A Grid of Core-Collapse Supernova Remnant Models I: The Effect of Wind-Driven Mass-Loss. (arXiv:2103.07980v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Jacovich_T/0/1/0/all/0/1">Taylor Jacovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patnaude_D/0/1/0/all/0/1">Daniel Patnaude</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slane_P/0/1/0/all/0/1">Pat Slane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badenes_C/0/1/0/all/0/1">Carles Badenes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_S/0/1/0/all/0/1">Shiu-Hang Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagataki_S/0/1/0/all/0/1">Shigehiro Nagataki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milisavljevic_D/0/1/0/all/0/1">Dan Milisavljevic</a>
Massive stars can shed material via steady, line-driven winds, eruptive
outflows, or mass-transfer onto a binary companion. In the case of single
stars, the mass is deposited by the stellar wind into the nearby environment.
After the massive star explodes, the stellar ejecta interact with this
circumstellar material (CSM), often-times resulting in bright X-ray line
emission from both the shock-heated CSM and ejecta. The amount of material lost
by the progenitor, the mass of ejecta, and its energetics all impact the bulk
spectral characteristics of this X-ray emission. Here we present a grid of
core-collapse supernova remnant models derived from models for massive stars
with zero age main sequence masses of $sim$ 10 – 30 M$_odot$ evolved from the
pre-main sequence stage with wind-driven mass-loss. Evolution is handled by a
multi-stage pipeline of software packages. First, we use mesa (Modules for
Experiments in Stellar Astrophysics) to evolve the progenitors from pre-main
sequence to iron core collapse. We then use the Supernova Explosion Code (snec)
to explode the mesa models, and follow them for the first 100 days following
core-collapse. Finally, we couple the snec output, along with the CSM generated
from mesa mass-loss rates, into the Cosmic-Ray Hydrodynamics code (ChN) to
model the remnant phase to 7000 years post core-collapse. At the end of each
stage, we compare our outputs with those found in the literature, and we
examine any qualitative and quantitative differences in the bulk properties of
the remnants and their spectra based on the initial progenitor mass, as well as
mass-loss history.
Massive stars can shed material via steady, line-driven winds, eruptive
outflows, or mass-transfer onto a binary companion. In the case of single
stars, the mass is deposited by the stellar wind into the nearby environment.
After the massive star explodes, the stellar ejecta interact with this
circumstellar material (CSM), often-times resulting in bright X-ray line
emission from both the shock-heated CSM and ejecta. The amount of material lost
by the progenitor, the mass of ejecta, and its energetics all impact the bulk
spectral characteristics of this X-ray emission. Here we present a grid of
core-collapse supernova remnant models derived from models for massive stars
with zero age main sequence masses of $sim$ 10 – 30 M$_odot$ evolved from the
pre-main sequence stage with wind-driven mass-loss. Evolution is handled by a
multi-stage pipeline of software packages. First, we use mesa (Modules for
Experiments in Stellar Astrophysics) to evolve the progenitors from pre-main
sequence to iron core collapse. We then use the Supernova Explosion Code (snec)
to explode the mesa models, and follow them for the first 100 days following
core-collapse. Finally, we couple the snec output, along with the CSM generated
from mesa mass-loss rates, into the Cosmic-Ray Hydrodynamics code (ChN) to
model the remnant phase to 7000 years post core-collapse. At the end of each
stage, we compare our outputs with those found in the literature, and we
examine any qualitative and quantitative differences in the bulk properties of
the remnants and their spectra based on the initial progenitor mass, as well as
mass-loss history.
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