Discrete Effects in Stellar Feedback: Individual Supernovae, Hypernovae, and IMF Sampling in Dwarf Galaxies. Su, K., Hopkins, P. F., Hayward, C. C., Ma, X., Boylan-Kolchin, M., Kasen, D., Kereš, D., Faucher-Giguère, C., & Orr, M. E. ArXiv e-prints, 1712:arXiv:1712.02795, December, 2017. ![Discrete Effects in Stellar Feedback: Individual Supernovae, Hypernovae, and IMF Sampling in Dwarf Galaxies [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex Using high-resolution simulations from the FIRE-2 (Feedback In Realistic Environments) project, we study the effects of discreteness in stellar feedback processes on the evolution of galaxies and the properties of the interstellar medium (ISM). We specifically consider the discretization of supernovae (SNe), including hypernovae (HNe), and sampling the initial mass function (IMF). We study these processes in cosmological simulations of dwarf galaxies with \$z=0\$ stellar masses \$M_\{{\textbackslash}ast\}{\textbackslash}sim 10{\textasciicircum}\{4\}-3{\textbackslash}times10{\textasciicircum}\{6\}{\textbackslash},M_{\textbackslash}odot\$ (halo masses \${\textbackslash}sim 10{\textasciicircum}\{9\}-10{\textasciicircum}\{10\}{\textbackslash},M_{\textbackslash}odot\$). We show that the discrete nature of individual SNe (as opposed to a model in which their energy/momentum deposition is continuous over time, similar to stellar winds) is crucial in generating a reasonable ISM structure and galactic winds and in regulating dwarf stellar masses. However, once SNe are discretized, accounting for the effects of IMF sampling on continuous mechanisms such as radiative feedback and stellar mass-loss (as opposed to adopting IMF-averaged rates) has weak effects on galaxy-scale properties. We also consider the effects of rare HNe events with energies \${\textbackslash}sim 10{\textasciicircum}\{53\}{\textbackslash},\{{\textbackslash}rm erg\}\$. The effects of HNe are similar to the effects of clustered explosions of SNe – which are already captured in our default simulation setup – and do not quench star formation (provided that the HNe do not dominate the total SNe energy budget), which suggests that HNe yield products should be observable in ultra-faint dwarfs today.
@article{su_discrete_2017,
title = {Discrete {Effects} in {Stellar} {Feedback}: {Individual} {Supernovae}, {Hypernovae}, and {IMF} {Sampling} in {Dwarf} {Galaxies}},
volume = {1712},
shorttitle = {Discrete {Effects} in {Stellar} {Feedback}},
url = {http://adsabs.harvard.edu/abs/2017arXiv171202795S},
abstract = {Using high-resolution simulations from the FIRE-2 (Feedback In Realistic
Environments) project, we study the effects of discreteness in stellar
feedback processes on the evolution of galaxies and the properties of
the interstellar medium (ISM). We specifically consider the
discretization of supernovae (SNe), including hypernovae (HNe), and
sampling the initial mass function (IMF). We study these processes in
cosmological simulations of dwarf galaxies with \$z=0\$ stellar masses
\$M\_\{{\textbackslash}ast\}{\textbackslash}sim 10{\textasciicircum}\{4\}-3{\textbackslash}times10{\textasciicircum}\{6\}{\textbackslash},M\_{\textbackslash}odot\$ (halo masses \${\textbackslash}sim
10{\textasciicircum}\{9\}-10{\textasciicircum}\{10\}{\textbackslash},M\_{\textbackslash}odot\$). We show that the discrete nature of
individual SNe (as opposed to a model in which their energy/momentum
deposition is continuous over time, similar to stellar winds) is crucial
in generating a reasonable ISM structure and galactic winds and in
regulating dwarf stellar masses. However, once SNe are discretized,
accounting for the effects of IMF sampling on continuous mechanisms such
as radiative feedback and stellar mass-loss (as opposed to adopting
IMF-averaged rates) has weak effects on galaxy-scale properties. We also
consider the effects of rare HNe events with energies \${\textbackslash}sim
10{\textasciicircum}\{53\}{\textbackslash},\{{\textbackslash}rm erg\}\$. The effects of HNe are similar to the effects of
clustered explosions of SNe -- which are already captured in our default
simulation setup -- and do not quench star formation (provided that the
HNe do not dominate the total SNe energy budget), which suggests that
HNe yield products should be observable in ultra-faint dwarfs today.},
urldate = {2018-01-10},
journal = {ArXiv e-prints},
author = {Su, Kung-Yi and Hopkins, Philip F. and Hayward, Christopher C. and Ma, Xiangcheng and Boylan-Kolchin, Michael and Kasen, Daniel and Kereš, Dušan and Faucher-Giguère, Claude-Andrè and Orr, Matthew E.},
month = dec,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:1712.02795},
}
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We specifically consider the discretization of supernovae (SNe), including hypernovae (HNe), and sampling the initial mass function (IMF). We study these processes in cosmological simulations of dwarf galaxies with \\$z=0\\$ stellar masses \\$M_\\{{\\textbackslash}ast\\}{\\textbackslash}sim 10{\\textasciicircum}\\{4\\}-3{\\textbackslash}times10{\\textasciicircum}\\{6\\}{\\textbackslash},M_{\\textbackslash}odot\\$ (halo masses \\${\\textbackslash}sim 10{\\textasciicircum}\\{9\\}-10{\\textasciicircum}\\{10\\}{\\textbackslash},M_{\\textbackslash}odot\\$). We show that the discrete nature of individual SNe (as opposed to a model in which their energy/momentum deposition is continuous over time, similar to stellar winds) is crucial in generating a reasonable ISM structure and galactic winds and in regulating dwarf stellar masses. However, once SNe are discretized, accounting for the effects of IMF sampling on continuous mechanisms such as radiative feedback and stellar mass-loss (as opposed to adopting IMF-averaged rates) has weak effects on galaxy-scale properties. We also consider the effects of rare HNe events with energies \\${\\textbackslash}sim 10{\\textasciicircum}\\{53\\}{\\textbackslash},\\{{\\textbackslash}rm erg\\}\\$. The effects of HNe are similar to the effects of clustered explosions of SNe – which are already captured in our default simulation setup – and do not quench star formation (provided that the HNe do not dominate the total SNe energy budget), which suggests that HNe yield products should be observable in ultra-faint dwarfs today.","urldate":"2018-01-10","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Su"],"firstnames":["Kung-Yi"],"suffixes":[]},{"propositions":[],"lastnames":["Hopkins"],"firstnames":["Philip","F."],"suffixes":[]},{"propositions":[],"lastnames":["Hayward"],"firstnames":["Christopher","C."],"suffixes":[]},{"propositions":[],"lastnames":["Ma"],"firstnames":["Xiangcheng"],"suffixes":[]},{"propositions":[],"lastnames":["Boylan-Kolchin"],"firstnames":["Michael"],"suffixes":[]},{"propositions":[],"lastnames":["Kasen"],"firstnames":["Daniel"],"suffixes":[]},{"propositions":[],"lastnames":["Kereš"],"firstnames":["Dušan"],"suffixes":[]},{"propositions":[],"lastnames":["Faucher-Giguère"],"firstnames":["Claude-Andrè"],"suffixes":[]},{"propositions":[],"lastnames":["Orr"],"firstnames":["Matthew","E."],"suffixes":[]}],"month":"December","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:1712.02795","bibtex":"@article{su_discrete_2017,\n\ttitle = {Discrete {Effects} in {Stellar} {Feedback}: {Individual} {Supernovae}, {Hypernovae}, and {IMF} {Sampling} in {Dwarf} {Galaxies}},\n\tvolume = {1712},\n\tshorttitle = {Discrete {Effects} in {Stellar} {Feedback}},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv171202795S},\n\tabstract = {Using high-resolution simulations from the FIRE-2 (Feedback In Realistic \nEnvironments) project, we study the effects of discreteness in stellar\nfeedback processes on the evolution of galaxies and the properties of\nthe interstellar medium (ISM). We specifically consider the\ndiscretization of supernovae (SNe), including hypernovae (HNe), and\nsampling the initial mass function (IMF). We study these processes in\ncosmological simulations of dwarf galaxies with \\$z=0\\$ stellar masses\n\\$M\\_\\{{\\textbackslash}ast\\}{\\textbackslash}sim 10{\\textasciicircum}\\{4\\}-3{\\textbackslash}times10{\\textasciicircum}\\{6\\}{\\textbackslash},M\\_{\\textbackslash}odot\\$ (halo masses \\${\\textbackslash}sim\n10{\\textasciicircum}\\{9\\}-10{\\textasciicircum}\\{10\\}{\\textbackslash},M\\_{\\textbackslash}odot\\$). We show that the discrete nature of\nindividual SNe (as opposed to a model in which their energy/momentum\ndeposition is continuous over time, similar to stellar winds) is crucial\nin generating a reasonable ISM structure and galactic winds and in\nregulating dwarf stellar masses. However, once SNe are discretized,\naccounting for the effects of IMF sampling on continuous mechanisms such\nas radiative feedback and stellar mass-loss (as opposed to adopting\nIMF-averaged rates) has weak effects on galaxy-scale properties. We also\nconsider the effects of rare HNe events with energies \\${\\textbackslash}sim\n10{\\textasciicircum}\\{53\\}{\\textbackslash},\\{{\\textbackslash}rm erg\\}\\$. 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