Coronal radiation of a cusp of spun-up stars and the X-ray luminosity of Sgr A*

TL;DR

The paper proposes that the X-ray emission observed near Sgr A* may largely originate from rapidly rotating, coronally active stars in the central region, affecting estimates of the black hole's accretion rate.

Contribution

It introduces a model where stellar coronae significantly contribute to Sgr A*'s X-ray luminosity, providing new constraints on the stellar population and accretion processes.

Findings

X-ray emission can be explained by active stars in the Galactic center.

Stellar activity may cause variability in the X-ray signal.

Implications for lower accretion rates of Sgr A*.

Abstract

Chandra has detected optically thin, thermal X-ray emission with a size of ~1 arcsec and luminosity ~10^33 erg/s from the direction of the Galactic supermassive black hole (SMBH), Sgr A*. We suggest that a significant or even dominant fraction of this signal may be produced by several thousand late-type main-sequence stars that possibly hide in the central ~0.1 pc region of the Galaxy. As a result of tidal spin-ups caused by close encounters with other stars and stellar remnants, these stars should be rapidly rotating and hence have hot coronae, emitting copious amounts of X-ray emission with temperatures kT<~ a few keV. The Chandra data thus place an interesting upper limit on the space density of (currently unobservable) low-mass main-sequence stars near Sgr A*. This bound is close to and consistent with current constraints on the central stellar cusp provided by infrared observations. If coronally active stars do provide a significant fraction of the X-ray luminosity of Sgr A*, it should be variable on hourly and daily time scales due to giant flares occurring on different stars. Another consequence is that the quiescent X-ray luminosity and accretion rate of the SMBH are yet lower than believed before.