Show simple item record

dc.contributor.authorLombardi, James C. Jr
dc.contributor.authorHoltzman, William
dc.contributor.authorDooley, Katherine L.
dc.contributor.authorGearity, Kyle
dc.contributor.authorKalogera, Vicky
dc.contributor.authorRasio, Frederic A.
dc.date.accessioned2018-01-23T19:32:47Z
dc.date.available2018-01-23T19:32:47Z
dc.date.issued2011-08-20
dc.identifier.citationLombardi, J.C. Jr., Holtzman, W., Dooley, K.L., Gearity, K., Kalogera, V., and Rasio, F.A. (2011). Twin binaries: Studies of stability, mass transfer, and coalescence. The Astrophysical Journal 737(2): 1-16. doi: 10.1088/0004-637X/737/2/49.en_US
dc.identifier.issn0004-637X
dc.identifier.issne1538-4357
dc.identifier.urihttp://hdl.handle.net/10456/45501
dc.description.abstractMotivated by suggestions that binaries with almost equal-mass components (“twins”) play an important role in the formation of double neutron stars and may be rather abundant among binaries, we study the stability of synchronized close and contact binaries with identical components in circular orbits. In particular, we investigate the dependency of the innermost stable circular orbit on the core mass, and we study the coalescence of the binary that occurs at smaller separations. For twin binaries composed of convective main-sequence stars, subgiants, or giants with low-mass cores (Mc 0.15M, where M is the mass of a component), a secular instability is reached during the contact phase, accompanied by a dynamical mass transfer instability at the same or at a slightly smaller orbital separation. Binaries that come inside this instability limit transfer mass gradually from one component to the other and then coalesce quickly as mass is lost through the outer Lagrangian points. For twin giant binaries with moderate to massive cores (Mc 0.15M), we find that stable contact configurations exist at all separations down to the Roche limit, when mass shedding through the outer Lagrangian points triggers a coalescence of the envelopes and leaves the cores orbiting in a central tight binary. In addition to the formation of binary neutron stars, we also discuss the implications of our results for the production of planetary nebulae with double degenerate central binaries.en_US
dc.language.isoen_USen_US
dc.publisherInstitute of Physicsen_US
dc.relation.ispartofThe Astrophysical Journalen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637X/737/2/49en_US
dc.rightsThis article has been accepted for publication in Astrophysical Journal ©: 2011 Lombardi, J.C. Jr, Holtzman, W., Dooley, K.L., Gearity, K., Kalogera, V., Rasio, F. Published by Institute of Physics. All rights reserved.en_US
dc.subjectbinaries: closeen_US
dc.subjectbinaries: generalen_US
dc.subjecthydrodynamicsen_US
dc.subjectinstabilitiesen_US
dc.subjectmethods: numericalen_US
dc.subjectstars: generalen_US
dc.titleTwin Binaries: Studies of Stability, Mass Transfer, and Coalescenceen_US
dc.description.versionPublished articleen_US
dc.contributor.departmentPhysicsen_US
dc.citation.volume737en_US
dc.citation.issue2en_US
dc.citation.spage1en_US
dc.citation.epage16en_US
dc.identifier.doi10.1088/0004-637X/737/2/49.
dc.contributor.avlauthorLombardi, James C. Jr


Files in this item

Thumbnail
Thumbnail

This item appears in the following Collection(s)

Show simple item record