A Physical Basis for the H-band Blue-edge Velocity and Light-Curve Shape Correlation in Context of Type Ia Supernova Explosion Physics. (arXiv:1904.01633v1 [astro-ph.HE])

A Physical Basis for the H-band Blue-edge Velocity and Light-Curve Shape Correlation in Context of Type Ia Supernova Explosion Physics. (arXiv:1904.01633v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ashall_C/0/1/0/all/0/1">C. Ashall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoeflich_P/0/1/0/all/0/1">P. Hoeflich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsiao_E/0/1/0/all/0/1">E. Y. Hsiao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Phillips_M/0/1/0/all/0/1">M. M. Phillips</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stritzinger_M/0/1/0/all/0/1">M. Stritzinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baron_E/0/1/0/all/0/1">E. Baron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_A/0/1/0/all/0/1">A. L. Piro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burns_C/0/1/0/all/0/1">C. Burns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_C/0/1/0/all/0/1">C. Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_S/0/1/0/all/0/1">S. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holmbo_S/0/1/0/all/0/1">S. Holmbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirshner_R/0/1/0/all/0/1">R. P. Kirshner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krisciunas_K/0/1/0/all/0/1">K. Krisciunas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marion_G/0/1/0/all/0/1">G. H. Marion</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morrell_N/0/1/0/all/0/1">N. Morrell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sand_D/0/1/0/all/0/1">D. J. Sand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shahbandeh_M/0/1/0/all/0/1">M. Shahbandeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suntzeff_N/0/1/0/all/0/1">N. B. Suntzeff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taddia_F/0/1/0/all/0/1">F. Taddia</a>

Our recent work demonstrates a correlation between the high-velocity blue
edge, $v_{edge}$, of the iron-peak Fe/Co/Ni $H$-band emission feature and the
optical light curve shape of normal, transitional and sub-luminous type Ia
Supernovae (SNe Ia). We explain this correlation in terms of SN Ia physics.
$v_{edge}$ corresponds to the sharp transition between the complete and
incomplete silicon burning regions in the ejecta. It measures the point in
velocity space where the outer $^{56}$Ni mass fraction, $X_{rm{Ni}}$, falls to
the order of 0.03-0.10. For a given $^{56}$Ni mass, $M(^{56}Ni)$, $v_{edge}$ is
sensitive to the specific kinetic energy $E_{rm kin}$($M(^{56}Ni)/M_{WD}$) of
the corresponding region. Combining $v_{edge}$ with light curve parameters
(i.e., s$_{BV}$, $Delta m_{15,s}$ in $B$ and $V$) allows us to distinguish
between explosion scenarios. The correlation between $v_{edge}$ and light-curve
shape is consistent with explosion models near the Chandrasekhar limit.
However, the available sub-$M_{Ch}$ WD explosion model based on SN 1999by
exhibits velocities which are too large to explain the observations. Finally,
the sub-luminous SN 2015bo exhibits signatures of a dynamical merger of two WDs
demonstrating diversity among explosion scenarios at the faint end of the SNe
Ia population.

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