Stellar Tidal Disruption Events with Abundances and Realistic Structures (STARS): Library of Fallback Rates

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 star...

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Bibliographic Details
Published in:The Astrophysical journal 2020-12, Vol.905 (2), p.141
Main Authors: Law-Smith, Jamie A. P., Coulter, David A., Guillochon, James, Mockler, Brenna, Ramirez-Ruiz, Enrico
Format: Article
Language:English
Subjects:
Abundance
Active galaxies
Age
Astrophysics
Black hole physics
Computational fluid dynamics
Diameters
Disruption
Equations of state
Finite element method
Fluid flow
Galaxy nuclei
Gravitation
Helmholtz equations
Hydrodynamics
Libraries
Light curve
Main sequence stars
Parameters
Simulation
Slopes
Stellar age
Stellar evolution
Stellar mass
Stellar structure
Tidal disruption
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Summary: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 (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 ( ) as a function of stellar mass, stellar age, and impact parameter. Each of these quantities varies 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 , and impact parameter β. We also find that, in general, more centrally concentrated stars have steeper dM/dt rise slopes and shallower decay slopes. For the same ΔM, 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.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abc489