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Post common envelope binary

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HD 101584 is a suspected post-common envelope binary. The engulfed red dwarf triggered an outflow of gas, creating the nebula seen by ALMA.
Key stages in a common envelope phase. Top: A star fills its Roche lobe. Middle: The companion is engulfed; the core and companion spiral towards one another inside a common envelope. Bottom: The envelope is ejected and forms a PCEB or the two stars merge.

A Post Common Envelope Binary, PCEB or pre-cataclysmic variable is a binary consisting of a white dwarf and a main-sequence star or a brown dwarf.[1] The star or brown dwarf shared a common envelope with the white dwarf progenitor in the red giant phase. In this scenario the star or brown dwarf loses angular momentum as it orbits within the envelope, eventually leaving a main-sequence star and white dwarf in a short-period orbit. A PCEB will continue to lose angular momentum via magnetic braking and gravitational waves and will eventually begin mass-transfer, resulting in a cataclysmic variable. While there are thousands of PCEBs known, there are only a few eclipsing PCEBs, also called ePCEBs.[2] Even more rare are PCEBs with a brown dwarf as the secondary.[1] A brown dwarf with a mass lower than 20 MJ might evaporate during the common envelope phase and therefore the secondary is supposed to have a mass higher than 20 MJ.[3]

The suspected PCEB HD 101584 is surrounded by an complex nebula. During the common envelope phase the red giant phase of the primary was terminated prematurely that ended avoiding a stellar merger. The remaining hydrogen envelope of HD 101584 was ejected during the interaction between the red giant and the red dwarf and it now forms a circumstellar medium around the binary.[4]

List of post common envelope binaries

Name Period Secondary Note
NN Serpentis 0.13 days red dwarf eclipsing binary
K 1-2 0.6758 days[5] planetary nebula
RR Caeli 7.2 hours red dwarf eclipsing binary
KOI-256 1.37865 days[2] red dwarf eclipsing binary
WD 0137−349 116 minutes brown dwarf first confirmed PCEB with a brown dwarf as a companion
WD 0837+185 4.2 hours[6] brown dwarf extreme mass ratio of the progenitor, with the primary having a mass of 3.5-3.7 M☉ and the secondary 25-30 MJ
SDSS 1557 2.27 hours[7] brown dwarf circumbinary debris disk with a polluted white dwarf
SDSS J1205-0242 71.2 minutes[8] low mass star or brown dwarf shortest period PCEB (as of 2017)
CSS21055 121.73 minutes[9] brown dwarf eclipsing binary
HD 101584 150-200 days[4] red dwarf the engulfment of the red dwarf probably triggered gas to outflow, creating the nebula, seen with Hubble and ALMA

See also

References

  1. ^ a b Casewell, S. L.; Braker, I. P.; Parsons, S. G.; Hermes, J. J.; Burleigh, M. R.; Belardi, C.; Chaushev, A.; Finch, N. L.; Roy, M.; Littlefair, S. P.; Goad, M. (2018-05-01). "The first sub-70 minute non-interacting WD-BD system: EPIC212235321". Monthly Notices of the Royal Astronomical Society. 476 (1): 1405–1411. arXiv:1801.07773. doi:10.1093/mnras/sty245. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  2. ^ a b Muirhead, Philip S.; Vanderburg, Andrew; Shporer, Avi; Becker, Juliette; Swift, Jonathan J.; Lloyd, James P.; Fuller, Jim; Zhao, Ming; Hinkley, Sasha; Pineda, J. Sebastian; Bottom, Michael (2013-04-02). "Characterizing the Cool KOIs. V. KOI-256: A Mutually Eclipsing Post-Common Envelope Binary". The Astrophysical Journal. 767 (2): 111. arXiv:1304.1165. Bibcode:2013ApJ...767..111M. doi:10.1088/0004-637X/767/2/111. ISSN 0004-637X.
  3. ^ information@eso.org. "A Sub-Stellar Jonah - Brown Dwarf Survives Being Swallowed". www.eso.org. Retrieved 2020-02-02.
  4. ^ a b Olofsson, H.; Khouri, T.; Maercker, M.; Bergman, P.; Doan, L.; Tafoya, D.; Vlemmings, W. H. T.; Humphreys, E. M. L.; Lindqvist, M.; Nyman, L.; Ramstedt, S. (March 2019). "HD 101584: circumstellar characteristics and evolutionary status". A&A. 623: A153. doi:10.1051/0004-6361/201834897. ISSN 0004-6361.
  5. ^ Ritter, H.; Kolb, U. (June 2003). "Catalogue of cataclysmic binaries, low-mass X-ray binaries and related objects (Seventh edition)". Astronomy & Astrophysics. 404: 301–303. arXiv:astro-ph/0301444. Bibcode:2003A&A...404..301R. doi:10.1051/0004-6361:20030330. ISSN 0004-6361.
  6. ^ Casewell, S. L.; Burleigh, M. R.; Wynn, G. A.; Alexander, R. D.; Napiwotzki, R.; Lawrie, K. A.; Dobbie, P. D.; Jameson, R. F.; Hodgkin, S. T. (November 2012). "WD0837+185: The Formation and Evolution of an Extreme Mass-ratio White-dwarf-Brown-dwarf Binary in Praesepe". ApJL. 759 (2): L34. Bibcode:2012ApJ...759L..34C. doi:10.1088/2041-8205/759/2/L34. ISSN 0004-637X.
  7. ^ Farihi, J.; Parsons, S. G.; Gänsicke, B. T. (March 2017). "A circumbinary debris disk in a polluted white dwarf system". NatAs. 1 (3): 0032. arXiv:1612.05259. Bibcode:2017NatAs...1E..32F. doi:10.1038/s41550-016-0032. ISSN 2397-3366.
  8. ^ Rappaport, S.; Vanderburg, A.; Nelson, L.; Gary, B. L.; Kaye, T. G.; Kalomeni, B.; Howell, S. B.; Thorstensen, J. R.; Lachapelle, F.-R.; Lundy, M.; St-Antoine, J. (October 2017). "WD 1202-024: the shortest-period pre-cataclysmic variable". MNRAS. 471 (1): 948–961. arXiv:1705.05863. Bibcode:2017MNRAS.471..948R. doi:10.1093/mnras/stx1611. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  9. ^ Beuermann, K.; Dreizler, S.; Hessman, F. V.; Backhaus, U.; Boesch, A.; Husser, T.-O.; Nortmann, L.; Schmelev, A.; Springer, R. (October 2013). "The eclipsing post-common envelope binary CSS21055: a white dwarf with a probable brown-dwarf companion". Astronomy & Astrophysics. 558: A96. arXiv:1312.5088. Bibcode:2013A&A...558A..96B. doi:10.1051/0004-6361/201322241. ISSN 0004-6361.
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