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dc.contributor.authorPerets, Hagai B.
dc.contributor.authorLi, Zhuo
dc.contributor.authorLombardi, James C. Jr
dc.contributor.authorMilcarek, Stephen R. Jr
dc.date.accessioned2018-01-29T13:29:49Z
dc.date.available2018-01-29T13:29:49Z
dc.date.issued2016-05-27
dc.identifier.citationPerets, H.B., Li, Z., Lombardi, J.C. Jr., and Milcarek, S.R. Jr. (2016). Micro-tidal disruption events by stellar compact objects and the production of ultra-long GRBs. The Astrophysical Journal 823: 1-9. doi: 10.3847/0004-637X/823/2/113en_US
dc.identifier.issn0004-637X
dc.identifier.issne1538-4357
dc.identifier.urihttp://hdl.handle.net/10456/45568
dc.description.abstractWe explore full/partial tidal disruption events (TDEs) of stars/planets by stellar compact objects (black holes (BHs) or neutron stars (NSs)), which we term micro-TDEs. Disruption of a star/planet with mass M sstarf may lead to the formation of a debris disk around the BH/NS. Efficient accretion of a fraction $({f}_{\mathrm{acc}}=0.1$ of the debris may then give rise to bright, energetic, long ({10}^{3} –{10}^{4} s), X-ray/gamma-ray flares, with total energies of up to $({f}_{\mathrm{acc}}/0.1)\times {10}^{52}\;({M}_{\star }/0.6\;{M}_{\odot })$ erg, possibly resembling ultra-long gamma-ray bursts (GRBs)/X-ray flashes (XRFs). The energy of such flares depends on the poorly constrained accretion processes. Significantly fainter flares might be produced if most of the disk mass is blown away through strong outflows. We suggest three dynamical origins for such disruptions. In the first, a star/planet is tidally disrupted following a close random encounter with a BH/NS in a dense cluster. We estimate the BH (NS) micro-TDE rates from this scenario to be a few $\times {10}^{-6}$ (a few $\times {10}^{-7}$) ${{\rm{yr}}}^{-1}$ per Milky Way galaxy. Another scenario involves the interaction of wide companions due to perturbations by stars in the field, likely producing comparable but lower rates. Finally, a third scenario involves a BH/NS that gains a natal velocity kick at birth, leading to a close encounter with a binary companion and the tidal disruption of that companion. Such events could be associated with a supernova, or even with a preceding GRB/XRF event, and would likely occur hours to days after the prompt explosion; the rates of such events could be larger than those obtained from the other scenarios, depending on the preceding complex binary stellar evolution.en_US
dc.language.isoen_USen_US
dc.publisherInstitute of Physicsen_US
dc.relation.ispartofThe Astrophysical Journalen_US
dc.relation.isversionofhttp://dx.doi.org/10.3847/0004-637X/823/2/113en_US
dc.rightsThis article has been accepted for publication in The Astrophysical Journal ©: 2016 Hagai, Li, Lombardi, and Milcarek. Published by the Institute of Physics. All rights reserved.en_US
dc.subjectgamma-ray burst: generalen_US
dc.subjectgamma rays: starsen_US
dc.subjectstars: black holesen_US
dc.subjectstars: neutronen_US
dc.subjectX-rays: binariesen_US
dc.titleMicro-tidal disruption events by stellar compact objects and the production of ultra-long GRBsen_US
dc.description.versionPublished articleen_US
dc.contributor.departmentPhysicsen_US
dc.citation.volume823en_US
dc.citation.spage1en_US
dc.citation.epage9en_US
dc.identifier.doi10.3847/0004-637X/823/2/113
dc.contributor.avlauthorLombardi, James C. Jr


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