A young and energetic pulsar powers the well-known Crab Nebula. Here, we describe two separate gamma-ray (photon energy greater than 100 mega–electron volts) flares from this source detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The first flare occurred in February 2009 and lasted approximately 16 days. The second flare was detected in September 2010 and lasted approximately 4 days. During these outbursts, the gamma-ray flux from the nebula increased by factors of four and six, respectively. The brevity of the flares implies that the gamma rays were emitted via synchrotron radiation from peta–electron-volt (1015 electron volts) electrons in a region smaller than 1.4 × 10−2 parsecs. These are the highest-energy particles that can be associated with a discrete astronomical source, and they pose challenges to particle acceleration theory.

Gamma-Ray Flares from the Crab Nebula

BALDINI, LUCA;RAZZANO, MASSIMILIANO;
2011-01-01

Abstract

A young and energetic pulsar powers the well-known Crab Nebula. Here, we describe two separate gamma-ray (photon energy greater than 100 mega–electron volts) flares from this source detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The first flare occurred in February 2009 and lasted approximately 16 days. The second flare was detected in September 2010 and lasted approximately 4 days. During these outbursts, the gamma-ray flux from the nebula increased by factors of four and six, respectively. The brevity of the flares implies that the gamma rays were emitted via synchrotron radiation from peta–electron-volt (1015 electron volts) electrons in a region smaller than 1.4 × 10−2 parsecs. These are the highest-energy particles that can be associated with a discrete astronomical source, and they pose challenges to particle acceleration theory.
2011
Abdo, Aa; Ackermann, M; Ajello, M; Allafort, A; Baldini, Luca; Ballet, J; Barbiellini, G; Bastieri, D; Bechtol, K; Bellazzini, R; Berenji, B; Blandford, Rd; Bloom, Ed; Bonamente, E; Borgland, Aw; Bouvier, A; Brandt, Tj; Bregeon, J; Brez, A; Brigida, M; Bruel, P; Buehler, R; Buson, S; Caliandro, Ga; Cameron, Ra; Cannon, A; Caraveo, Pa; Casandjian, Jm; Celik, O; Charles, E; Chekhtman, A; Cheung, Cc; Chiang, J; Ciprini, S; Claus, R; Cohen Tanugi, J; Costamante, L; Cutini, S; D'Ammando, F; Dermer, Cd; de Angelis, A; de Luca, A; de Palma, F; Digel, Sw; Silva, Ede; Drell, Ps; Drlica Wagner, A; Dubois, R; Dumora, D; Favuzzi, C; Fegan, Sj; Ferrara, Ec; Focke, Wb; Fortin, P; Frailis, M; Fukazawa, Y; Funk, S; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Germani, S; Giglietto, N; Giordano, F; Giroletti, M; Glanzman, T; Godfrey, G; Grenier, Ia; Grondin, Mh; Grove, Je; Guiriec, S; Hadasch, D; Hanabata, Y; Harding, Ak; Hayashi, K; Hayashida, M; Hays, E; Horan, D; Itoh, R; Johannesson, G; Johnson, As; Johnson, Tj; Khangulyan, D; Kamae, T; Katagiri, H; Kataoka, J; Kerr, M; Knodlseder, J; Kuss, M; Lande, J; Latronico, L; Lee, Sh; Lemoine Goumard, M; Longo, F; Loparco, F; Lubrano, P; Madejski, Gm; Makeev, A; Marelli, M; Mazziotta, Mn; Mcenery, Je; Michelson, Pf; Mitthumsiri, W; Mizuno, T; Moiseev, Aa; Monte, C; Monzani, Me; Morselli, A; Moskalenko, Iv; Murgia, S; Nakamori, T; Naumann Godo, M; Nolan, Pl; Norris, Jp; Nuss, E; Ohsugi, T; Okumura, A; Omodei, N; Ormes, Jf; Ozaki, M; Paneque, D; Parent, D; Pelassa, V; Pepe, M; Pesce Rollins, M; Pierbattista, M; Piron, F; Porter, Ta; Raino, S; Rando, R; Ray, Ps; Razzano, Massimiliano; Reimer, A; Reimer, O; Reposeur, T; Ritz, S; Romani, Rw; Sadrozinski, Hfw; Sanchez, D; Parkinson, Pms; Scargle, Jd; Schalk, Tl; Sgro, C; Siskind, Ej; Smith, Pd; Spandre, G; Spinelli, P; Strickman, Ms; Suson, Dj; Takahashi, H; Takahashi, T; Tanaka, T; Thayer, Jb; Thompson, Dj; Tibaldo, L; Torres, Df; Tosti, G; Tramacere, A; Troja, E; Uchiyama, Y; Vandenbroucke, J; Vasileiou, V; Vianello, G; Vitale, V; Wang, P; Wood, Ks; Yang, Z; Ziegler, M.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11568/190343
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