• Login
    View Item 
    •   DSpace Home
    • Faculty Scholarship
    • Faculty Scholarship and Open Access Collection
    • View Item
    •   DSpace Home
    • Faculty Scholarship
    • Faculty Scholarship and Open Access Collection
    • View Item
    JavaScript is disabled for your browser. Some features of this site may not work without it.

    Browse

    All of DSpaceCommunities & CollectionsAuthorFirst ReaderOther ReaderTitleSubjectDateThis CollectionAuthorFirst ReaderOther ReaderTitleSubjectDate

    My Account

    Login

    V1309 Sco: Understanding a merger

    • File:Lombardi 2014 Astro39.pdf
      Description:Published Article
      Show File
      MIME type:application/pdf
      File Size:6.010Mb

      Lombardi 2014 Astro39.pdf

      View/Open
    Date
    2014-05-01
    Author
    Nandez, J. L. A.
    Ivanova, N.
    Lombardi, James C. Jr
    Thumbnail
    View/Open
    Published Article (6.010Mb)

    Metadata
    Show full item record
    URI
    http://hdl.handle.net/10456/37034
    Subject
     binaries: close; hydrodynamics; stars: individual: V1309 Sco; stars: kinematics and dynamics; stars: rotation 
    Abstract
    One of the two outcomes of a common envelope (CE) event is a merger of the two stars. To date, the best known case of a binary merger is the V1309 Sco outburst, where the orbital period was known and observed to decay up to the outburst. Using the hydrodynamical code StarSmasher, we study in detail which characteristics of the progenitor binary affect the outburst and produce the best match with observations. We have developed a set of tools in order to quantify any CE event. We consider binaries consisting of a 1.52M(circle dot) giant and a 0.16M(circle dot) companion with P-orb similar to 1.4 days, varying the nature of the companion and its synchronization. We show that all considered progenitor binaries evolve toward the merger primarily because of Darwin instability. The merger is accompanied by mass ejection that proceeds in several separate mass outbursts and takes away a few percent of the donor mass. This very small mass, nonetheless, is important as it is not only sufficient to explain the observed light curve, but it also carries away up to one-third of both the initial total angular momentum and initial orbital energy. We find that all synchronized systems experience L-2 mass loss that operates during just a few days prior to the merger and produces ring-shaped ejecta. The formed star is always a strongly heated radiative star that differentially rotates. We conclude that the case of a synchronized binary with a main-sequence companion gives the best match with observations of V1309 Sco.
    Collections
    • Faculty Scholarship and Open Access Collection
    Department
    Physics
    Rights
    Copyright, 2014. The American Astronomical Society. All rights reserved.
    Citation
    Nandez, J. L. A., N. Ivanova, and J. C. Lombardi Jr. 2014. "V1309 Sco: Understanding a merger." Astrophysical Journal 786, no. 1 (May 1): 39.
    Version
    Published article
    Published As
    http://iopscience.iop.org/0004-637X/786/1/39/
    Journal
    Astrophysical Journal
    Publisher
    IOP
    DSpace software Copyright © 2015  Duraspace
    Contact Us | Send Feedback