%0 Generic %1 citeulike:13658683 %A Li, Miao %A Ostriker, Jeremiah P. %A Cen, Renyue %A Bryan, Greg L. %A Naab, Thorsten %D 2015 %K imported %T Supernova Feedback and the Hot Gas Filling Fraction of the Interstellar Medium %U http://arxiv.org/abs/1506.07180 %X Supernovae are the most energetic among stellar feedback processes, and are crucial for regulating the interstellar medium (ISM) and launching galactic winds. We explore how supernova remnants (SNRs) create a multiphase medium by performing high resolution, 3D hydrodynamical simulations at various SN rates, \$S\$, and ISM average densities, \$n\$. We find that the evolution of a SNR in a self-consistently generated three-phase ISM is qualitatively different from that in a uniform or a two-phase warm/cold medium. By traveling faster and further in the cooling-inefficient hot phase, the spatial-temporal domain of a SNR is enlarged by \$>10^2.5\$ in a hot-dominated multiphase medium (HDMM) compared to the uniform case. We then examine the resultant ISM as we vary \$n\$ and \$S\$, finding that a steady state can only be achieved when the hot gas volume fraction \$0.60.1\$. Above that, overlapping SNRs render connecting topology of the hot gas, and such a HDMM is subjected to thermal runaway with growing pressure and \fvh. Photoelectric heating (PEH) has a surprisingly strong impact on \fvh. For \$n 3 cm^-3\$, a reasonable PEH rate is able to suppress the ISM from undergoing thermal runaway. Overall, we determine that the critical SN rate for the onset of thermal runaway is roughly \$S\_crit = 200 (n/1cm^-3)^k (E\_SN/10^51 erg)^-1 kpc^-3 Myr^-1\$, where k=(1.2,2.7) for \$n\$ < 1 and >1 cm\$^-3\$, respectively. We present a fitting formula of the ISM pressure \$P(n, S)\$, which can be used as an effective equation of state in cosmological simulations. The observed velocities of OB stars imply that the core collapse SN are almost randomly located on scales \$łesssim\$ 150 pc. Despite the 5 orders of magnitude span of \$(n,S)\$, the average Mach number shows very small variations: \$M 0.5\pm 0.2, 1.20.3, 2.30.9\$ for the hot, warm and cold phases, respectively.

@misc{citeulike:13658683, abstract = {Supernovae are the most energetic among stellar feedback processes, and are crucial for regulating the interstellar medium (ISM) and launching galactic winds. We explore how supernova remnants (SNRs) create a multiphase medium by performing high resolution, 3D hydrodynamical simulations at various SN rates, \$S\$, and ISM average densities, \$n\$. We find that the evolution of a SNR in a self-consistently generated three-phase ISM is qualitatively different from that in a uniform or a two-phase warm/cold medium. By traveling faster and further in the cooling-inefficient hot phase, the spatial-temporal domain of a SNR is enlarged by \$\>10^{2.5}\$ in a hot-dominated multiphase medium (HDMM) compared to the uniform case. We then examine the resultant ISM as we vary \$n\$ and \$S\$, finding that a steady state can only be achieved when the hot gas volume fraction \fvh \$\lesssim 0.6\pm 0.1\$. Above that, overlapping SNRs render connecting topology of the hot gas, and such a HDMM is subjected to thermal runaway with growing pressure and \fvh. Photoelectric heating (PEH) has a surprisingly strong impact on \fvh. For \$n \gtrsim 3 cm^{-3}\$, a reasonable PEH rate is able to suppress the ISM from undergoing thermal runaway. Overall, we determine that the critical SN rate for the onset of thermal runaway is roughly \$S\_{crit} = 200 (n/1cm^{-3})^k (E\_{SN}/10^{51} erg)^{-1} kpc^{-3} Myr^{-1}\$, where k=(1.2,2.7) for \$n\$ \< 1 and \>1 cm\$^{-3}\$, respectively. We present a fitting formula of the ISM pressure \$P(n, S)\$, which can be used as an effective equation of state in cosmological simulations. The observed velocities of OB stars imply that the core collapse SN are almost randomly located on scales \$\lesssim\$ 150 pc. Despite the 5 orders of magnitude span of \$(n,S)\$, the average Mach number shows very small variations: \$M \approx 0.5\pm 0.2, 1.2\pm 0.3, 2.3\pm 0.9\$ for the hot, warm and cold phases, respectively.}, added-at = {2019-03-25T08:20:55.000+0100}, archiveprefix = {arXiv}, author = {Li, Miao and Ostriker, Jeremiah P. and Cen, Renyue and Bryan, Greg L. and Naab, Thorsten}, biburl = {https://www.bibsonomy.org/bibtex/297fdb1b2c754ddc5ce7abe9ed15d2f5d/ericblackman}, citeulike-article-id = {13658683}, citeulike-linkout-0 = {http://arxiv.org/abs/1506.07180}, citeulike-linkout-1 = {http://arxiv.org/pdf/1506.07180}, day = 23, eprint = {1506.07180}, interhash = {652182f09df937734648510ac47415bf}, intrahash = {97fdb1b2c754ddc5ce7abe9ed15d2f5d}, keywords = {imported}, month = jun, posted-at = {2015-06-28 09:26:37}, priority = {2}, timestamp = {2019-03-25T08:20:55.000+0100}, title = {{Supernova Feedback and the Hot Gas Filling Fraction of the Interstellar Medium}}, url = {http://arxiv.org/abs/1506.07180}, year = 2015 }