Volume 429, Number 2, January II 2005
|Page(s)||L33 - L36|
|Published online||17 December 2004|
Letter to the Editor
Using close stars as probes of hot accretion flow in Sgr A*
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, 85741 Garching, Germany e-mail: email@example.com
Accepted: 6 November 2004
The extremely hot and tenuous accretion flow in the immediate vicinity of Sgr A* is believed to be invisible (too dim) in the X-ray band, except for short X-ray flares. Here we point out that during pericenter passages, close brightest stars irradiate the inner region of the accretion flow, providing a plenty of optical/UV photons. These seed photons are Compton up-scattered by the hot electrons of the accretion flow to higher frequencies, some into the X-ray band, potentially making the innermost accretion flow much brighter in X-rays than usual. We propose to use coordinated near infra-red and X-ray observations of close star passages to put constraints onto Sgr A* accretion theories. The absence of a noticeable change in the steady emission of Sgr A* as observed by Chandra in the year 2002, when the star named S2 passed through a pericenter of its orbit, already rules out the hotter of the “standard” Advection-Dominated Accretion Flows. The less dense accretion flows, in particular the model of [CITE], passes the test and is constrained to accretion rates no larger than ~ few 10 year-1.
Key words: accretion, accretion disks / black hole physics / Galaxy: center / radiation mechanisms: general
© ESO, 2005
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