%0 Generic %1 Bisbas2011 %A Bisbas, Thomas G. %A Wunsch, Richard %A Whitworth, Anthony P. %A Hubber, David A. %A Walch, Stefanie %D 2011 %K pressure radiation sfr triggered %T Radiation driven implosion and triggered star formation %U http://arxiv.org/abs/1105.3727 %X We present simulations of initially stable isothermal clouds exposed to ionising radiation from a discrete external source, and identify the conditions that lead to radiatively driven implosion and star formation. We use the Smoothed Particle Hydrodynamics code SEREN and an HEALPix-based photo-ionisation algorithm to simulate the propagation of the ionising radiation and the resulting dynamical evolution of the cloud. We find that the incident ionising flux, $\Phi__LyC$, is the critical parameter determining the cloud evolution. At moderate fluxes, a large fraction of the cloud mass is converted into stars. As the flux is increased, the fraction of the cloud mass that is converted into stars and the mean masses of the individual stars both decrease. Very high fluxes simply disperse the cloud. Newly-formed stars tend to be concentrated along the central axis of the cloud (i.e. the axis pointing in the direction of the incident flux). For given cloud parameters, the time, $t__\star$, at which star formation starts is proportional to $\Phi__LyC^-1/3$. The pattern of star formation found in the simulations is similar to that observed in bright-rimmed clouds.

@misc{Bisbas2011, abstract = { We present simulations of initially stable isothermal clouds exposed to ionising radiation from a discrete external source, and identify the conditions that lead to radiatively driven implosion and star formation. We use the Smoothed Particle Hydrodynamics code SEREN and an HEALPix-based photo-ionisation algorithm to simulate the propagation of the ionising radiation and the resulting dynamical evolution of the cloud. We find that the incident ionising flux, $\Phi_{_{\rm LyC}}$, is the critical parameter determining the cloud evolution. At moderate fluxes, a large fraction of the cloud mass is converted into stars. As the flux is increased, the fraction of the cloud mass that is converted into stars and the mean masses of the individual stars both decrease. Very high fluxes simply disperse the cloud. Newly-formed stars tend to be concentrated along the central axis of the cloud (i.e. the axis pointing in the direction of the incident flux). For given cloud parameters, the time, $t_{_\star}$, at which star formation starts is proportional to $\Phi_{_{\rm LyC}}^{-1/3}$. The pattern of star formation found in the simulations is similar to that observed in bright-rimmed clouds. }, added-at = {2011-05-20T19:53:38.000+0200}, author = {Bisbas, Thomas G. and Wunsch, Richard and Whitworth, Anthony P. and Hubber, David A. and Walch, Stefanie}, biburl = {https://www.bibsonomy.org/bibtex/20ea8a7e01b814b0db93481d12e7774d5/miki}, description = {[1105.3727] Radiation driven implosion and triggered star formation}, interhash = {3a310acbfaee1577baa6d7f698ccf311}, intrahash = {0ea8a7e01b814b0db93481d12e7774d5}, keywords = {pressure radiation sfr triggered}, note = {cite arxiv:1105.3727 Comment: 36 pages, 13 figures, accepted in ApJ}, timestamp = {2011-05-20T19:53:38.000+0200}, title = {Radiation driven implosion and triggered star formation}, url = {http://arxiv.org/abs/1105.3727}, year = 2011 }