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dc.contributor.authorHatfull, Roger W. M.
dc.contributor.authorIvanova, Natalia
dc.contributor.authorLombardi, James C., Jr.
dc.date.accessioned2021-10-08T20:17:38Z
dc.date.available2021-10-08T20:17:38Z
dc.date.issued2021-07-27
dc.identifier.citationRoger W M Hatfull, Natalia Ivanova, James C Lombardi, Jr., Simulating a stellar contact binary merger – I. Stellar models, Monthly Notices of the Royal Astronomical Society, Volume 507, Issue 1, October 2021, Pages 385–397, https://doi.org/10.1093/mnras/stab2140en_US
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.urihttps://dspace.allegheny.edu/handle/10456/53960
dc.description.abstractWe study the initial conditions of a common envelope (CE) event resulting in a stellar merger. A merger’s dynamics could be understood through its light curve, but no synthetic light curve has yet been created for the full evolution. Using the smoothed particle hydrodynamics (SPH) code STARSMASHER, we have created three-dimensional (3D) models of a 1.52 M⊙ star that is a plausible donor in the V1309 Sco progenitor. The integrated total energy profiles of our 3D models match their initial one-dimensional (1D) models to within a 0.1 per cent difference in the top 0.1 M⊙ of their envelopes. We have introduced a new method for obtaining radiative flux by linking intrinsically optically thick SPH particles to a single stellar envelope solution from a set of unique solutions. For the first time, we calculated our 3D models’ effective temperatures to within a few per cent of the initial 1D models, and found a corresponding improvement in luminosity by a factor of ≳106 compared to ray tracing. We let our highest resolution 3D model undergo Roche lobe overflow with a 0.16 M⊙ point-mass accretor (P ≃ 1.6 d) and found a bolometric magnitude variability amplitude of ∼0.3 – comparable to that of the V1309 Sco progenitor. Our 3D models are, in the top 0.1 M⊙ of the envelope and in terms of total energy, the most accurate models so far of the V1309 Sco donor star. A dynamical simulation that uses the initial conditions we presented in this paper can be used to create the first ever synthetic CE evolution light curve.en_US
dc.language.isoen_USen_US
dc.publisherOxford University Pressen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.relation.isversionofhttps://academic.oup.com/mnras/article-abstract/507/1/385/6328494?redirectedFrom=fulltexten_US
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.en_US
dc.subjecthydrodynamicsen_US
dc.subjectradiative transferen_US
dc.subjectmethods: numericalen_US
dc.subjectstars: low-massen_US
dc.subject(stars:) binaries (including multiple): closeen_US
dc.titleSimulating a stellar contact binary merger – I. Stellar modelsen_US
dc.description.versionOriginal manuscript prior to peer review (preprint)en_US
dc.contributor.departmentPhysicsen_US
dc.citation.volume507en_US
dc.citation.issue1en_US
dc.citation.spage385en_US
dc.citation.epage397en_US
dc.identifier.doi10.1093/mnras/stab2140
dc.contributor.avlauthorLombardi, Jamie C., Jr.


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