Fermi-LAT Observations of High-energy Behind-the-limb Solar Flares

被引：47

作者：

Ackermann, M. ^{[1
]}

Allafort, A. ^{[2
,3
]}

Baldini, L. ^{[4
,5
]}

Barbiellini, G. ^{[6
,7
]}

Bastieri, D. ^{[8
,9
]}

Bellazzini, R. ^{[10
]}

Bissaldi, E. ^{[11
]}

Bonino, R. ^{[12
,13
]}

Bottacini, E. ^{[2
,3
]}

Bregeon, J. ^{[14
]}

Bruel, P. ^{[15
]}

Buehler, R. ^{[1
]}

Cameron, R. A. ^{[2
,3
]}

Caragiulo, M. ^{[11
,16
]}

Caraveo, P. A. ^{[17
]}

Cavazzuti, E. ^{[18
]}

Cecchi, C. ^{[19
,20
]}

Charles, E. ^{[2
,3
]}

Ciprini, S. ^{[18
,19
]}

Costanza, F. ^{[11
]}

Cutini, S. ^{[18
,19
]}

D'Ammando, F. ^{[21
,22
]}

de Palma, F. ^{[11
,23
]}

Desiante, R. ^{[12
,24
]}

Digel, S. W. ^{[2
,3
]}

Di Lalla, N. ^{[4
,5
]}

Di Mauro, M. ^{[2
,3
]}

Di Venere, L. ^{[11
,16
]}

Drell, P. S. ^{[2
,3
]}

Favuzzi, C. ^{[11
,16
]}

Fukazawa, Y. ^{[25
]}

Fusco, P. ^{[16
]}

Gargano, F. ^{[11
]}

Giglietto, N. ^{[11
,16
]}

Giordano, F. ^{[11
,16
]}

Giroletti, M. ^{[21
]}

Grenier, I. A. ^{[26
]}

Guillemot, L. ^{[27
,28
]}

Guiriec, S. ^{[29
,30
]}

Jogler, T. ^{[31
]}

Johannesson, G. ^{[32
]}

Kashapova, L. ^{[33
]}

Krucker, S. ^{[34
,35
]}

Kuss, M. ^{[10
]}

La Mura, G. ^{[9
]}

Larsson, S. ^{[36
,37
]}

Latronico, L. ^{[12
]}

Li, J. ^{[38
]}

Liu, W. ^{[2
,3
,39
,40
]}

Longo, F. ^{[6
,7
]}

机构：

[1] DESY, D-15738 Zeuthen, Germany

[2] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA

[3] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[4] Univ Pisa, I-56127 Pisa, Italy

[5] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[6] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[7] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[8] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[9] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[10] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[11] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[12] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[13] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy

[14] Univ Montpellier, CNRS IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France

[15] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[16] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[17] INAF Ist Astrofis Spaziale & Fis Cosm Milano, Via E Bassini 15, I-20133 Milan, Italy

[18] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy

[19] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[20] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[21] INAF Ist Radioastron, I-40129 Bologna, Italy

[22] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[23] Univ Telemat Pegaso, Piazza Trieste Trento 48, I-80132 Naples, Italy

[24] Univ Udine, I-33100 Udine, Italy

[25] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan

[26] CEA Saclay, Serv Astrophys, CEA IRFU CNRS Univ Paris Diderot, Lab AIM, F-91191 Gif Sur Yvette, France

[27] Univ Orleans, CNRS, Lab Phys & Chim Environnem & Espace, F-45071 Orleans 02, France

[28] Observ Paris, CNRS INSU, Stn Radioastron Nancay, F-18330 Nancay, France

[29] Goddard Space Flight Ctr, NASA, Greenbelt, MD 20771 USA

[30] Friedrich Alexander Univ, Schlosspl 4, D-91054 Erlangen, Germany

[31] Univ Iceland, Sci Inst, IS-107 Reykjavik, Iceland

[32] NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[33] Inst Solar Terrestrial SB RAS, Lermontov St 126a, Irkutsk 664003, Russia

[34] Univ Appl Sci & Arts NW Switzerland, CH-5210 Windisch, Switzerland

[35] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[36] KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden

[37] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[38] Campus UAB, Inst Space Sci IEEC CSIC, Carrer Magrans S-N, E-08193 Barcelona, Spain

[39] Bay Area Environm Res Inst, 625 2nd St,Suite 209, Petaluma, CA 94952 USA

[40] Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St,Bldg 252, Palo Alto, CA 94304 USA

[41] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[42] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[43] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand

[44] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan

[45] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[46] Vedeneeva 2-31, St Petersburg, Russia

[47] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[48] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

[49] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[50] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 835卷 / 02期

关键词：

Sun: flares; Sun:; X-rays; gamma rays; GAMMA-RAY EMISSION; HARD X-RAY; LARGE-AREA TELESCOPE; STOCHASTIC ACCELERATION; EVENT;

D O I：

10.3847/1538-4357/835/2/219

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the Fermi-LAT detection of high-energy emission from the behind-the-limb (BTL) solar flares that occurred on 2013 October 11, and 2014 January 6 and September 1. The Fermi-LAT observations are associated with flares from active regions originating behind both the eastern and western limbs, as determined by STEREO. All three flares are associated with very fast coronal mass ejections (CMEs) and strong solar energetic particle events. We present updated localizations of the > 100 MeV photon emission, hard X-ray (HXR) and EUV images, and broadband spectra from 10 keV to 10 GeV, as well as microwave spectra. We also provide a comparison of the BTL flares detected by Fermi-LAT with three on-disk flares and present a study of some of the significant quantities of these flares as an attempt to better understand the acceleration mechanisms at work during these occulted flares. We interpret the HXR emission to be due to electron bremsstrahlung from a coronal thin-target loop top with the accelerated electron spectra steepening at semirelativistic energies. The > 100 MeV gamma-rays are best described by a pion-decay model resulting from the interaction of protons (and other ions) in a thick-target photospheric source. The protons are believed to have been accelerated (to energies > 10 GeV) in the CME environment and precipitate down to the photosphere from the downstream side of the CME shock and landed on the front side of the Sun, away from the original flare site and the HXR emission.

引用

页数：13

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