Show simple item record

dc.contributor.authorKremer, Kyle
dc.contributor.authorLombardi, James C., Jr.
dc.contributor.authorLu, Wenbin
dc.contributor.authorPiro, Anthony L.
dc.contributor.authorRasio, Frederic A.
dc.date.accessioned2022-09-21T16:46:35Z
dc.date.available2022-09-21T16:46:35Z
dc.date.issued2022-07-01
dc.identifier.citationKyle Kremer et al 2022 ApJ 933 203en_US
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.otherArticle number: 203
dc.identifier.urihttps://dspace.allegheny.edu/handle/10456/55382
dc.description.abstractRecent analyses have shown that close encounters between stars and stellar black holes occur frequently in dense star clusters. Depending upon the distance at closest approach, these interactions can lead to dissipating encounters such as tidal captures and disruptions, or direct physical collisions, all of which may be accompanied by bright electromagnetic transients. In this study, we perform a wide range of hydrodynamic simulations of close encounters between black holes and main-sequence stars that collectively cover the parameter space of interest, and we identify and classify the various possible outcomes. In the case of nearly head-on collisions, the star is completely disrupted with roughly half of the stellar material becoming bound to the black hole. For more distant encounters near the classical tidal-disruption radius, the star is only partially disrupted on the first pericenter passage. Depending upon the interaction details, the partially disrupted stellar remnant may be tidally captured by the black hole or become unbound (in some cases, receiving a sufficiently large impulsive kick from asymmetric mass loss to be ejected from its host cluster). In the former case, the star will undergo additional pericenter passages before ultimately being disrupted fully. Based on the properties of the material bound to the black hole at the end of our simulations (in particular, the total bound mass and angular momentum), we comment upon the expected accretion process and associated electromagnetic signatures that are likely to result.en_US
dc.language.isoen_USen_US
dc.publisherIOP Publishing Ltden_US
dc.relation.ispartofAstrophysical Journalen_US
dc.relation.isversionofhttp://dx.doi.org/10.3847/1538-4357/ac714fen_US
dc.rightsOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en_US
dc.subjectAstrophysical black holesen_US
dc.subjectHydrodynamical simulationsen_US
dc.subjectTidal disruptionen_US
dc.subjectGlobular star clustersen_US
dc.subjectTransient sourcesen_US
dc.titleHydrodynamics of Collisions and Close Encounters between Stellar Black Holes and Main-sequence Starsen_US
dc.description.versionPublished articleen_US
dc.contributor.departmentPhysicsen_US
dc.citation.volume933en_US
dc.citation.issue2en_US
dc.identifier.doi10.3847/1538-4357/ac714f
dc.contributor.avlauthorLombardi, James C., Jr.


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record