Model Light Curves for Type Ib and Ic Supernovae. (arXiv:2009.06868v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Woosley_S/0/1/0/all/0/1">Stan Woosley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sukhbold_T/0/1/0/all/0/1">Tuguldur Sukhbold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasen_D/0/1/0/all/0/1">Daniel Kasen</a>
Using the Monte Carlo code, SEDONA, multiband photometry and spectra are
calculated for supernovae derived from stripped helium stars with presupernova
masses from 2.2 to 10.0 $M_odot$. The models are representative of evolution
in close binaries and have previously been exploded using a parametrized
one-dimensional model for neutrino-transport. A subset, those with presupernova
masses in the range 2.2 – 5.6 $M_odot$, have many properties in common with
observed Type Ib and Ic supernovae, including a median ejected mass near 2
$M_odot$, explosion energies near $1 times 10^{51}$ erg, typical $^{56}$Ni
masses 0.07 – 0.09 $M_odot$, peak times of about 20 days, and a narrow range
for the $V$-$R$ color index 10 days post $V$-maximum near 0.3 mag. The median
peak bolometric luminosity, near 10$^{42.3}$ erg s$^{-1}$, is fainter, however,
than for several observational tabulations and the brightest explosion has a
bolometric luminosity of only 10$^{42.50}$ erg s$^{-1}$. The brightest absolute
$B$, $V$, and $R$ magnitudes at peak are $-17.2$, $-17.8$, and $-18.0$. These
limits are fainter than some allegedly typical Type Ib and Ic supernovae and
could reflect problems in our models or the observational analysis. Helium
stars with lower and higher masses also produce interesting transients that may
have been observed including fast, faint, blue transients and long, red, faint
Type Ic supernovae. New models are specifically presented for SN 2007Y, SN
2007gr, SN 2009jf, LSQ13abf, SN 2008D, and SN 2010X.
Using the Monte Carlo code, SEDONA, multiband photometry and spectra are
calculated for supernovae derived from stripped helium stars with presupernova
masses from 2.2 to 10.0 $M_odot$. The models are representative of evolution
in close binaries and have previously been exploded using a parametrized
one-dimensional model for neutrino-transport. A subset, those with presupernova
masses in the range 2.2 – 5.6 $M_odot$, have many properties in common with
observed Type Ib and Ic supernovae, including a median ejected mass near 2
$M_odot$, explosion energies near $1 times 10^{51}$ erg, typical $^{56}$Ni
masses 0.07 – 0.09 $M_odot$, peak times of about 20 days, and a narrow range
for the $V$-$R$ color index 10 days post $V$-maximum near 0.3 mag. The median
peak bolometric luminosity, near 10$^{42.3}$ erg s$^{-1}$, is fainter, however,
than for several observational tabulations and the brightest explosion has a
bolometric luminosity of only 10$^{42.50}$ erg s$^{-1}$. The brightest absolute
$B$, $V$, and $R$ magnitudes at peak are $-17.2$, $-17.8$, and $-18.0$. These
limits are fainter than some allegedly typical Type Ib and Ic supernovae and
could reflect problems in our models or the observational analysis. Helium
stars with lower and higher masses also produce interesting transients that may
have been observed including fast, faint, blue transients and long, red, faint
Type Ic supernovae. New models are specifically presented for SN 2007Y, SN
2007gr, SN 2009jf, LSQ13abf, SN 2008D, and SN 2010X.
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