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dc.contributor.authorWen, Sixiang
dc.contributor.authorJonker, Peter G.
dc.contributor.authorStone, Nicholas C.
dc.contributor.authorZabludoff, Ann I.
dc.contributor.authorPsaltis, Dimitrios
dc.date.accessioned2020-12-17T02:57:02Z
dc.date.available2020-12-17T02:57:02Z
dc.date.issued2020-07-06
dc.identifier.citationWen, S., Jonker, P. G., Stone, N. C., Zabludoff, A. I., & Psaltis, D. (2020). Continuum-Fitting the X-ray Spectra of Tidal Disruption Events. The Astrophysical Journal, 897, 80.en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab9817
dc.identifier.urihttp://hdl.handle.net/10150/649323
dc.description.abstractWe develop a new model for X-ray emission from tidal disruption events (TDEs), applying stationary general relativistic "slim disk" accretion solutions to supermassive black holes (SMBHs) and then ray-tracing the photon trajectories from the image plane to the disk surface, including gravitational redshift, Doppler, and lensing effects self-consistently. We simultaneously and successfully fit the multi-epoch XMM-Newton X-ray spectra for two TDEs: ASASSN-14li and ASASSN-15oi. We test explanations for the observed, unexpectedly slow X-ray brightening of ASASSN-15oi, including delayed disk formation and variable obscuration by a reprocessing layer. We propose a new mechanism that better fits the data: a "slimming disk" scenario in which accretion onto an edgeon disk slows, reducing the disk height and exposing more X-rays from the inner disk to the sightline over time. For ASASSN-15oi, we constrain the SMBH mass to 4.0(-3.1)(+2.5) x 10(6)M(circle dot). For ASASSN-14li, the SMBH mass is 10(-7)(+1) x 10(6) M-circle dot, and the spin is >0.3. For both TDEs, our fitted masses are consistent with independent estimates; for ASASSN-14li, application of the external mass constraint narrows our spin constraint to >0.85. The mass accretion rate of ASASSN-14li decays slowly, as proportional to t(-1.1), perhaps due to inefficient debris circularization. Over approximate to 1100 days, its SMBH has accreted Delta M approximate to 0.17M(circle dot), implying a progenitor star mass of >0.34M(circle dot), i.e., no "missing energy problem." For both TDEs, the hydrogen column density declines to the host galaxy plus Milky Way value after a few hundred days, suggesting a characteristic timescale for the depletion or removal of obscuring gas.en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rights© 2020. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://iopscience.iop.org/info/page/text-and-data-miningen_US
dc.subjectTidal disruptionen_US
dc.subjectX-ray transient sourcesen_US
dc.subjectAccretionen_US
dc.subjectBlack hole physicsen_US
dc.subjectSupermassive black holesen_US
dc.titleContinuum-fitting the X-Ray Spectra of Tidal Disruption Eventsen_US
dc.typeArticleen_US
dc.identifier.eissn1538-4357
dc.contributor.departmentUniv Arizonaen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume897
dc.source.issue1
dc.source.beginpage80
refterms.dateFOA2020-12-17T02:57:17Z


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