Monte Carlo radiative transfer for the nebular phase of Type Ia supernovae. (arXiv:1912.02214v1 [astro-ph.HE])

Monte Carlo radiative transfer for the nebular phase of Type Ia supernovae. (arXiv:1912.02214v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Shingles_L/0/1/0/all/0/1">L. J. Shingles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sim_S/0/1/0/all/0/1">S. A. Sim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kromer_M/0/1/0/all/0/1">M. Kromer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maguire_K/0/1/0/all/0/1">K. Maguire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulla_M/0/1/0/all/0/1">M. Bulla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_C/0/1/0/all/0/1">C. Collins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballance_C/0/1/0/all/0/1">C. P. Ballance</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michel_A/0/1/0/all/0/1">A. S. Michel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramsbottom_C/0/1/0/all/0/1">C. A. Ramsbottom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roepke_F/0/1/0/all/0/1">F. K. Roepke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seitenzahl_I/0/1/0/all/0/1">I. R. Seitenzahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tyndall_N/0/1/0/all/0/1">N. B. Tyndall</a>

We extend the range of validity of the ARTIS 3D radiative transfer code up to
hundreds of days after explosion, when Type Ia supernovae are in their nebular
phase. To achieve this, we add a non-local thermodynamic equilibrium (non-LTE)
population and ionisation solver, a new multi-frequency radiation field model,
and a new atomic dataset with forbidden transitions. We treat collisions with
non-thermal leptons resulting from nuclear decays to account for their
contribution to excitation, ionisation, and heating. We validate our method
with a variety of tests including comparing our synthetic nebular spectra for
the well-known one-dimensional W7 model with the results of other studies. As
an illustrative application of the code, we present synthetic nebular spectra
for the detonation of a sub-Chandrasekhar white dwarf in which the possible
effects of gravitational settling of Ne22 prior to explosion have been
explored. Specifically, we compare synthetic nebular spectra for a 1.06
M$_odot$ white dwarf model obtained when 5.5 Gyr of very-efficient settling is
assumed to a similar model without settling. We find that this degree of Ne22
settling has only a modest effect on the resulting nebular spectra due to
increased Ni58 abundance. Due to the high ionisation in sub-Chandrasekhar
models, the nebular [Ni II] emission remains negligible, while the [Ni III]
line strengths are increased and the overall ionisation balance is slightly
lowered in the model with Ne22 settling. In common with previous studies of
sub-Chandrasekhar models at nebular epochs, these models overproduce [Fe III]
emission relative to [Fe II] in comparison to observations of normal Type Ia
supernovae.

We extend the range of validity of the ARTIS 3D radiative transfer code up to
hundreds of days after explosion, when Type Ia supernovae are in their nebular
phase. To achieve this, we add a non-local thermodynamic equilibrium (non-LTE)
population and ionisation solver, a new multi-frequency radiation field model,
and a new atomic dataset with forbidden transitions. We treat collisions with
non-thermal leptons resulting from nuclear decays to account for their
contribution to excitation, ionisation, and heating. We validate our method
with a variety of tests including comparing our synthetic nebular spectra for
the well-known one-dimensional W7 model with the results of other studies. As
an illustrative application of the code, we present synthetic nebular spectra
for the detonation of a sub-Chandrasekhar white dwarf in which the possible
effects of gravitational settling of Ne22 prior to explosion have been
explored. Specifically, we compare synthetic nebular spectra for a 1.06
M$_odot$ white dwarf model obtained when 5.5 Gyr of very-efficient settling is
assumed to a similar model without settling. We find that this degree of Ne22
settling has only a modest effect on the resulting nebular spectra due to
increased Ni58 abundance. Due to the high ionisation in sub-Chandrasekhar
models, the nebular [Ni II] emission remains negligible, while the [Ni III]
line strengths are increased and the overall ionisation balance is slightly
lowered in the model with Ne22 settling. In common with previous studies of
sub-Chandrasekhar models at nebular epochs, these models overproduce [Fe III]
emission relative to [Fe II] in comparison to observations of normal Type Ia
supernovae.

http://arxiv.org/icons/sfx.gif

Comments are closed.