%0 Generic %1 tsukamoto2014effects %A Tsukamoto, Yusuke %A Takahashi, Sanemichi Z. %A Machida, Masahiro N. %A Inutsuka, Shu-ichiro %D 2014 %K 2014 PPD a:Tsukamoto a:takahashi radiative-transfer self-gravity %T Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments %U http://arxiv.org/abs/1404.7271 %X We investigate structure of self-gravitating disks, their fragmentation and evolution of the fragments (the clumps) using both analytic approach and three-dimensional radiation hydrodynamics simulations. The simulations show that non-local radiation transfer determines disk temperature. We find the disk structure is well described by an analytical model of quasi-steady self-gravitating disk. Because the radiation process is not local and radiation from the interstellar medium cannot be ignored, the local balance between the radiation cooling and the viscous heating is not achieved in a massive disk around a low mass star. In our simulations, there are cases in which the disk does not fragment even though it satisfies the fragmentation criterion based on disk cooling time ($Q 1$ and $Ømega t_cool1$). This indicates that at least the criterion is not sufficient condition for fragmentation. We also investigate the disk fragmentation process induced by mass accretion from the envelope. We determine the parameter range for the host cloud core in which disk fragmentation occurs. In addition, we show that the temperature evolution of the center of the clump is almost consistent with that of a typical first core and we show the minimum initial mass of clumps to be about a few Jupiter mass.

@misc{tsukamoto2014effects, abstract = {We investigate structure of self-gravitating disks, their fragmentation and evolution of the fragments (the clumps) using both analytic approach and three-dimensional radiation hydrodynamics simulations. The simulations show that non-local radiation transfer determines disk temperature. We find the disk structure is well described by an analytical model of quasi-steady self-gravitating disk. Because the radiation process is not local and radiation from the interstellar medium cannot be ignored, the local balance between the radiation cooling and the viscous heating is not achieved in a massive disk around a low mass star. In our simulations, there are cases in which the disk does not fragment even though it satisfies the fragmentation criterion based on disk cooling time ($Q \sim 1$ and $\Omega t_{\rm cool}\sim 1$). This indicates that at least the criterion is not sufficient condition for fragmentation. We also investigate the disk fragmentation process induced by mass accretion from the envelope. We determine the parameter range for the host cloud core in which disk fragmentation occurs. In addition, we show that the temperature evolution of the center of the clump is almost consistent with that of a typical first core and we show the minimum initial mass of clumps to be about a few Jupiter mass.}, added-at = {2014-08-05T16:33:24.000+0200}, author = {Tsukamoto, Yusuke and Takahashi, Sanemichi Z. and Machida, Masahiro N. and Inutsuka, Shu-ichiro}, biburl = {https://www.bibsonomy.org/bibtex/2e1b09e7cdacf67af95e97fdbc386d702/danielcarrera}, description = {[1404.7271] Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments}, interhash = {ab5188c57294e42358bf7904c4a4b349}, intrahash = {e1b09e7cdacf67af95e97fdbc386d702}, keywords = {2014 PPD a:Tsukamoto a:takahashi radiative-transfer self-gravity}, note = {cite arxiv:1404.7271Comment: 17 pages, 13 figures, submitted to MNRAS}, timestamp = {2014-08-05T16:33:24.000+0200}, title = {Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments}, url = {http://arxiv.org/abs/1404.7271}, year = 2014 }