The Origin of the Young Stars in the Nucleus of M31 - INSPIRE

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The Origin of the Young Stars in the Nucleus of M31

Apr, 2007

10 pages

Published in:

Astrophys.J. 668 (2007) 236

e-Print:

0704.3831 [astro-ph]

DOI:

10.1086/521018

View in:

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Abstract: (arXiv)

The triple nucleus of M31 consists of a population of old red stars in an eccentric disk (P1 and P2) and another population of younger A stars in a circular disk (P3) around M31's central supermassive black hole (SMBH). We argue that P1 and P2 determine the maximal radial extent of the younger A star population and provide the gas that fueled the starburst that generated P3. The eccentric stellar disk creates an

m=1

non-axisymmetric perturbation to the potential. This perturbed potential drives gas into the inner parsec around the SMBH, if the pattern speed of the eccentric stellar disk is

\Omega_p \lesssim 3-10 {\rm km s^{-1} pc^{-1}}

. We show that stellar mass loss from P1 and P2 is sufficient to create a gravitationally unstable gaseous disk of \sim 10^5\Msun every

0.1-1

Gyrs, consistent with the 200 Myr age of P3. Similar processes may act in other systems to produce very compact nuclear starbursts.

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