Post common envelope binary

A post-common envelope binary (PCEB) or pre-cataclysmic variable is a binary system consisting of a white dwarf or hot subdwarf 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]

HD 101584 is a suspected post-common envelope binary. The engulfed companion 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.

The material ejected from the common envelope forms a planetary nebula. One in five planetary nebulae are ejected from common envelopes, but this might be an underestimate. A planetary nebula formed by a common envelope system usually shows a bipolar structure.[4]

The suspected PCEB HD 101584 is surrounded by a complex nebula. During the common envelope phase the red giant phase of the primary was terminated prematurely, avoiding a stellar merger. The remaining hydrogen envelope of HD 101584 was ejected during the interaction between the red giant and the companion and it now forms the circumstellar medium around the binary.[5]

Many eclipsing post-common envelope binaries show variations in the timing of eclipses, the cause of which is uncertain. While orbiting exoplanets are often proposed as the cause of these variations, planetary models often fail to predict subsequent changes in eclipse timing. Other proposed causes, such as the Applegate mechanism, often cannot fully explain the observed eclipse timing variations either.[6]

List of post-common envelope binaries

Sorted by increasing orbital period.

Name Period Secondary Note
SDSS J1205-0242 71.2 minutes[7] low-mass star or brown dwarf shortest period PCEB (as of 2017)
WD 0137−349 116 minutes brown dwarf first confirmed PCEB with a brown dwarf as a companion
CSS21055 121.73 minutes[8] brown dwarf eclipsing binary
SDSS 1557 2.27 hours[9] brown dwarf circumbinary debris disk with a polluted white dwarf
V470 Camelopardalis
(HS0705+6700)		 2.3 hours[6] red dwarf eclipsing binary
NY Virginis 2.4 hours[6] red dwarf eclipsing binary
NSVS 14256825 2.6 hours[6] red dwarf eclipsing binary
HW Virginis 2.8 hours[6] red dwarf eclipsing binary
NN Serpentis 3.12 hours[6] red dwarf eclipsing binary
WD 0837+185 4.2 hours[10] 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
RR Caeli 7.3 hours[6] red dwarf eclipsing binary
DE Canum Venaticorum 8.7 hours[6] red dwarf eclipsing binary
central source of Hen 2-11 14.616 hours[11] K-type main sequence star planetary nebula and eclipsing binary
K 1-2 16.2192 hours[12] planetary nebula
central source of Fleming 1 1.1953 days[13] white dwarf planetary nebula
KOI-256 1.37865 days[2] red dwarf eclipsing binary
central source of NGC 2392 1.9 days[14] hot white dwarf planetary nebula and x-ray binary
central source of NGC 5189 4.04 days[15] massive white dwarf planetary nebula; primary is a low-mass Wolf-Rayet star
central source of NGC 2346 16 days[16] >3.5 M☉ sub-giant planetary nebula; one of the longest period PCEB which could host the most massive secondary
HD 101584 150–200 days[5] red dwarf or white dwarf the engulfment of the companion probably triggered gas to outflow, creating the nebula, seen with Hubble and ALMA; primary is a post-RGB star

See also

References
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  2. 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. S2CID 30368826.
  3. "A Sub-Stellar Jonah – Brown Dwarf Survives Being Swallowed". www.eso.org. Retrieved 2020-02-02.
  4. De Marco, Orsola; Reichardt, T.; Iaconi, R.; Hillwig, T.; Jacoby, G. H.; Keller, D.; Izzard, R. G.; Nordhaus, J.; Blackman, E. G. (October 2017). "Post-common envelope PN, fundamental or irrelevant?". Proceedings of the International Astronomical Union. 323: 213–217. arXiv:1612.03515. Bibcode:2017IAUS..323..213D. doi:10.1017/S1743921317002149. ISSN 1743-9221. S2CID 119069917.
  5. 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". Astronomy & Astrophysics. 623: A153. arXiv:1902.02153. Bibcode:2019A&A...623A.153O. doi:10.1051/0004-6361/201834897. ISSN 0004-6361. S2CID 102480818.
  6. Pulley, D.; Sharp, I. D.; Mallett, J.; von Harrach, S. (August 2022). "Eclipse timing variations in post-common envelope binaries: Are they a reliable indicator of circumbinary companions?". Monthly Notices of the Royal Astronomical Society. 514 (4): 5725–5738. arXiv:2206.06919. Bibcode:2022MNRAS.514.5725P. doi:10.1093/mnras/stac1676.
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  14. Miszalski, Brent; Manick, Rajeev; Van Winckel, Hans; Escorza, Ana (May 2019). "The post-common-envelope X-ray binary nucleus of the planetary nebula NGC 2392". Publications of the Astronomical Society of Australia. 36: e018. arXiv:1903.07264. Bibcode:2019PASA...36...18M. doi:10.1017/pasa.2019.11. ISSN 1323-3580. S2CID 119400616.
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