Modeling mm- to X-ray flare emission from SgrA*

Details Modeling mm- to X-ray flare emission from SgrA* Modeling mm- to X-ray flare emission from SgrA*

2009-04-16

arxiv.org/abs/0904.2460v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

13 pages, 10 figures, A&A in press

Scientific paper

We report on new modeling results based on the mm- to X-ray emission of the SgrA* counterpart associated with the massive black hole at the Galactic Center. Our modeling is based on simultaneous observations carried out on 07 July, 2004, using the ESO NACO adaptive optics instrument and the ACIS-I instrument aboard the Chandra X-ray Observatory as well as the SMA and the VLA. The observations revealed several flare events in all wavelength domains. Here we show that a combined synchrotron self-Compton (SSC) model followed by an adiabatic expansion of the source components can fully account for the observed flare flux densities and delay times covering the spectral range from the X-ray to the mm-radio domain. The derived physical quantities that describe the flare emission give a blob expansion speed of v{exp}=0.005c, magnetic field of < 60G and spectral indices of 0.8 to 1.4. The derived model parameters suggest that the adiabatic expansion takes place in source components that have a bulk motion larger than v{exp} or the expanding material contributes to a corona or disk, confined to the immediate surroundings of SgrA*.

Affiliated with

Also associated with

No associations

Rating

Modeling mm- to X-ray flare emission from SgrA* does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Modeling mm- to X-ray flare emission from SgrA*, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Modeling mm- to X-ray flare emission from SgrA* will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-464755