Black hole lightning due to particle acceleration at subhorizon scales

被引：114

作者：

Aleksic, J. ^{[1
]}

Ansoldi, S. ^{[2
,3
,4
]}

Antonelli, L. A. ^{[5
]}

Antoranz, P. ^{[6
,7
]}

Babic, A. ^{[8
,9
]}

Bangale, P. ^{[10
]}

Barrio, J. A. ^{[11
]}

Becerra Gonzalez, J. ^{[12
]}

Bednarek, W. ^{[13
]}

Bernardini, E. ^{[14
]}

Biasuzzi, B. ^{[2
,3
,4
]}

Biland, A. ^{[15
]}

Blanch, O. ^{[1
]}

Bonnefoy, S. ^{[11
]}

Bonnoli, G. ^{[5
]}

Borracci, F. ^{[10
]}

Bretz, T. ^{[16
]}

Carmona, E. ^{[17
]}

Carosi, A. ^{[5
]}

Colin, P. ^{[10
]}

Colombo, E. ^{[12
]}

Contreras, J. L. ^{[11
]}

Cortina, J. ^{[1
]}

Covino, S. ^{[5
]}

Da Vela, P. ^{[6
,7
]}

Dazzi, F. ^{[10
]}

De Angelis, A. ^{[2
,3
,4
]}

De Caneva, G. ^{[14
]}

De Lotto, B. ^{[2
,3
,4
]}

de Ona Wilhelmi, E. ^{[18
]}

Delgado Mendez, C. ^{[17
]}

Dominis Prester, D. ^{[8
,9
]}

Dorner, D. ^{[16
]}

Doro, M. ^{[19
,20
]}

Einecke, S. ^{[21
]}

Eisenacher, D. ^{[16
]}

Elsaesser, D. ^{[16
]}

Fonseca, M. V. ^{[11
]}

Font, L. ^{[22
,23
]}

Frantzen, K. ^{[21
]}

Fruck, C. ^{[10
]}

Galindo, D. ^{[24
]}

Garcia Lopez, R. J. ^{[12
]}

Garczarczyk, M. ^{[14
]}

Garrido Terrats, D. ^{[22
,23
]}

Gaug, M. ^{[22
,23
]}

Godinovic, N. ^{[8
,9
]}

Gonzalez Munoz, A. ^{[1
]}

Gozzini, S. R. ^{[14
]}

Hadasch, D. ^{[18
]}

机构：

[1] Inst Fis Altes Energies, E-08193 Bellaterra, Spain

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

[3] Ist Nazl Fis Nucl INFN Trieste, I-33100 Udine, Italy

[4] Ist Nazl Astrofis INAF Trieste, I-34127 Trieste, Italy

[5] INAF Natl Inst Astrophys, I-00136 Rome, Italy

[6] Univ Siena, I-53100 Siena, Italy

[7] INFN Pisa, I-53100 Siena, Italy

[8] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia

[9] Univ Split, HR-10000 Zagreb, Croatia

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

[11] Univ Complutense, E-28040 Madrid, Spain

[12] Inst Astrofis Canarias, E-38200 Tenerife, Spain

[13] Univ Lodz, PL-90236 Lodz, Poland

[14] DESY, D-15738 Zeuthen, Germany

[15] ETH, CH-8093 Zurich, Switzerland

[16] Univ Wurzburg, D-97074 Wurzburg, Germany

[17] Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain

[18] Inst Space Sci, E-08193 Barcelona, Spain

[19] Univ Padua, I-35131 Padua, Italy

[20] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[21] Tech Univ Dortmund, D-44221 Dortmund, Germany

[22] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, E-08193 Bellaterra, Spain

[23] Univ Autonoma Barcelona, Inst Estudis Espacials Catalunya, Ctr Estudios Invest Espaciales, E-08193 Bellaterra, Spain

[24] Univ Barcelona, Inst Estudis Espacials Catalunya, Inst Ciencies Cosmos, E-08028 Barcelona, Spain

[25] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan

[26] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland

[27] Univ Oulu, Dept Phys, SF-90100 Oulu, Finland

[28] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria

[29] Univ Pisa, I-56126 Pisa, Italy

[30] Ist Nazl Fis Nucl, I-56126 Pisa, Italy

[31] ICREA, E-08193 Barcelona, Spain

[32] Univ Insubria, I-22100 Como, Italy

[33] INFN Milano Bicocca, I-22100 Como, Italy

[34] Univ Erlangen Nurnberg, ECAP, Astron Inst, Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany

[35] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[36] Univ Valencia, Astron Observ, E-46980 Valencia, Spain

[37] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain

来源：

SCIENCE | 2014年 / 346卷 / 6213期

基金：

芬兰科学院;

关键词：

GAMMA-RAY EMISSION; FAST TEV VARIABILITY; RELATIVISTIC JETS; ENERGY; BLAZARS; FLARE; NUCLEUS; MODEL; M87;

D O I：

10.1126/science.1256183

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet.

引用

页码：1080 / 1084

页数：5

共 40 条

[21] Fast TeV variability in blazars: jets in a jet [J].