Astronomy:KPD 1930+2752
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 32m 14.81s[2] |
| Declination | +27° 58′ 35.5″[2] |
| Apparent magnitude (V) | 13.82[2] |
| Characteristics | |
| Spectral type | sdB+D? |
| Astrometry | |
| Radial velocity (Rv) | 5 km/s |
| Proper motion (μ) | RA: 1.744 mas/yr Dec.: -0.499 mas/yr |
| Parallax (π) | 1.1411 ± 0.0492[3] mas |
| Distance | 2,900 ± 100 ly (880 ± 40 pc) |
| Orbit[4] | |
| Primary | KPD 1930+2752 |
| Companion | KPD 1930+2752 B |
| Period (P) | 136 min. |
| Details[5] | |
| KPD 1930+2752 | |
| Mass | 0.5 M☉ |
| KPD 1930+2752 B | |
| Mass | 0.97±0.01 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | 1930+2752 data |
KPD 1930+2752 is a binary star system including a subdwarf B star and a probable white dwarf with relatively high mass.[6] Due to the nature of this astronomical system, it seems like a likely candidate for a potential type Ia supernova, a type of supernova which occurs when a white dwarf star takes on enough matter to approach the Chandrasekhar limit, the point at which electron degeneracy pressure would not be enough to support its mass. However, carbon fusion would occur before this limit was reached, releasing enough energy to overcome the force of gravity holding the star together and resulting in a supernova.
The total mass of the binary star system slightly exceeds the Chandrasekhar limit, making this system a candidate as a progenitor for a future type Ia supernova, although future mass loss is likely to reduce system mass below threshold.[7]
See also
- IK Pegasi, the nearest supernova progenitor candidate
References
- ↑ Billéres, M.; Fontaine, G.; Brassard, P.; Charpinet, S.; Liebert, James; Saffer, R. A. (February 2000). "Detection of p-Mode Pulsations and Possible Ellipsoidal Luminosity Variations in the Hot Subdwarf B Star KPD 1930+2752". The Astrophysical Journal 530 (1): 441–453. doi:10.1086/308369. Bibcode: 2000ApJ...530..441B.
- ↑ 2.0 2.1 2.2 "KPD 1930+2752". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=KPD+1930%2B2752.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Kupfer, Thomas et al. (2020), "The First Ultracompact Roche Lobe–Filling Hot Subdwarf Binary", The Astrophysical Journal 891 (1): 45, doi:10.3847/1538-4357/ab72ff, Bibcode: 2020ApJ...891...45K
- ↑ Neunteufel, P.; Yoon, S.-C.; Langer, N. (2019), "Evolution of helium star plus carbon-oxygen white dwarf binary systems and implications for diverse stellar transients and hypervelocity stars", Astronomy & Astrophysics 627: A14, doi:10.1051/0004-6361/201935322, Bibcode: 2019A&A...627A..14N
- ↑ Geier, S.; Nesslinger, S.; Heber, U.; Przybilla, N.; Napiwotzki, R.; Kudritzki, R.-P. (2007). "The hot subdwarf B + white dwarf binary KPD 1930+2752. A supernova type Ia progenitor candidate". Astronomy and Astrophysics 464 (1): 299–307. doi:10.1051/0004-6361:20066098. Bibcode: 2007A&A...464..299G.
- ↑ Is KPD 1930+2752 a good candidate type Ia supernova progenitor?
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