., Liu, H.T., Liu, J.C., Liu, J.L., Liu, M., Liu, Q., Liu, R.X., Liu, S.Y., Liu, S.B., Liu, S.L., Liu, X.W., Liu, Y., Lokhov, A., Lombardi, P., Loo, K., Lorenz, S., Lu, C., Lu, H.Q., Lu, J.B., Lu, J.G., Lu, S.X., Lu, X.X., Lubsandorzhiev, B., Lubsandorzhiev, S., Ludhova, L., Luk, K.B., Luo, F.J., Luo, G., Luo, P.W., Luo, S., Luo, W.M., Lyashuk, V., Ma, Q.M., Ma, S., Ma, X.B., Ma, X.Y., Ma, Y.Q., Malyshkin, Y., Mantovani, F., Mao, Y.J., Mari, S.M., Marini, F., Marium, S., Marshall, C., Martellini, C., Martin-Chassard, G., Caicedo, D.A. Martinez, Martini, A., Martino, J., Mayilyan, D., McDonald, K.T., McKeown, R.D., Müller, A., Meng, G., Mednieks, I., Meng, Y., Meregaglia, A., Meroni, E., Meyhöfer, D., Mezzetto, M., Miller, J., Miramonti, L., Monforte, S., Montini, P., Montuschi, M., Morozov, N., Muralidharan, P., Napolitano, J., Nastasi, M., Naumov, D.V., Naumova, E., Nemchenok, I., Nikolaev, A., Ning, F.P., Ning, Z., Nunokawa, H., Oberauer, L., Ochoa-Ricoux, J.P., Olshevskiy, A., Ortica, F., Pan, H.R., Paoloni, A., Park, J., Parkalian, N., Parmeggiano, S., Patton, S., Payupol, T., Pec, V., Pedretti, D., Pei, Y.T., Pelliccia, N., Peng, A.G., Peng, H.P., Peng, J.C., Perrot, F., Petitjean, P.A., Rico, L.F. Pineres, Popov, A., Poussot, P., Pratumwan, W., Previtali, E., Pun, C.S.J., Qi, F.Z., Qi, M., Qian, S., Qian, X., Qian, X.H., Qiao, H., Qin, Z.H., Qiu, S.K., Rajput, M., Ranucci, G., Raper, N., Re, A., Rebber, H., Rebii, A., Ren, B., Ren, J., Reveco, C.M., Rezinko, T., Ricci, B., Robens, M., Roche, M., Rodphai, N., Rohwer, L., Romani, A., Rosero, R., Roskovec, B., Roth, C., Ruan, X.C., Ruan, X.D., Rujirawat, S., Rybnikov, A., Sadovsky, A., Saggese, P., Salamanna, G., Sangka, A., Sanguansak, N., Sawangwit, U., Sawatzki, J., Sawy, F., Schever, M., Schuler, J., Schwab, C., Schweizer, K., Selivanov, D., Selyunin, A., Serafini, A., Settanta, G., Settimo, M., Shahzad, M., Shi, G., Shi, J.Y., Shi, Y.J., Shutov, V., Sidorenkov, A., Šimkovic, F., Sirignano, C., Siripak, J., Sisti, M., Slupecki, M., Smirnov, M., Smirnov, O., Sogo-Bezerra, T., Songwadhana, J., Soonthornthum, B., Sotnikov, A., Sramek, O., Sreethawong, W., Stahl, A., Stanco, L., Stankevich, K., Štefánik, D., Steiger, H., Steiner, H., Steinmann, J., Stender, M., Strati, V., Studenikin, A., Sun, G.X., Sun, L.T., Sun, J.L., Sun, S.F., Sun, X.L., Sun, Y.J., Sun, Y.Z., Suwonjandee, N., Szelezniak, M., Tang, J., Tang, Q., Tang, X., Tietzsch, A., Tkachev, I., Tmej, T., Treskov, K., Troni, G., Trzaska, W., Tse, W.-H., Tull, C.E., Tuve, C., van Waasen, S., Boom, J. van den, Vassilopoulos, N., Vedin, V., Verde, G., Vialkov, M., Viaud, B., Viren, B., Volpe, C., Vorobel, V., Votano, L., Walker, P., Wang, C., Wang, C.H., Wang, E., Wang, G.L., Wang, J., Wang, K.Y., Wang, L., Wang, M.F., Wang, M., Wang, N.Y., Wang, R.G., Wang, S.G., Wang, W., Wang, W.S., Wang, X., Wang, X.Y., Wang, Y., Wang, Y.F., Wang, Y.G., Wang, Y.M., Wang, Y.Q., Wang, Z., Wang, Z.M., Wang, Z.Y., Watcharangkool, A., Wei, H.Y., Wei, L.H., Wei, W., Wei, Y.D., Wen, L.J., Whisnant, K., White, C.G., Wiebusch, C., Wong, S.C.F., Wong, H.L.H., Wonsak, B., Worcester, E., Wu, C.H., Wu, D.R., Wu, F.L., Wu, Q., Wu, W.J., Wu, Z., Wurm, M., Wurtz, J., Wysotzki, C., Xi, Y.F., Xia, D.M., Xie, Y.G., Xie, Z.Q., Xing, Z.Z., Xu, D.L., Xu, F.R., Xu, H.K., Xu, J.L., Xu, J., Xu, M.H., Xu, T., Xu, Y., Xue, T., Yan, B.J., Yan, X.B., Yan, Y.P., Yang, A.B., Yang, C.G., Yang, H., Yang, J., Yang, L., Yang, X.Y., Yang, Y.F., Yang, Y.Z., Yao, H.F., Yasin, Z., Ye, J.X., Ye, M., Yegin, U., Yeh, M., Yermia, F., Yi, P.H., You, Z.Y., Young, B.L., Yu, B.X., Yu, C.X., Yu, C.Y., Yu, H.Z., Yu, M., Yu, X.H., Yu, Z.Y., Yuan, C.Z., Yuan, Y., Yuan, Z.X., Yuan, Z.Y., Yue, B.B., Zafar, N., Zambanini, A., Zeng, P., Zeng, S., Zeng, T.X., Zeng, Y.D., Zhan, L., Zhang, C., Zhang, F.Y., Zhang, G.Q., Zhang, H.H., Zhang, H.Q., Zhang, J., Zhang, J.B., Zhang, J.W., Zhang, P., Zhang, Q.M., Zhang, T., Zhang, X.M., Zhang, X.T., Zhang, Y., Zhang, Y.H., Zhang, Y.M., Zhang, Y.P., Zhang, Y.X., Zhang, Y.Y., Zhang, Z.J., Zhang, Z.P., Zhang, Z.Y., Zhao, F.Y., Zhao, J., Zhao, R., Zhao, S.J., Zhao, T.C., Zheng, D.Q., Zheng, H., Zheng, M.S., Zheng, Y.H., Zhong, W.R., Zhou, J., Zhou, L., Zhou, N., Zhou, S., Zhou, X., Zhu, J., Zhu, K.J., Zhuang, H.L., Zong, L., and Zou, J.H.

Published
2021
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23. Stringent upper limits of minor species at the cloud top of Venus: PH3, HCN, and NH3.

Author

Encrenaz, T., Greathouse, T. K., Giles, R., Widemann, T., Bézard, B., Lefèvre, F., Lefèvre, M., Shao, W., Sagawa, H., Marcq, E., and Arredondo, A.

Subjects
NATURAL satellite atmospheres, INNER planets, SOUND recording & reproducing, PLANETARY atmospheres, VENUS (Planet)
Abstract

Aims. Following several reports announcing the detection or non-detection of minor species above the clouds of Venus, we have searched for other possible signatures of PH3, HCN, and NH3 in the infrared range. Methods. Since 2012, we have performed ground-based observations of Venus in the thermal infrared at various wavelengths to monitor the behavior of SO2 and H2O at the cloud top. We have identified spectral intervals where transitions of PH3 (around 955 cm−1), HCN (around 747 cm−1), and NH3 (around 951cm−1) are present. Results. From the absence of any feature at these frequencies, we derive, on the disk-integrated spectrum, a 3-σ upper limit of 3 ppbv for the PH3 mixing ratio, 0.5 ppbv for HCN, and 0.3 ppbv for NH3, assuming that these species have a constant mixing ratio throughout the atmosphere. Maps of the Venus disk recorded at the center position of the lines show that there is no evidence for local detection anywhere over the Venus disk. Conclusions. Our results bring new constraints on the maximum abundance of these species at the cloud top and in the lower mesosphere of Venus. [ABSTRACT FROM AUTHOR]

Published
2024
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24. Relationships Between HCl, H2O, Aerosols, and Temperature in the Martian Atmosphere: 1. Climatological Outlook.

Author

Olsen, K. S., Fedorova, A. A., Kass, D. M., Kleinböhl, A., Trokhimovskiy, A., Korablev, O. I., Montmessin, F., Lefèvre, F., Baggio, L., Alday, J., Belyaev, D. A., Holmes, J. A., Mason, J. P., Streeter, P. M., Rajendran, K., Patel, M. R., Patrakeev, A., and Shakun, A.

Subjects
MARTIAN atmosphere, ATMOSPHERIC chemistry, ATMOSPHERIC temperature, DUST, HYDROGEN chloride, WATER vapor
Abstract

Detecting trace gases such as hydrogen chloride (HCl) in Mars' atmosphere is among the primary objectives of the ExoMars Trace Gas Orbiter (TGO) mission. Terrestrially, HCl is closely associated with active volcanic activity, so its detection on Mars was expected to point to some form of active magmatism/outgassing. However, after its discovery using the mid‐infrared channel of the TGO Atmospheric Chemistry Suite (ACS MIR), a clear seasonality was observed, beginning with a sudden increase in HCl abundance from below detection limits to 1–3 ppbv in both hemispheres coincident with the start of dust activity, followed by very sudden and rapid loss at the southern autumnal equinox. In this study, we have investigated the relationship between HCl and atmospheric dust by making comparisons in the vertical distribution of gases measured with ACS and aerosols measured co‐located with the Mars Climate Sounder (MCS). This study includes HCl, water vapor, and ozone measured using ACS MIR, water vapor and temperature measured with the near infrared channel of ACS, and temperature, dust opacity, and water ice opacity measured with MCS. In part 1, we show that dust loading has a strong impact in temperature, which controls the abundance of water ice and water vapor, and that HCl is very closely linked to water activity. In part 2, we investigate the quantitative correlations between each quantity and discuss the possible source and sinks of HCl, their likelihood given the correlations, and any issues arising from them. Plain Language Summary: After four full Martian years in orbit since 2018, the ExoMars Trace Gas Orbiter (TGO) has observed three Martian dusty seasons, which occur when it is spring and summer in the southern hemisphere. The first, starting in summer 2018, featured a global dust storm (GDS) after which we made the first detection of hydrogen chloride (HCl) in the Martian atmosphere using the Atmospheric Chemistry Suite (ACS) instrument. Finding this gas was a priority of ExoMars because its presence may indicate that the planet is volcanically active. Since then, we have observed two more dusty periods without a GDS and observed the reappearance of HCl each time. Here, we present the climatology of HCl in both hemispheres over these three dusty periods (in Mars years 34, 35, and 36) and investigate their relationships with temperature and water vapor measured by ACS, and with airborne dust and water ice measured with the Mars Climate Sounder (MCS) on the Mars Reconnaissance Orbiter (MRO). In this paper, we examine how the vertical structure of each quantity changes over time. We show that there is a close relationship between HCl and H2O, and that both are controlled by temperature, driven by dust loading. Key Points: Comparison of trace gas abundance and aerosol extinction between Atmospheric Chemistry Suite on ExoMars TGO and Mars Climate Sounder on Mars Reconnaissance OrbiterReveal the seasonal changes in hydrogen chloride on MarsShow that dust affects atmospheric temperature, which controls water vapor abundance and ice extinction, and thus impacts HCl abundance [ABSTRACT FROM AUTHOR]

Published
2024
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25. Relationships Between HCl, H2O, Aerosols, and Temperature in the Martian Atmosphere: 2. Quantitative Correlations.

Author

Olsen, K. S., Fedorova, A. A., Kass, D. M., Kleinböhl, A., Trokhimovskiy, A., Korablev, O. I., Montmessin, F., Lefèvre, F., Baggio, L., Alday, J., Belyaev, D. A., Holmes, J. A., Mason, J. P., Streeter, P. M., Rajendran, K., Patel, M. R., Patrakeev, A., and Shakun, A.

Subjects
WATER vapor, MARTIAN atmosphere, ATMOSPHERIC chemistry, ATMOSPHERIC aerosols, HYDROLOGIC cycle
Abstract

The detection of hydrogen chloride (HCl) in the atmosphere of Mars was among the primary objectives of the ExoMars Trace Gas Orbiter (TGO) mission. Its discovery using the Atmospheric Chemistry Suite mid‐infrared channel (ACS MIR) showed a distinct seasonality and possible link to dust activity. This paper is part 2 of a study investigating the link between HCl and aerosols by comparing gas measurements made with TGO to dust and water ice opacities measured with the Mars Climate Sounder (MCS). In part 1, we showed, and compared, the seasonal evolution of vertical profiles of HCl, water vapor, temperature, dust opacity, and water ice opacity over the dusty periods around perihelion (solar longitudes 180°–360°) across Mars years 34–36. In part 2, we investigated the quantitative correlations in the vertical distribution between each quantity, as well as ozone. We show that there is a strong positive correlation between HCl and water vapor, which is expected due to fast photochemical production rates for HCl when reacting with water vapor photolysis products. We also show a strong positive correlation between water vapor and temperature, but are unable to show any correlation between temperature and HCl. There are weak correlations between the opacities of dust and water ice, and dust and water vapor, but only very low correlations between dust and HCl. We close with a discussion of possible sources and sinks and that interactions between HCl and water ice are the most likely for both, given the inter‐comparison. Plain Language Summary: The ExoMars Trace Gas Orbiter (TGO) has observed three Martian dusty seasons (summer in the southern hemisphere). In mid‐2018, we made the first detection of hydrogen chloride (HCl) in the Martian atmosphere using the Atmospheric Chemistry Suite (ACS). Finding this gas, among others, was a priority of ExoMars because its primary source may be volcanic. Since then, we have observed two more dusty periods with the reappearance of HCl each time. In part 1, we presented the climatology of HCl over these three dusty periods (in Mars years 34, 35, and 36) and investigate their relationships with temperature and water vapor measured by ACS, and with airborne dust and water ice measured with the Mars Climate Sounder (MCS) on the Mars Reconnaissance Orbiter (MRO). In this paper, part 2, we quantify the correlations between HCl, water vapor, ozone, dust, temperature, and water ice. We show that HCl is closely correlated to water vapor, which is, in turn, correlated to temperature. There is only a very low correlation between HCl and dust or water ice, which both impact water vapor. Possible mechanisms for seasonal HCl production and destruction are discussed, concluding that the freeze‐thaw cycle of atmospheric water is most likely. Key Points: Comparison of trace gases and aerosol opacity between ACS on ExoMars TGO and MCS on MROLow correlations between HCl and the opacities of dust or water ice, but very strong correlation with water vapor and the formation of icesHCl source and sink possibilities are discussed, concluding that frost activity may be the most likely possibility for both [ABSTRACT FROM AUTHOR]

Published
2024
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27. Inclusive J/psi production in pp collisions at sqrt(s) = 2.76 TeV

Author

ALICE Collaboration, Abelev, B., Adam, J., Adamova, D., Adare, A. M., Aggarwal, M. M., Rinella, G. Aglieri, Agocs, A. G., Agostinelli, A., Salazar, S. Aguilar, Ahammed, Z., Masoodi, A. Ahmad, Ahmad, N., Ahn, S. U., Akindinov, A., Aleksandrov, D., Alessandro, B., Molina, R. Alfaro, Alici, A., Alkin, A., Avina, E. Almaraz, Alme, J., Alt, T., Altini, V., Altinpinar, S., Altsybeev, I., Andrei, C., Andronic, A., Anguelov, V., Anielski, J., Anson, C., Anticic, T., Antinori, F., Antonioli, P., Aphecetche, L., Appelshauser, H., Arbor, N., Arcelli, S., Arend, A., Armesto, N., Arnaldi, R., Aronsson, T., Arsene, I. C., Arslandok, M., Asryan, A., Augustinus, A., Averbeck, R., Awes, T. C., Aysto, J., Azmi, M. D., Bach, M., Badala, A., Baek, Y. W., Bailhache, R., Bala, R., Ferroli, R. Baldini, Baldisseri, A., Baldit, A., Pedrosa, F. Baltasar Dos Santos, Ban, J., Baral, R. C., Barbera, R., Barile, F., Barnafoldi, G. G., Barnby, L. S., Barret, V., Bartke, J., Basile, M., Bastid, N., Bathen, B., Batigne, G., Batyunya, B., Baumann, C., Bearden, I. G., Beck, H., Belikov, I., Bellini, F., Bellwied, R., Belmont-Moreno, E., Bencedi, G., Beole, S., Berceanu, I., Bercuci, A., Berdnikov, Y., Berenyi, D., Bergmann, C., Berzano, D., Betev, L., Bhasin, A., Bhati, A. K., Bianchi, L., Bianchi, N., Bianchin, C., Bielcik, J., Bielcikova, J., Bjelogrlic, S., Blanco, F., Blau, D., Blume, C., Boccioli, M., Bock, N., Bogdanov, A., Boggild, H., Bogolyubsky, M., Boldizsar, L., Bombara, M., Book, J., Borel, H., Borissov, A., Bose, S., Bossu, F., Botje, M., Bottger, S., Boyer, B., Braidot, E., Braun-Munzinger, P., Bregant, M., Breitner, T., Browning, T. A., Broz, M., Brun, R., Bruna, E., Bruno, G. E., Budnikov, D., Buesching, H., Bufalino, S., Bugaiev, K., Busch, O., Buthelezi, Z., Orduna, D. Caballero, Caffarri, D., Cai, X., Caines, H., Villar, E. Calvo, Camerini, P., Roman, V. Canoa, Romeo, G. Cara, Carena, W., Carena, F., Filho, N. Carlin, Carminati, F., Montoya, C. A. Carrillo, Diaz, A. Casanova, Castellanos, J. Castillo, Hernandez, J. F. Castillo, Casula, E. A. R., Catanescu, V., Cavicchioli, C., Cepila, J., Cerello, P., Chang, B., Chapeland, S., Charvet, J. L., Chattopadhyay, S., Chawla, I., Cherney, M., Cheshkov, C., Cheynis, B., Chiavassa, E., Barroso, V. Chibante, Chinellato, D. D., Chochula, P., Chojnacki, M., Christakoglou, P., Christensen, C. H., Christiansen, P., Chujo, T., Chung, S. U., Cicalo, C., Cifarelli, L., Cindolo, F., Cleymans, J., Coccetti, F., Colamaria, F., Colella, D., Balbastre, G. Conesa, del Valle, Z. Conesa, Constantin, P., Contin, G., Contreras, J. G., Cormier, T. M., Morales, Y. Corrales, Cortese, P., Maldonado, I. Cortes, Cosentino, M. R., Costa, F., Cotallo, M. E., Crescio, E., Crochet, P., Alaniz, E. Cruz, Cuautle, E., Cunqueiro, L., Dainese, A., Dalsgaard, H. H., Danu, A., Das, K., Das, I., Das, D., Dash, A., Dash, S., De, S., de Barros, G. O. V., De Caro, A., de Cataldo, G., de Cuveland, J., De Falco, A., De Gruttola, D., Delagrange, H., Sanchez, E. Del Castillo, Deloff, A., Demanov, V., De Marco, N., Denes, E., De Pasquale, S., Deppman, A., Erasmo, G. D, de Rooij, R., Corchero, M. A. Diaz, Di Bari, D., Dietel, T., Di Giglio, C., Di Liberto, S., Di Mauro, A., Di Nezza, P., Divia, R., Djuvsland, O., Dobrin, A., Dobrowolski, T., Dominguez, I., Donigus, B., Dordic, O., Driga, O., Dubey, A. K., Ducroux, L., Dupieux, P., Majumdar, A. K. Dutta, Majumdar, M. R. Dutta, Elia, D., Emschermann, D., Engel, H., Erdal, H. A., Espagnon, B., Estienne, M., Esumi, S., Evans, D., Eyyubova, G., Fabris, D., Faivre, J., Falchieri, D., Fantoni, A., Fasel, M., Fearick, R., Fedunov, A., Fehlker, D., Feldkamp, L., Felea, D., Feofilov, G., Tellez, A. Fernandez, Ferreiro, E. G., Ferretti, A., Ferretti, R., Figiel, J., Figueredo, M. A. S., Filchagin, S., Finogeev, D., Fionda, F. M., Fiore, E. M., Floris, M., Foertsch, S., Foka, P., Fokin, S., Fragiacomo, E., Fragkiadakis, M., Frankenfeld, U., Fuchs, U., Furget, C., Girard, M. Fusco, Gaardhoje, J. J., Gagliardi, M., Gago, A., Gallio, M., Gangadharan, D. R., Ganoti, P., Garabatos, C., Garcia-Solis, E., Garishvili, I., Gerhard, J., Germain, M., Geuna, C., Gheata, A., Gheata, M., Ghidini, B., Ghosh, P., Gianotti, P., Girard, M. R., Giubellino, P., Gladysz-Dziadus, E., Glassel, P., Gomez, R., Gonzalez-Trueba, L. H., Gonzalez-Zamora, P., Gorbunov, S., Goswami, A., Gotovac, S., Grabski, V., Graczykowski, L. K., Grajcarek, R., Grelli, A., Grigoras, A., Grigoras, C., Grigoriev, V., Grigoryan, A., Grigoryan, S., Grinyov, B., Grion, N., Gros, P., Grosse-Oetringhaus, J. F., Grossiord, J. -Y., Grosso, R., Guber, F., Guernane, R., Gutierrez, C. Guerra, Guerzoni, B., Guilbaud, M., Gulbrandsen, K., Gunji, T., Gupta, A., Gupta, R., Gutbrod, H., Haaland, O., Hadjidakis, C., Haiduc, M., Hamagaki, H., Hamar, G., Han, B. H., Hanratty, L. D., Hansen, A., Harmanova, Z., Harris, J. W., Hartig, M., Hasegan, D., Hatzifotiadou, D., Hayrapetyan, A., Heckel, S. T., Heide, M., Helstrup, H., Herghelegiu, A., Corral, G. Herrera, Herrmann, N., Hetland, K. F., Hicks, B., Hille, P. T., Hippolyte, B., Horaguchi, T., Hori, Y., Hristov, P., Hrivnacova, I., Huang, M., Huber, S., Humanic, T. J., Hwang, D. S., Ichou, R., Ilkaev, R., Ilkiv, I., Inaba, M., Incani, E., Innocenti, G. M., Innocenti, P. G., Ippolitov, M., Irfan, M., Ivan, C., Ivanov, V., Ivanov, A., Ivanov, M., Ivanytskyi, O., Jacholkowski, A., Jacobs, P. M., Jancurova, L., Jang, H. J., Jangal, S., Janik, M. A., Janik, R., Jayarathna, P. H. S. Y., Jena, S., Bustamante, R. T. Jimenez, Jirden, L., Jones, P. G., Jung, H., Jusko, A., Kaidalov, A. B., Kakoyan, V., Kalcher, S., Kalinak, P., Kalisky, M., Kalliokoski, T., Kalweit, A., Kanaki, K., Kang, J. H., Kaplin, V., Uysal, A. Karasu, Karavichev, O., Karavicheva, T., Karpechev, E., Kazantsev, A., Kebschull, U., Keidel, R., Khan, M. M., Khan, S. A., Khan, P., Khanzadeev, A., Kharlov, Y., Kileng, B., Kim, M., Kim, J. S., Kim, D. J., Kim, T., Kim, B., Kim, S., Kim, S. H., Kim, D. W., Kim, J. H., Kirsch, S., Kisel, I., Kiselev, S., Kisiel, A., Klay, J. L., Klein, J., Klein-Bosing, C., Kliemant, M., Kluge, A., Knichel, M. L., Knospe, A. G., Koch, K., Kohler, M. K., Kolojvari, A., Kondratiev, V., Kondratyeva, N., Konevskikh, A., Korneev, A., Don, C. Kottachchi Kankanamge, Kour, R., Kowalski, M., Kox, S., Meethaleveedu, G. Koyithatta, Kral, J., Kralik, I., Kramer, F., Kraus, I., Krawutschke, T., Krelina, M., Kretz, M., Krivda, M., Krizek, F., Krus, M., Kryshen, E., Krzewicki, M., Kucheriaev, Y., Kuhn, C., Kuijer, P. G., Kurashvili, P., Kurepin, A., Kurepin, A. B., Kuryakin, A., Kushpil, S., Kushpil, V., Kvaerno, H., Kweon, M. J., Kwon, Y., de Guevara, P. Ladron, Lakomov, I., Langoy, R., Lara, C., Lardeux, A., La Rocca, P., Lazzeroni, C., Lea, R., Bornec, Y. Le, Lee, S. C., Lee, K. S., Lefevre, F., Lehnert, J., Leistam, L., Lenhardt, M., Lenti, V., Leon, H., Monzon, I. Leon, Vargas, H. Leon, Levai, P., Lien, J., Lietava, R., Lindal, S., Lindenstruth, V., Lippmann, C., Lisa, M. A., Liu, L., Loenne, P. I., Loggins, V. R., Loginov, V., Lohn, S., Lohner, D., Loizides, C., Loo, K. K., Lopez, X., Torres, E. Lopez, Lovhoiden, G., Lu, X. -G., Luettig, P., Lunardon, M., Luo, J., Luparello, G., Luquin, L., Luzzi, C., Ma, K., Ma, R., Madagodahettige-Don, D. M., Maevskaya, A., Mager, M., Mahapatra, D. P., Maire, A., Malaev, M., Cervantes, I. Maldonado, Malinina, L., Mal'Kevich, D., Malzacher, P., Mamonov, A., Manceau, L., Mangotra, L., Manko, V., Manso, F., Manzari, V., Mao, Y., Marchisone, M., Mares, J., Margagliotti, G. V., Margotti, A., Marin, A., Tobon, C. A. Marin, Markert, C., Martashvili, I., Martinengo, P., Martinez, M. I., Davalos, A. Martinez, Garcia, G. Martinez, Martynov, Y., Mas, A., Masciocchi, S., Masera, M., Masoni, A., Massacrier, L., Mastromarco, M., Mastroserio, A., Matthews, Z. L., Matyja, A., Mayani, D., Mayer, C., Mazer, J., Mazzoni, M. A., Meddi, F., Menchaca-Rocha, A., Perez, J. Mercado, Meres, M., Miake, Y., Milano, L., Milosevic, J., Mischke, A., Mishra, A. N., Miskowiec, D., Mitu, C., Mlynarz, J., Mohanty, A. K., Mohanty, B., Molnar, L., Zetina, L. Montano, Monteno, M., Montes, E., Moon, T., Morando, M., De Godoy, D. A. Moreira, Moretto, S., Morsch, A., Muccifora, V., Mudnic, E., Muhuri, S., Muller, H., Munhoz, M. G., Musa, L., Musso, A., Nandi, B. K., Nania, R., Nappi, E., Nattrass, C., Naumov, N. P., Navin, S., Nayak, T. K., Nazarenko, S., Nazarov, G., Nedosekin, A., Nicassio, M., Nielsen, B. S., Niida, T., Nikolaev, S., Nikolic, V., Nikulin, V., Nikulin, S., Nilsen, B. S., Nilsson, M. S., Noferini, F., Nomokonov, P., Nooren, G., Novitzky, N., Nyanin, A., Nyatha, A., Nygaard, C., Nystrand, J., Ochirov, A., Oeschler, H., Oh, S. K., Oh, S., Oleniacz, J., Oppedisano, C., Velasquez, A. Ortiz, Ortona, G., Oskarsson, A., Ostrowski, P., Otwinowski, J., Ovrebekk, G., Oyama, K., Ozawa, K., Pachmayer, Y., Pachr, M., Padilla, F., Pagano, P., Paic, G., Painke, F., Pajares, C., Pal, S. K., Pal, S., Palaha, A., Palmeri, A., Papikyan, V., Pappalardo, G. S., Park, W. J., Passfeld, A., Pastircak, B., Patalakha, D. I., Paticchio, V., Pavlinov, A., Pawlak, T., Peitzmann, T., Filho, E. Pereira De Oliveira, Peresunko, D., Lara, C. E. Perez, Lezama, E. Perez, Perini, D., Perrino, D., Peryt, W., Pesci, A., Peskov, V., Pestov, Y., Petracek, V., Petran, M., Petris, M., Petrov, P., Petrovici, M., Petta, C., Piano, S., Piccotti, A., Pikna, M., Pillot, P., Pinazza, O., Pinsky, L., Pitz, N., Piuz, F., Piyarathna, D. B., Ploskon, M., Pluta, J., Pocheptsov, T., Pochybova, S., Podesta-Lerma, P. L. M., Poghosyan, M. G., Polak, K., Polichtchouk, B., Pop, A., Porteboeuf-Houssais, S., Pospisil, V., Potukuchi, B., Prasad, S. K., Preghenella, R., Prino, F., Pruneau, C. A., Pshenichnov, I., Puchagin, S., Puddu, G., Teixido, J. Pujol, Pulvirenti, A., Punin, V., Putis, M., Putschke, J., Quercigh, E., Qvigstad, H., Rachevski, A., Rademakers, A., Radomski, S., Raiha, T. S., Rak, J., Rakotozafindrabe, A., Ramello, L., Reyes, A. Ramirez, Raniwala, S., Raniwala, R., Rasanen, S. S., Rascanu, B. T., Rathee, D., Read, K. F., Real, J. S., Redlich, K., Reichelt, P., Reicher, M., Renfordt, R., Reolon, A. R., Reshetin, A., Rettig, F., Revol, J. -P., Reygers, K., Riccati, L., Ricci, R. A., Richert, T., Richter, M., Riedler, P., Riegler, W., Riggi, F., Cahuantzi, M. Rodriguez, Roed, K., Rohr, D., Rohrich, D., Romita, R., Ronchetti, F., Rosnet, P., Rossegger, S., Rossi, A., Roukoutakis, F., Roy, C., Roy, P., Montero, A. J. Rubio, Rui, R., Ryabinkin, E., Rybicki, A., Sadovsky, S., Safarik, K., Sahoo, R., Sahu, P. K., Saini, J., Sakaguchi, H., Sakai, S., Sakata, D., Salgado, C. A., Salzwedel, J., Sambyal, S., Samsonov, V., Castro, X. Sanchez, Sandor, L., Sandoval, A., Sano, S., Sano, M., Santo, R., Santoro, R., Sarkamo, J., Scapparone, E., Scarlassara, F., Scharenberg, R. P., Schiaua, C., Schicker, R., Schmidt, H. R., Schmidt, C., Schreiner, S., Schuchmann, S., Schukraft, J., Schutz, Y., Schwarz, K., Schweda, K., Scioli, G., Scomparin, E., Scott, P. A., Scott, R., Segato, G., Selyuzhenkov, I., Senyukov, S., Seo, J., Serci, S., Serradilla, E., Sevcenco, A., Sgura, I., Shabetai, A., Shabratova, G., Shahoyan, R., Sharma, N., Sharma, S., Shigaki, K., Shimomura, M., Shtejer, K., Sibiriak, Y., Siciliano, M., Sicking, E., Siddhanta, S., Siemiarczuk, T., Silvermyr, D., Silvestre, C., Simonetti, G., Singaraju, R., Singh, R., Singha, S., Sinha, T., Sinha, B. C., Sitar, B., Sitta, M., Skaali, T. B., Skjerdal, K., Smakal, R., Smirnov, N., Snellings, R. J. M., Sogaard, C., Soltz, R., Son, H., Song, M., Song, J., Soos, C., Soramel, F., Sputowska, I., Spyropoulou-Stassinaki, M., Srivastava, B. K., Stachel, J., Stan, I., Stefanek, G., Stefanini, G., Steinbeck, T., Steinpreis, M., Stenlund, E., Steyn, G., Stocco, D., Stolpovskiy, M., Strabykin, K., Strmen, P., Suaide, A. A. P., Vasquez, M. A. Subieta, Sugitate, T., Suire, C., Sukhorukov, M., Sultanov, R., Sumbera, M., Susa, T., de Toledo, A. Szanto, Szarka, I., Szostak, A., Tagridis, C., Takahashi, J., Takaki, J. D. Tapia, Tauro, A., Munoz, G. Tejeda, Telesca, A., Terrevoli, C., Thader, J., Thomas, D., Tieulent, R., Timmins, A. R., Tlusty, D., Toia, A., Torii, H., Toscano, L., Tosello, F., Truesdale, D., Trzaska, W. H., Tsuji, T., Tumkin, A., Turrisi, R., Tveter, T. S., Ulery, J., Ullaland, K., Ulrich, J., Uras, A., Urban, J., Urciuoli, G. M., Usai, G. L., Vajzer, M., Vala, M., Palomo, L. Valencia, Vallero, S., van der Kolk, N., Vyvre, P. Vande, van Leeuwen, M., Vannucci, L., Vargas, A., Varma, R., Vasileiou, M., Vasiliev, A., Vechernin, V., Veldhoen, M., Venaruzzo, M., Vercellin, E., Vergara, S., Vernekohl, D. C., Vernet, R., Verweij, M., Vickovic, L., Viesti, G., Vikhlyantsev, O., Vilakazi, Z., Baillie, O. Villalobos, Vinogradov, A., Vinogradov, Y., Vinogradov, L., Virgili, T., Viyogi, Y. P., Vodopyanov, A., Voloshin, S., Voloshin, K., Volpe, G., von Haller, B., Vranic, D., Vrlakova, J., Vulpescu, B., Vyushin, A., Wagner, B., Wagner, V., Wan, R., Wang, Y., Wang, D., Wang, M., Watanabe, K., Wessels, J. P., Westerhoff, U., Wiechula, J., Wikne, J., Wilde, M., Wilk, G., Wilk, A., Williams, M. C. S., Windelband, B., Karampatsos, L. Xaplanteris, Yang, H., Yang, S., Yasnopolskiy, S., Yi, J., Yin, Z., Yokoyama, H., Yoo, I. -K., Yoon, J., Yu, W., Yuan, X., Yushmanov, I., Zach, C., Zampolli, C., Zaporozhets, S., Zarochentsev, A., Zavada, P., Zaviyalov, N., Zbroszczyk, H., Zelnicek, P., Zgura, I. S., Zhalov, M., Zhang, X., Zhou, D., Zhou, Y., Zhou, F., Zhu, X., Zichichi, A., Zimmermann, A., Zinovjev, G., Zoccarato, Y., and Zynovyev, M.

Subjects
High Energy Physics - Experiment
Abstract

The ALICE Collaboration has measured inclusive J/psi production in pp collisions at a center of mass energy sqrt(s)=2.76 TeV at the LHC. The results presented in this Letter refer to the rapidity ranges |y|<0.9 and 2.5

Published
2012
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29. The Role and Lifetime of Dissociative Heterogeneous Processes in Improving Simulated Ozone on Mars.

Author

Brown, M. A. J., Patel, M. R., Lewis, S. R., Holmes, J. A., Lefèvre, F., Mason, J. P., and Crismani, M.

Subjects
CLIMATE change models, GASES, TRACE gases, MARTIAN atmosphere, RADICALS (Chemistry)
Abstract

Ozone simulated in Mars Global Climate Models (MGCMs) is used to assess the underlying chemistry occurring in the atmosphere. Currently, ozone total column abundance (TCA) is under‐predicted in MGCMs by up to 120%, implying missing or inaccurate chemistry in models. Heterogeneous reactions of hydroxyl radicals (HOX) have been offered as an explanation for some of this bias, because they cause ozone to increase at locations where it's currently under‐predicted. We use four simulations to compare modeled ozone TCA with observations from the UVIS spectrometer aboard the ExoMars Trace Gas Orbiter to improve the representation of heterogeneous processes and their impact on ozone. We use a gas‐phase only run, a dissociative scheme, an adsorbed HOX retention scheme, and a hybrid scheme that combines the dissociative mechanism with the retention of HOX on water ice. We find retention of HOX is dependent on water ice sublimation, and ozone abundance increases when water ice persists for longer periods (1–20 sols). Over time, the loss of HOX causes a depletion in H2O2 concentration (HOX reservoir), and thus allows ozone concentration to increase. When adsorbed HOX are desorbed and dissociate into other by‐products, HOX are not immediately available to destroy ozone. This results in larger ozone concentrations than if desorbed HOX are released directly back into their gaseous states. When using the hybrid scheme, ozone TCA is increased up to 50% where the ozone deficit is greatest, demonstrating the best agreement with observations, and implying that HOX radicals are both retained when adsorbed and dissociate. Plain Language Summary: Ozone is a trace gas in the martian atmosphere, sensitive to chemical and light‐induced reactions. This makes it ideal for assessing the underlying reactions for chemical species called hydroxyl radicals, which destroy ozone and would otherwise be too reactive and shortlived to be measured directly. There has been an under‐prediction of ozone in global climate models which implies missing or inaccurate reactions. Heterogeneous reactions (a reaction which includes two or more phases) have been suggested to fill the deficit in modeled ozone. This involves hydroxyl radicals adsorbing onto water ice, which causes ozone to increase. We look at different simulations to understand hydroxyl radical chemistry on the surface of water ice by comparing to observations from the ExoMars Trace Gas Orbiter. We run four climate model simulations to test different theories as to what is occurring at the surface. There are two theories (a) reactions happen at the surface which alter hydroxyl radicals into other chemicals, and (b) hydroxyl radicals stay adsorbed onto water ice for as long as the ice persists. When we combine these theories, we have a more accurate prediction of ozone, which we can then use to infer what happens at the surface. Key Points: Heterogeneous reactions can have a major impact on martian ozone abundance at locations where water ice clouds persist for several solsLifetime of adsorbed hydroxyl radicals depends on water ice sublimation and longer lifetimes result in a greater abundance of ozoneA combination of longer lifetimes and dissociation of adsorbed HOX suppresses gaseous HOX and improves simulated ozone total column abundance [ABSTRACT FROM AUTHOR]

Published
2024
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30. Scintillation Signal in XEMIS2, a Liquid Xenon Compton Camera with 3γ Imaging Technique

Author

Zhu, Y., Abaline, M., Acounis, S., Beaupère, N., Beney, J. L., Bert, J., Bouvier, S., Briend, P., Butterworth, J., Carlier, T., Chanal, H., Cherel, M., Cussonneau, J. P., Dahoumane, M., Gallego-Manzano, L., Giovagnoli, D., Idier, J., Kraeber-Bodere, F., Le Ray, P., Lefèvre, F., Lemaire, O., Manen, S., Masbou, J., Mathez, H., Morteau, E., Pillet, N., Roy, D., Royer, L., Staempflin, M., Stutzmann, J. S., Vandaele, R., Virone, L., Visvikis, D., Xing, Y., Thers, D., and Liu, Zhen-An, editor

Published
2018
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31. XEMIS: Liquid Xenon Compton Camera for 3γ Imaging

Author

Xing, Y., Abaline, M., Acounis, S., Beaupère, N., Beney, J. L., Bert, J., Bouvier, S., Briend, P., Butterworth, J., Carlier, T., Chanal, H., Cherel, M., Cussonneau, J. P., Dahoumane, M., Gallego-Manzano, L., Giovagnoli, D., Idier, J., Kraeber-Bodéré, F., Le Ray, P., Lefèvre, F., Lemaire, O., Manen, S., Masbou, J., Mathez, H., Morteau, E., Pillet, N., Roy, D., Royer, L., Staempflin, M., Stutzmann, J. S., Vandaele, R., Virone, L., Visvikis, D., Zhu, Y., Thers, D., and Liu, Zhen-An, editor

Published
2018
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32. Enhancement of ferromagnetism by nickel doping in the 112 cobaltite EuBaCo2O5.50

Author

Raveau, B., Simon, Ch., Caignaert, V., Pralong, V., and Lefevre, F. X.

Subjects
Condensed Matter - Materials Science
Abstract

The study of the ordered oxygen deficient perovskite EuBaCo2-xNixO5.50 shows that the doping of cobalt sites by nickel induces a strong ferromagnetic component at low temperature in the antiferromagnetic matrix of EuBaCo2O5.50. This system exhibits indeed phase separation, i.e. consists of ferromagnetic domains embedded in the antiferromagnetic matrix of EuBaCo2O5.50. Besides, a magnetic transition is observed for the first time at 40K in the undoped and nickel doped phases, which can be attributed to the ferromagnetic ordering of the Eu3+ moments below this temperature. Moreover sharp ultra magnetization multisteps are observed below 5K, characteristic of motion of domain walls in a strong pinning system and very different from any metamagnetic transition.

Published
2006
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33. XEMIS2: A liquid xenon detector for small animal medical imaging

Author

Gallego Manzano, L., Abaline, J.M., Acounis, S., Beaupère, N., Beney, J.L., Bert, J., Bouvier, S., Briend, P., Butterworth, J., Carlier, T., Chanal, H., Cherel, M., Cussonneau, J.P., Dahoumane, M., Diglio, S., Giovagnoli, D., Idier, J., Kraeber-Bodere, F., Lefevre, F., Lemaire, O., Le Ray, P., Manen, S., Masbou, J., Mathez, H., Morteau, E., Pillet, N., Royer, L., Staempflin, M., Stutzmann, J.S., Vandaele, R., Virone, L., Visvikis, D., Xing, Y., Zhu, Y., and Thers, D.

Published
2018
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34. Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time

Author

Jakosky, B.M., Brain, D., Chaffin, M., Curry, S., Deighan, J., Grebowsky, J., Halekas, J., Leblanc, F., Lillis, R., Luhmann, J.G., Andersson, L., Andre, N., Andrews, D., Baird, D., Baker, D., Bell, J., Benna, M., Bhattacharyya, D., Bougher, S., Bowers, C., Chamberlin, P., Chaufray, J.-Y., Clarke, J., Collinson, G., Combi, M., Connerney, J., Connour, K., Correira, J., Crabb, K., Crary, F., Cravens, T., Crismani, M., Delory, G., Dewey, R., DiBraccio, G., Dong, C., Dong, Y., Dunn, P., Egan, H., Elrod, M., England, S., Eparvier, F., Ergun, R., Eriksson, A., Esman, T., Espley, J., Evans, S., Fallows, K., Fang, X., Fillingim, M., Flynn, C., Fogle, A., Fowler, C., Fox, J., Fujimoto, M., Garnier, P., Girazian, Z., Groeller, H., Gruesbeck, J., Hamil, O., Hanley, K.G., Hara, T., Harada, Y., Hermann, J., Holmberg, M., Holsclaw, G., Houston, S., Inui, S., Jain, S., Jolitz, R., Kotova, A., Kuroda, T., Larson, D., Lee, Y., Lee, C., Lefevre, F., Lentz, C., Lo, D., Lugo, R., Ma, Y.-J., Mahaffy, P., Marquette, M.L., Matsumoto, Y., Mayyasi, M., Mazelle, C., McClintock, W., McFadden, J., Medvedev, A., Mendillo, M., Meziane, K., Milby, Z., Mitchell, D., Modolo, R., Montmessin, F., Nagy, A., Nakagawa, H., Narvaez, C., Olsen, K., Pawlowski, D., Peterson, W., Rahmati, A., Roeten, K., Romanelli, N., Ruhunusiri, S., Russell, C., Sakai, S., Schneider, N., Seki, K., Sharrar, R., Shaver, S., Siskind, D.E., Slipski, M., Soobiah, Y., Steckiewicz, M., Stevens, M.H., Stewart, I., Stiepen, A., Stone, S., Tenishev, V., Terada, N., Terada, K., Thiemann, E., Tolson, R., Toth, G., Trovato, J., Vogt, M., Weber, T., Withers, P., Xu, S., Yelle, R., Yiğit, E., and Zurek, R.

Published
2018
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35. Mediterranean Forest Research Agenda 2030

Author

Bou Dagher Kharrat, Magda, primary, Martinez de Arano, Inazio, additional, Zeki-Bašken, E, additional, Feder, S, additional, Adams, Sarah, additional, Briers, Siebe, additional, Fady, B, additional, Lefèvre, F, additional, Górriz-Mifsud, Elena, additional, Mauri, Eduard, additional, Mavsar, Robert, additional, Muys, Bart, additional, Nocentini, S, additional, Pettenella, D, additional, Peñuelas, J, additional, Sardans, J, additional, Secco, L, additional, Travaglini, D, additional, Tripodi, Giuseppe, additional, Wunder, Sven, additional, and Bozzano, Michele, additional

Published
2022
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36. The STAR Silicon Strip Detector (SSD)

Author

Arnold, L., Baudot, J., Bonnet, D., Boucham, A., Bouvier, S., Castillo, J., Coffin, J. P., Drancourt, C., Erazmus, B., Gaudichet, L., Germain, M., Gojak, C., Grabski, J., Guilloux, G., Guedon, M., Hippolyte, B., Janik, M., Kisiel, A., Kuhn, C., Lakehal-Ayat, L., Lefevre, F., LeMoal, C., Leszczynski, P., Lutz, J. R., Maliszewski, A., Martin, L., Milletto, T., Pawlak, T., Peryt, W., Pluta, J., Przewlocki, M., Radomski, S., Ravel, O., Renard, C., Renault, G., Rigalleau, L. M., Roy, C., Roy, D., Suire, C., Szarwas, P., and Tarchini, A.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

The STAR Silicon Strip Detector (SSD) completes the three layers of the Silicon Vertex Tracker (SVT) to make an inner tracking system located inside the Time Projection Chamber (TPC). This additional fourth layer provides two dimensional hit position and energy loss measurements for charged particles, improving the extrapolation of TPC tracks through SVT hits. To match the high multiplicity of central Au+Au collisions at RHIC the double sided silicon strip technology was chosen which makes the SSD a half million channels detector. Dedicated electronics have been designed for both readout and control. Also a novel technique of bonding, the Tape Automated Bonding (TAB), was used to fullfill the large number of bounds to be done. All aspects of the SSD are shortly described here and test performances of produced detection modules as well as simulated results on hit reconstruction are given., Comment: 11 pages, 8 figures, 1 table

Published
2002
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38. Photon production in heavy-ion collisions close to the pion threshold

Author

Martinez, G., Aphecetche, L., Charbonnier, Y., Delagrange, H., d'Enterria, D., Matulewicz, T., Schutz, Y., Turrisi, R., Appenheimer, M., Metag, V., Novotny, R., Stroeher, H., Wolf, A. R., Wolf, M., Weiss, J., Averbeck, R., Hlavavc, S., Holzmann, R., Lefevre, F., Simon, R. S., Stratmann, R., Wissmann, F., Hoefman, M., van Goethem, M. J., Loehner, H., Ostendorf, R. W, Siemssen, R. H., Vogt, P., Wilschut, H. W., Diaz, J., Marin, A., Kugler, A., Tlusty, P., Wagner, V., and Doeppenschmidt, A.

Subjects
Nuclear Experiment
Abstract

We report on a measurement of hard photons (Eg>30 MeV) in the reaction Ar+Ca at 180A MeV at an energy in which photons from the decay of pi0 mesons are dominating. Simultaneous measurement with the TAPS spectrometer of the photon spectrum and photon-photon coincidences used for the identification of pi0 enabled the subtraction of pi0 contribution. The resulting photon spectrum exhibits an exponential shape with an inverse slope of E0=(53+-0.03(stat)-5+8(syst)) MeV. The photon multiplicity, equal to (1.21+-0.03(stat)+0.3-0.2(syst))10E0-2, is roughly one order of magnitude larger than the value extrapolated from existing systematics. This enhancement of the hard photon production is attributed to a strong increase in the contribution of secondary np collisions to the total photon yield. We conclude that, on average, the number of np collisions which contribute to the hard photon production is 7 times larger than the number of first chance np collisions in the reaction Ar+Ca at 180A MeV., Comment: 15 pages, 4 figures, references added

Published
1999
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39. SPICAM on Mars Express: A 10 year in-depth survey of the Martian atmosphere

Author

Montmessin, F., Korablev, O., Lefèvre, F., Bertaux, J.-L., Fedorova, A., Trokhimovskiy, A., Chaufray, J.Y., Lacombe, G., Reberac, A., Maltagliati, L., Willame, Y., Guslyakova, S., Gérard, J.-C., Stiepen, A., Fussen, D., Mateshvili, N., Määttänen, A., Forget, F., Witasse, O., Leblanc, F., Vandaele, A.C., Marcq, E., Sandel, B., Gondet, B., Schneider, N., Chaffin, M., and Chapron, N.

Published
2017
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44. Acceptance and resolution simulation studies for the dielectron spectrometer HADES at GSI

Author

Schicker, R., Brenschede, A., Garrow, K., Schoen, H., Balanda, A., Bokemeyer, H., Friese, J., Karig, W., Kienle, P., Koenig, W., Kuehn, W., Lefevre, F., Metag, V., Roche, G., Salabura, P., Schroeter, A., Stroth, J., and Tsertos, H.

Subjects
Nuclear Experiment
Abstract

Design studies for a second generation Dilepton Spectrometer to be built at the SIS accelerator of GSI are presented. The basic design parameters of this system are specified and the different detector components for charged particle tracking and for lepton identification are described. The geometrical acceptance for lepton pairs is given. Results on single track momentum resolution and on lepton pair mass resolution are reported., Comment: 36 pages, documentstyle[epsfig]{elsart}, 14 postscript figures (included); Submitted to NIM A

Published
1996
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46. Discovery of a proton aurora at Mars

Author

Deighan, J., Jain, S. K., Chaffin, M. S., Fang, X., Halekas, J. S., Clarke, J. T., Schneider, N. M., Stewart, A. I. F., Chaufray, J.-Y., Evans, J. S., Stevens, M. H., Mayyasi, M., Stiepen, A., Crismani, M., McClintock, W. E., Holsclaw, G. M., Lo, D. Y., Montmessin, F., Lefèvre, F., and Jakosky, B. M.

Published
2018
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47. Seasonal, Latitudinal, and Longitudinal Trends in Nighttime Ozone Vertical Structure on Mars From MAVEN/IUVS Stellar Occultations

Author

Braude, A. S., primary, Montmessin, F., additional, Schneider, N. M., additional, Gupta, S., additional, Jain, S. K., additional, Lefèvre, F., additional, Määttänen, A., additional, Verdier, L., additional, Flimon, Z., additional, Jiang, F. Y., additional, Yelle, R. V., additional, Deighan, J., additional, and Curry, S. M., additional

Published
2023
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