Flares from Sgr A* and their Emission Mechanism

被引：0

作者：

Dodds-Eden, K. ^{[1
]}

Porquet, D. ^{[2
]}

Trap, G. ^{[3
,4
]}

Quataert, E. ^{[5
]}

Gillessen, S. ^{[1
]}

Grosso, N. ^{[2
]}

Genzel, R. ^{[1
,6
]}

Goldwurm, A. ^{[3
,4
]}

Yusef-Zadeh, F. ^{[7
]}

Trippe, S. ^{[8
]}

Bartko, H. ^{[1
]}

Eisenhauer, F. ^{[1
]}

Ott, T. ^{[1
]}

Fritz, T. K. ^{[1
]}

Pfuhl, O. ^{[1
]}

机构：

[1] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany

[2] Univ Strasbourg, CNRS, Observ Astron Strasbourg, INSU, Strasbourg, France

[3] CEA, Ctr Saclay, Serv Astrophys, IRFU, Gif Sur Yvette, France

[4] APC, Paris, France

[5] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[6] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[7] Northwestern Univ, Dept Phys & Astron, Evanston, IL USA

[8] Inst Radioastron Millimetr, St Martin Dheres, France

来源：

GALACTIC CENTER: A WINDOW TO THE NUCLEAR ENVIRONMENT OF DISK GALAXIES | 2011年 / 439卷

关键词：

SUPERMASSIVE BLACK-HOLE; NEAR-INFRARED FLARES; SAGITTARIUS-A; X-RAY; GALACTIC-CENTER; FLARING ACTIVITY; XMM-NEWTON;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We summarize recent observations and modeling of the brightest Sgr A* flare to be observed simultaneously in (near)-infrared and X-rays to date. Trying to explain the spectral characteristics of this flare through inverse Compton mechanisms implies physical parameters that are unrealistic for Sgr A*. Instead, a "cooling break" synchrotron model provides a more feasible explanation for the X-ray emission. In a magnetic field of about 5-30 Gauss the X-ray emitting electrons cool very quickly on the typical dynamical timescale while the NIR-emitting electrons cool more slowly. This produces a spectral break in the model between NIR and X-ray wavelengths that can explain the differences in the observed spectral indices.

引用

页码：309 / +

页数：2

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