CP Puppis

CP Puppis (or Nova Puppis 1942) was a bright nova occurring in the constellation Puppis in 1942. From a 17th magnitude star, it reached an apparent visual magnitude of –0.2 then began a rapid decline. It had dropped by three magnitudes in an interval of 6.5 days, one of the sharpest declines ever noted for a nova. About 14 years later, the shell ejected by the nova event was detected, which allowed the distance to be computed. In 2000, this distance was revised to 3,720 light-years (1,140 parsecs) after correcting for probable errors.[5] The Gaia spacecraft later measured the parallax of the star leading to an accurate distance of 815+15
−14 parsecs.[1][2]

CP Puppis
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension  08h 11m 46.0635s[1]
Declination −35° 21′ 04.9863″[1]
Apparent magnitude (V) 0.7 Max.
18 Min.[2]
Characteristics
Variable type Nova[2]
Astrometry
Radial velocity (Rv)+37[3] km/s
Proper motion (μ) RA: −1.761±0.034[1] mas/yr
Dec.: 2.432±0.037[1] mas/yr
Parallax (π)1.2298 ± 0.0211[1] mas
Distance814+14
−15[2] pc
Other designations
Nova Puppis 1942, AAVSO 0808-35, Gaia DR2 5544760551021856000, 2MASS J08114606-3521049[4]
Database references
SIMBADdata

The nova outburst can be explained by a white dwarf that is accreting matter from a companion; most likely a low-mass main sequence star. This close binary system has an orbital period of 1.47 hours, which is one of the shortest periods of the known classical nova. Unusually, the white dwarf may have a magnetic field. Other properties of the system remain uncertain, although observations of X-ray emission from the system suggest that the white dwarf has a mass of more than 1.1 times the mass of the Sun.[5]

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Schaefer, Bradley E. (2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society. 481 (3): 3033–3051. arXiv:1809.00180. Bibcode:2018MNRAS.481.3033S. doi:10.1093/mnras/sty2388.
  3. Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
  4. "CP Puppis". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-31.
  5. Orio, M.; et al. (January 2009), "New X-Ray Observations of the Old Nova CP Puppis and of the More Recent Nova V351 Puppis", The Astrophysical Journal, 690 (2): 1753–1763, arXiv:0809.3992, Bibcode:2009ApJ...690.1753O, doi:10.1088/0004-637X/690/2/1753
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