Stellar Feedback & Bulge Formation in Clumpy Disks

Дата и время публикации : 2011-11-28T21:00:04Z

Авторы публикации и институты :
Philip F. Hopkins (Berkeley)
Dusan Keres (Berkeley)
Norman Murray (CITA)
Eliot Quataert (Berkeley)
Lars Hernquist (Harvard)

Ссылка на журнал-издание: Mon.Not.Roy.Astron.Soc. Volume 427, Issue 2, pp. 968-978, 2012
Коментарии к cтатье: 11 pages, 4 figures, MNRAS (Revised to match accepted version, additional numerical tests added). Movies of the simulations are available at https://www.cfa.harvard.edu/~phopkins/Site/Movies_sbw.html
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO, astro-ph.GA, astro-ph.SR

Краткий обзор статьи: We use numerical simulations of isolated galaxies to study the effects of stellar feedback on the formation and evolution of giant star-forming gas ‘clumps’ in high-redshift, gas-rich galaxies. Such galactic disks are unstable to the formation of bound gas-rich clumps whose properties initially depend only on global disk properties, not the microphysics of feedback. In simulations without stellar feedback, clumps turn an order-unity fraction of their mass into stars and sink to the center, forming a large bulge and kicking most of the stars out into a much more extended stellar envelope. By contrast, strong radiative stellar feedback disrupts even the most massive clumps after they turn ~10-20% of their mass into stars, in a timescale of ~10-100 Myr, ejecting some material into a super-wind and recycling the rest of the gas into the diffuse ISM. This suppresses the bulge formation rate by direct ‘clump coalescence’ by a factor of several. However, the galactic disks do undergo significant internal evolution in the absence of mergers: clumps form and disrupt continuously and torque gas to the galactic center. The resulting evolution is qualitatively similar to bar/spiral evolution in simulations with a more homogeneous ISM.

Category: Physics