Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 379, Issue 1, Pages 21-33Publisher
BLACKWELL PUBLISHING
DOI: 10.1111/j.1365-2966.2007.11938.x
Keywords
accretion, accretion discs; methods : numerical; Galaxy : centre
Categories
Funding
- STFC [PP/E00119X/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E00119X/1] Funding Source: researchfish
Ask authors/readers for more resources
We numerically model fragmentation of a gravitationally unstable gaseous disc under conditions that may be appropriate for the formation of the young massive stars observed in the central parsec of our Galaxy. In this study, we adopt a simple prescription with a locally constant cooling time. We find that, for cooling times just short enough to induce disc fragmentation, stars form with a top-heavy initial mass function (IMF), as observed in the Galactic Centre (GC). For shorter cooling times, the disc fragments much more vigorously, leading to lower average stellar masses. Thermal feedback associated with gas accretion on to protostars slows down disc fragmentation, as predicted by some analytical models. We also simulate the fragmentation of a gas stream on an eccentric orbit in a combined Sgr A* plus stellar cusp gravitational potential. The stream precesses, self-collides and forms stars with a top-heavy IMF. None of our models produces large enough comoving groups of stars that could account for the observed 'ministar cluster' IRS 13E in the GC. In all of the gravitationally unstable disc models that we explored, star formation takes place too fast to allow any gas accretion on to the central supermassive black hole. While this can help to explain the quiescence of 'failed active galactic nucleus' such as Sgr A*, it poses a challenge for understanding the high gas accretion rates inferred for many quasars.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available