Time-resolved hadronic particle acceleration in the recurrent Nova RS Ophiuchi
Creators: name: Collaboration, H. E. S. S.
name: Aharonian, F.
name: Benkhali, F. Ait
name: Angüner, E. O.
name: Ashkar, H.
name: Backes, M.
name: Baghmanyan, V.
name: Martins, V. Barbosa
name: Batzofin, R.
name: Becherini, Y.
name: Berge, D.
name: Bernlöhr, K.
name: Bi, B.
name: Böttcher, M.
name: Boisson, C.
name: Bolmont, J.
name: de Lavergne, M. de Bony
name: Breuhaus, M.
name: Brose, R.
name: Brun, F.
name: Caroff, S.
name: Casanova, S.
name: Cerruti, M.
name: Chand, T.
name: Chen, A.
name: Cotter, G.
name: Mbarubucyeye, J. Damascene
name: Djannati-Ataï, A.
name: Dmytriiev, A.
name: Doroshenko, V.
name: Duffy, C.
name: Egberts, K.
name: Ernenwein, J. -P.
name: Fegan, S.
name: Feijen, K.
name: Fiasson, A.
name: de Clairfontaine, G. Fichet
name: Fontaine, G.
name: Füßling, M.
name: Funk, S.
name: Gabici, S.
name: Gallant, Y. A.
name: Ghafourizadeh, S.
name: Giavitto, G.
name: Giunti, L.
name: Glawion, D.
name: Glicenstein, J. F.
name: Grondin, M. -H.
name: Hermann, G.
name: Hinton, J. A.
name: Hörbe, M.
name: Hofmann, W.
name: Hoischen, C.
name: Holch, T. L.
name: Holler, M.
name: Horns, D.
name: Huang, Zhiqiu
name: Jamrozy, M.
name: Jankowsky, F.
name: Jung-Richardt, I.
name: Kasai, E.
name: Katarzyński, K.
name: Katz, U.
name: Khangulyan, D.
name: Khélifi, B.
name: Klepser, S.
name: Kluźniak, W.
name: Komin, Nu.
name: Konno, R.
name: Kosack, K.
name: Kostunin, D.
name: Stum, S. Le
name: Lemière, A.
name: Lemoine-Goumard, M.
name: Lenain, J. -P.
name: Leuschner, F.
name: Lohse, T.
name: Luashvili, A.
name: Lypova, I.
name: Mackey, J.
name: Malyshev, D.
name: Malyshev, D.
name: Marandon, V.
name: Marchegiani, P.
name: Marcowith, A.
name: Martí-Devesa, G.
name: Marx, R.
name: Maurin, G.
name: Meyer, M.
name: Mitchell, A.
name: Moderski, R.
name: Mohrmann, L.
name: Montanari, A.
name: Moulin, E.
name: Muller, J.
name: Murach, T.
name: Nakashima, K.
name: de Naurois, M.
name: Nayerhoda, A.
name: Niemiec, J.
name: Noel, A. Priyana
name: O'Brien, P.
name: Ohm, S.
name: Olivera-Nieto, L.
name: Wilhelmi, E. de Ona
name: Ostrowski, M.
name: Panny, S.
name: Panter, M.
name: Parsons, R. D.
name: Peron, G.
name: Pita, S.
name: Poireau, V.
name: Prokhorov, D. A.
name: Prokoph, H.
name: Pühlhofer, G.
name: Punch, M.
name: Quirrenbach, A.
name: Reichherzer, P.
name: Reimer, A.
name: Reimer, O.
name: Renaud, M.
name: Reville, B.
name: Rieger, F.
name: Rowell, G.
name: Rudak, B.
name: Ricarte, H. Rueda
name: Ruiz-Velasco, E.
name: Sahakian, V.
name: Sailer, S.
name: Salzmann, H.
name: Sanchez, D. A.
name: Santangelo, A.
name: Sasaki, M.
name: Schäfer, J.
name: Schüssler, F.
name: Schutte, H. M.
name: Schwanke, U.
name: Senniappan, M.
name: Shapopi, J. N. S.
name: Simoni, R.
name: Sinha, A.
name: Sol, H.
name: Specovius, A.
name: Spencer, S.
name: Stawarz, Ł.
name: Steinmassl, S.
name: Steppa, C.
name: Takahashi, T.
name: Tanaka, T.
name: Taylor, A. M.
name: Terrier, R.
name: Thorpe-Morgan, C.
name: Tsirou, M.
name: Tsuji, N.
name: Tuffs, R.
name: Uchiyama, Y.
name: Unbehaun, T.
name: van Eldik, C.
name: van Soelen, B.
name: Veh, J.
name: Venter, C.
name: Vink, J.
name: Wagner, S. J.
name: Werner, F.
name: White, R.
name: Wierzcholska, A.
name: Wong, Yu Wun
name: Yusafzai, A.
name: Zacharias, M.
name: Zargaryan, D.
name: Zdziarski, A. A.
name: Zech, A.
name: Zhu, S. J.
name: Zouari, S.
name: Żywucka, N.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Recurrent Novae are repeating thermonuclear explosions in the outer layers of white dwarfs, due to the accretion of fresh material from a binary companion. The shock generated by ejected material slamming into the companion star's wind, accelerates particles to very-high-energies. We report very-high-energy (VHE, $\gtrsim100$\,GeV) gamma rays from the recurrent nova RS\,Ophiuchi up to a month after its 2021 outburst, using the High Energy Stereoscopic System. The VHE emission has a similar temporal profile to lower-energy GeV emission, indicating a common origin, with a two-day delay in peak flux. These observations constrain models of time-dependent particle energization, favouring a hadronic emission scenario over the leptonic alternative. This confirms that shocks in dense winds provide favourable environments for efficient cosmic-ray acceleration to very-high-energies.
description: Submitted 1st Nov. 2021, first release 10th March 2022 (accepted version)