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Paper: Flares from Sgr A* and their Emission Mechanism
Volume: 439, The Galactic Center: a Window to the Nuclear Environment of Disk Galaxies
Page: 309
Authors: Dodds-Eden, K.; Porquet, D.; Trap, G.; Quataert, E.; Gillessen, S.; Grosso, N.; Genzel, R.; Goldwurm, A.; Yusef-Zadeh, F.; Trippe, S.; Bartko, H.; Eisenhauer, F.; Ott, T.; Fritz, T.; Pfuhl, O.
Abstract: 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.
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