%0 Generic %1 tsang2017radiation %A Tsang, Benny Tsz-Ho %A Milosavljevic, Milos %D 2017 %K accretion cluster feedback formation radiation star %T Radiation pressure in super star cluster formation %U http://arxiv.org/abs/1709.07539 %X The physics of star formation at its extreme, in the nuclei of the largest and densest star clusters in the universe - potential massive black hole nurseries - has for decades eluded scrutiny. Spectroscopy of these systems has been scarce, whereas theoretical claims have been made that radiation pressure on dust grains somehow inhibits star formation. Here, we harness an accelerated Monte Carlo radiation transport scheme to report a radiation hydrodynamical simulation of super star cluster formation in turbulent clouds. We find that radiation pressure reduces the global star formation efficiency by 30-35%, and the star formation rate by 15-50%, both relative to a radiation-free control run. Overall, radiation pressure is ineffective in limiting the gas supply for star formation and the final stellar mass of the most massive cluster is $\sim 1.3\times10^6\,M_ødot$. The limited impact as compared to that implied by idealized theoretical models is attributed to a radiation-matter anti-correlation in the supersonically turbulent, gravitationally collapsing medium. In isolated regions outside massive clusters, where the gas distribution is less disturbed, radiation pressure is more effective in limiting star formation. The resulting stellar density at the cluster core is $10^8\,M_ødot\,pc^-3$, with stellar velocity dispersion $70\,km\,s^-1$. We conclude that the super star cluster nucleus is propitious to the formation of very massive stars via dynamical core collapse and stellar merging. We speculate that the very massive star may avoid the claimed catastrophic mass loss by continuing to accrete dense gas condensing from a gravitationally-confined ionized phase.

@misc{tsang2017radiation, abstract = {The physics of star formation at its extreme, in the nuclei of the largest and densest star clusters in the universe - potential massive black hole nurseries - has for decades eluded scrutiny. Spectroscopy of these systems has been scarce, whereas theoretical claims have been made that radiation pressure on dust grains somehow inhibits star formation. Here, we harness an accelerated Monte Carlo radiation transport scheme to report a radiation hydrodynamical simulation of super star cluster formation in turbulent clouds. We find that radiation pressure reduces the global star formation efficiency by 30-35%, and the star formation rate by 15-50%, both relative to a radiation-free control run. Overall, radiation pressure is ineffective in limiting the gas supply for star formation and the final stellar mass of the most massive cluster is $\sim 1.3\times10^6\,M_\odot$. The limited impact as compared to that implied by idealized theoretical models is attributed to a radiation-matter anti-correlation in the supersonically turbulent, gravitationally collapsing medium. In isolated regions outside massive clusters, where the gas distribution is less disturbed, radiation pressure is more effective in limiting star formation. The resulting stellar density at the cluster core is $\ge 10^{8}\,M_{\odot}\,\textrm{pc}^{-3}$, with stellar velocity dispersion $\gtrsim 70\,\text{km}\,\text{s}^{-1}$. We conclude that the super star cluster nucleus is propitious to the formation of very massive stars via dynamical core collapse and stellar merging. We speculate that the very massive star may avoid the claimed catastrophic mass loss by continuing to accrete dense gas condensing from a gravitationally-confined ionized phase.}, added-at = {2017-09-25T10:24:47.000+0200}, author = {Tsang, Benny Tsz-Ho and Milosavljevic, Milos}, biburl = {https://www.bibsonomy.org/bibtex/2969e690b9b40e14cddb2ba51809db495/miki}, description = {[1709.07539] Radiation pressure in super star cluster formation}, interhash = {ffa151646e2d2dcaab95879af0480c3f}, intrahash = {969e690b9b40e14cddb2ba51809db495}, keywords = {accretion cluster feedback formation radiation star}, note = {cite arxiv:1709.07539Comment: 20 pages, 16 figures}, timestamp = {2017-09-25T10:24:47.000+0200}, title = {Radiation pressure in super star cluster formation}, url = {http://arxiv.org/abs/1709.07539}, year = 2017 }