Stellar Tidal Disruption Events with Abundances and Realistic Structures (STARS): Library of Fallback Rates. (arXiv:2007.10996v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Law_Smith_J/0/1/0/all/0/1">Jamie A.P. Law-Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coulter_D/0/1/0/all/0/1">David A. Coulter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guillochon_J/0/1/0/all/0/1">James Guillochon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mockler_B/0/1/0/all/0/1">Brenna Mockler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_Ruiz_E/0/1/0/all/0/1">Enrico Ramirez-Ruiz</a>
We present the STARS library, a grid of tidal disruption event (TDE)
simulations interpolated to provide the mass fallback rate ($dM/dt$) to the
black hole for a main-sequence star of any stellar mass, stellar age, and
impact parameter. We use a one-dimensional stellar evolution code to construct
stars with accurate stellar structures and chemical abundances, then perform
tidal disruption simulations in a three-dimensional adaptive-mesh hydrodynamics
code with a Helmholtz equation of state, in unprecedented resolution: from 131
to 524 cells across the diameter of the star. The interpolated library of
fallback rates is available on GitHub
(https://github.com/jamielaw-smith/STARS_library) and version 1.0.0 is archived
on Zenodo; one can query the library for any stellar mass, stellar age, and
impact parameter. We provide new fitting formulae for important disruption
quantities ($beta_{rm crit}, Delta M, dot M_{rm peak}, t_{rm peak},
n_infty$) as a function of stellar mass, stellar age, and impact parameter.
Each of these quantities vary significantly with stellar mass and stellar age,
but we are able to reduce all of our simulations to a single relationship that
depends only on stellar structure, characterized by a single parameter
$rho_c/barrho$, and impact parameter $beta$. We also find that, in general,
more centrally concentrated stars have steeper $dM/dt$ rise slopes and
shallower decay slopes. For the same $Delta M$, the $dM/dt$ shape varies
significantly with stellar mass, promising the potential determination of
stellar properties from the TDE light curve alone. The $dM/dt$ shape depends
strongly on stellar structure and to a certain extent stellar mass, meaning
that fitting TDEs using this library offers a better opportunity to determine
the nature of the disrupted star and the black hole.
We present the STARS library, a grid of tidal disruption event (TDE)
simulations interpolated to provide the mass fallback rate ($dM/dt$) to the
black hole for a main-sequence star of any stellar mass, stellar age, and
impact parameter. We use a one-dimensional stellar evolution code to construct
stars with accurate stellar structures and chemical abundances, then perform
tidal disruption simulations in a three-dimensional adaptive-mesh hydrodynamics
code with a Helmholtz equation of state, in unprecedented resolution: from 131
to 524 cells across the diameter of the star. The interpolated library of
fallback rates is available on GitHub
(https://github.com/jamielaw-smith/STARS_library) and version 1.0.0 is archived
on Zenodo; one can query the library for any stellar mass, stellar age, and
impact parameter. We provide new fitting formulae for important disruption
quantities ($beta_{rm crit}, Delta M, dot M_{rm peak}, t_{rm peak},
n_infty$) as a function of stellar mass, stellar age, and impact parameter.
Each of these quantities vary significantly with stellar mass and stellar age,
but we are able to reduce all of our simulations to a single relationship that
depends only on stellar structure, characterized by a single parameter
$rho_c/barrho$, and impact parameter $beta$. We also find that, in general,
more centrally concentrated stars have steeper $dM/dt$ rise slopes and
shallower decay slopes. For the same $Delta M$, the $dM/dt$ shape varies
significantly with stellar mass, promising the potential determination of
stellar properties from the TDE light curve alone. The $dM/dt$ shape depends
strongly on stellar structure and to a certain extent stellar mass, meaning
that fitting TDEs using this library offers a better opportunity to determine
the nature of the disrupted star and the black hole.
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