On the X-ray Emission from the Radio Source Sgr A*

Details On the X-ray Emission from the Radio Source Sgr A* On the X-ray Emission from the Radio Source Sgr A*

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005xrrc.proce2.04c&link_type=abstract

"X-Ray and Radio Connections (eds. L.O. Sjouwerman and K.K Dyer) Published electronically by NRAO, http://www.aoc.nrao.edu/event

Computer Science

X-Ray, Radio, Colliding Stellar Winds

Scientific paper

Recent infrared observations of the Galactic center have permitted the estimation of orbital parameters for the eight O stars closest to the compact, non-thermal radio source, Sagittarius A* (Sgr A*). The emission of Sgr A* is thought to be due to the accretion of gas down the potential well of a 3×10^6 solar mass black hole at the dynamical heart of the Milky Way. The O stars are located within 0.03 parsec of Sgr A* and are likely to have significant stellar winds. Since they are deep within the potential well of a black hole, much of their winds are gravitationally bound. These hot winds may be piling up and emitting significantly in the X-rays. Thus it is possible that the emission from the recently detected compact Chandra source may, at least in part, be due to the winds of these O stars rather than the hot gas close to the event horizon of the black hole. This has serious implications for applicable black hole accretion models. From preliminary three dimensional numerical simulations which treat the eight O stars as mass and energy sources moving on individual orbits, we have constructed simulated X-ray images. We present these images and discuss their impact on accretion models for Sgr A*.

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