%0 Generic %1 citeulike:13242956 %A Suwa, Yudai %A Yamada, Shoichi %A Takiwaki, Tomoya %A Kotake, Kei %D 2014 %K imported %T The criterion of supernova explosion revisited: the mass accretion history %U http://arxiv.org/abs/1406.6414 %X By performing neutrino-radiation hydrodynamic simulations in spherical symmetry (1D) and axial symmetry (2D) with different progenitor models by Woosley & Heger (2007) from 12 \$M\_ødot\$ to 100 \$M\_ødot\$, we find that all 1D runs fail to produce explosion and several 2D runs succeed. The difference of shock evolution can be interpreted by the difference of mass accretion history, which is determined by the density structure of the progenitor. The exploding models exhibit high neutrino luminosity with low mass accretion rate. This is consistent with the discussion about the so-called critical curve in the mass accretion rate and neutrino luminosity plane, above which there is no steady solution of the accretion flow so that a dynamical expanding shock wave is expected. In addition, we developed a phenomenological model to evaluate the trajectories in this plane. This model reasonably reproduces the numerical results by using the initial density structure of the progenitors alone. By this model, we can predict the possibility of explosion by using the initial density structure of the progenitors alone.

@misc{citeulike:13242956, abstract = {{By performing neutrino-radiation hydrodynamic simulations in spherical symmetry (1D) and axial symmetry (2D) with different progenitor models by Woosley \& Heger (2007) from 12 \$M\_\odot\$ to 100 \$M\_\odot\$, we find that all 1D runs fail to produce explosion and several 2D runs succeed. The difference of shock evolution can be interpreted by the difference of mass accretion history, which is determined by the density structure of the progenitor. The exploding models exhibit high neutrino luminosity with low mass accretion rate. This is consistent with the discussion about the so-called critical curve in the mass accretion rate and neutrino luminosity plane, above which there is no steady solution of the accretion flow so that a dynamical expanding shock wave is expected. In addition, we developed a phenomenological model to evaluate the trajectories in this plane. This model reasonably reproduces the numerical results by using the initial density structure of the progenitors alone. By this model, we can predict the possibility of explosion by using the initial density structure of the progenitors alone.}}, added-at = {2019-03-25T08:20:55.000+0100}, archiveprefix = {arXiv}, author = {Suwa, Yudai and Yamada, Shoichi and Takiwaki, Tomoya and Kotake, Kei}, biburl = {https://www.bibsonomy.org/bibtex/23dc2b381c5f618aa3a6980b0f36f8d7b/ericblackman}, citeulike-article-id = {13242956}, citeulike-linkout-0 = {http://arxiv.org/abs/1406.6414}, citeulike-linkout-1 = {http://arxiv.org/pdf/1406.6414}, day = 24, eprint = {1406.6414}, interhash = {8904f100b6d41ae179ca3811783d99b8}, intrahash = {3dc2b381c5f618aa3a6980b0f36f8d7b}, keywords = {imported}, month = jun, posted-at = {2014-06-26 07:06:52}, priority = {2}, timestamp = {2019-03-25T08:20:55.000+0100}, title = {{The criterion of supernova explosion revisited: the mass accretion history}}, url = {http://arxiv.org/abs/1406.6414}, year = 2014 }