GP Comae Berenices

GP Comae Berenices

An ultraviolet band light curve for GP Comae Berenices, adapted from Smak (1975).[1] The error bar shown on the leftmost point applies to all points.
Observation data
Epoch J2000      Equinox J2000
Constellation Coma Berenices
Right ascension 13h 05m 42.401s[2]
Declination +18° 01′ 03.76″[2]
Apparent magnitude (V) 15.69[3]
Characteristics
Evolutionary stage White dwarf
Spectral type DBe[4]
Apparent magnitude (g) 15.929[2]
Variable type AM CVn
Astrometry
Proper motion (μ) RA: −344.92±0.06 mas/yr[2]
Dec.: 34.85±0.06 mas/yr[2]
Parallax (π)13.7306 ± 0.0452 mas[2]
Distance237.5 ± 0.8 ly
(72.8 ± 0.2 pc)
Details[5]
Mass0.59±0.09 M☉
Temperature14,800±500 K
Other designations
Gaia DR2 3938156295111047680, G 61-29, LTT 18284, WD 1303+18, 2MASS J13054243+1801039[6]
Database references
SIMBADdata

GP Comae Berenices, abbreviated to GP Com and also known as G 61-29, is a star system composed of a white dwarf orbited by a planetary mass object, likely the highly eroded core of another white dwarf star.[7] The white dwarf is slowly accreting material from its satellite at a rate of (3.5±0.5)×10−11 M☉/year and was proven[8] to be a low-activity AM CVn star.[7][5] The star system is showing signs of a high abundance of ionized nitrogen from the accretion disk around the primary.[9]

  1. ^ Cite error: The named reference Smak was invoked but never defined (see the help page).
  2. ^ a b c d e Cite error: The named reference EDR3 was invoked but never defined (see the help page).
  3. ^ Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ^ Burbidge, E. M.; Strittmatter, P. A. (1971), "G61 - 29, a Helium Emission-Line Star", The Astrophysical Journal, 170: L39, Bibcode:1971ApJ...170L..39B, doi:10.1086/180836
  5. ^ a b Sion, Edward M.; Linnell, Albert P.; Godon, Patrick; Ballouz, Ronald-Louis (2011), "THE HOT COMPONENTS OF AM CVN HELIUM CATACLYSMICS", The Astrophysical Journal, 741 (1): 63, arXiv:1108.1388, Bibcode:2011ApJ...741...63S, doi:10.1088/0004-637X/741/1/63, S2CID 119284962
  6. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Zhang2018 was invoked but never defined (see the help page).
  8. ^ Morales-Rueda, L.; Marsh, T. R.; Steeghs, D.; Unda-Sanzana, E.; Wood, J. H.; North, R. C. (2003), "New results on GP Com", Astronomy & Astrophysics, 405: 249–261, arXiv:astro-ph/0304265, Bibcode:2003A&A...405..249M, doi:10.1051/0004-6361:20030552, S2CID 119033361
  9. ^ Kupfer, T.; Steeghs, D.; Groot, P. J.; Marsh, T. R.; Nelemans, G.; Roelofs, G. H. A. (2016), "UVES and X-Shooter spectroscopy of the emission line AM CVN systems GP Com and V396 Hya", Monthly Notices of the Royal Astronomical Society, 457 (2): 1828, arXiv:1601.02841, Bibcode:2016MNRAS.457.1828K, doi:10.1093/mnras/stw126