Explosions Driven by the Coalescence of a Compact Object with the Core of a Massive-star Companion inside a Common Envelope: Circumstellar Properties, Light Curves, and Population Statistics
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Explosions Driven by the Coalescence of a Compact Object with the Core of a Massive-star Companion inside a Common Envelope : Circumstellar Properties, Light Curves, and Population Statistics. / Schroder, Sophie Lund; MacLeod, Morgan; Loeb, Abraham; Vigna-Gomez, Alejandro; Mandel, Ilya.
In: Astrophysical Journal, Vol. 892, No. 1, 13, 20.03.2020.Research output: Contribution to journal › Journal article › peer-review
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TY - JOUR
T1 - Explosions Driven by the Coalescence of a Compact Object with the Core of a Massive-star Companion inside a Common Envelope
T2 - Circumstellar Properties, Light Curves, and Population Statistics
AU - Schroder, Sophie Lund
AU - MacLeod, Morgan
AU - Loeb, Abraham
AU - Vigna-Gomez, Alejandro
AU - Mandel, Ilya
PY - 2020/3/20
Y1 - 2020/3/20
N2 - We model explosions driven by the coalescence of a black hole or neutron star with the core of its massive-star companion. Upon entering a common-envelope phase, a compact object may spiral all the way to the core. The concurrent release of energy is likely to be deposited into the surrounding common envelope, powering a merger-driven explosion. We use hydrodynamic models of binary coalescence to model the common-envelope density distribution at the time of coalescence. We find toroidal profiles of material, concentrated in the binary's equatorial plane and extending to many times the massive star's original radius. We use the spherically averaged properties of this circumstellar material (CSM) to estimate the emergent light curves that result from the interaction between the blast wave and the CSM. We find that typical merger-driven explosions are brightened by up to three magnitudes by CSM interaction. From population synthesis models, we discover that the brightest merger-driven explosions, M-V similar to -18 to -20, are those involving black holes because they have the most massive and extended CSM. Black hole coalescence events are also common; they represent about 50% of all merger-driven explosions and approximately 0.25% of the core-collapse rate. Merger-driven explosions offer a window into the highly uncertain physics of common-envelope interactions in binary systems by probing the properties of systems that merge rather than eject their envelopes.
AB - We model explosions driven by the coalescence of a black hole or neutron star with the core of its massive-star companion. Upon entering a common-envelope phase, a compact object may spiral all the way to the core. The concurrent release of energy is likely to be deposited into the surrounding common envelope, powering a merger-driven explosion. We use hydrodynamic models of binary coalescence to model the common-envelope density distribution at the time of coalescence. We find toroidal profiles of material, concentrated in the binary's equatorial plane and extending to many times the massive star's original radius. We use the spherically averaged properties of this circumstellar material (CSM) to estimate the emergent light curves that result from the interaction between the blast wave and the CSM. We find that typical merger-driven explosions are brightened by up to three magnitudes by CSM interaction. From population synthesis models, we discover that the brightest merger-driven explosions, M-V similar to -18 to -20, are those involving black holes because they have the most massive and extended CSM. Black hole coalescence events are also common; they represent about 50% of all merger-driven explosions and approximately 0.25% of the core-collapse rate. Merger-driven explosions offer a window into the highly uncertain physics of common-envelope interactions in binary systems by probing the properties of systems that merge rather than eject their envelopes.
KW - Close binary stars
KW - Stellar evolution
KW - Astronomical simulations
KW - NEUTRON-STAR
KW - BLACK-HOLE
KW - HYPERCRITICAL ACCRETION
KW - SUPERNOVA EJECTA
KW - SHOCK BREAKOUT
KW - SN 2009IP
KW - EVOLUTION
KW - JETS
KW - MODEL
KW - MERGERS
U2 - 10.3847/1538-4357/ab7014
DO - 10.3847/1538-4357/ab7014
M3 - Journal article
VL - 892
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 13
ER -
ID: 247442338