Hen 2-428
| Emission nebula | |
|---|---|
| Planetary nebula | |
 ESO image of Hen 2-428 | |
| Observation data: J2000.0[1] epoch | |
| Right ascension | 19h 13m 05.239s[1] |
| Declination | +15° 46′ 39.80″[1] |
| Constellation | Aquila |
| Designations | Henize 2-428, Hen 2-428,[1] He 2-428, PN G049.4+02.4,[1] M 4-12,[1] ARO 186,[1] PK 49+02 1,[1] IRAS 19108+1541[1] |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 13m 05.239s[1] |
| Declination | +15° 46′ 39.80″[1] |
| Spectral type | D |
| Other designations | |
| Database references | |
| SIMBAD | data |
Hen 2-428 is a planetary nebula with a binary double white dwarf system core. This core star system is the first discovered candidate for Type Ia supernova through binary white dwarf merger process. At the time of its discovery, the star system at the core was the heaviest known double white dwarf binary star system.
Planetary nebula[edit]
The planetary nebula is asymmetric, which is the result of there being not a single star, but a binary system at the heart of the nebula.[2][3][4][5]
Binary double white dwarf[edit]
The binary nature of the star at the centre of the nebula was discovered in 2014, when a study of why the nebula was not regular was conducted, resolving the previously thought single star into a double star. The two white dwarf stars forming the binary star system at the heart of the nebula orbit each other with a period of about 4 hours. The two stars have a combined mass of about 1.8 solar masses, with each star being slightly less massive than the Sun. As of 2015, they are the most massive binary double white dwarf star system known.[2][3][4][5]
Progenitor system for potential Type-Ia supernova[edit]
The pair are expected to merge into a single star in about 700 million years, whereupon they will explode in a Type Ia supernova. The inspiralling of the stars is caused by the emission of gravitational waves, resulting in the loss of orbital energy. The explosion is due to the combined mass of the merged star exceeding the Chandrasekhar limit of 1.4 solar masses. This is the first candidate for binary double white dwarf star merger progenitor Type Ia supernova star system known. The system is important to astrophysicists as Type Ia supernovae are used as standard candles to measure the distance to faraway objects, thus understanding the process is important to regularize and quantify the variations in the standard candle to reduce the error uncertainty in determining distance.[2][3][4][5][6]
Further reading[edit]
- M. Santander-Garcıa; P. Rodrıguez-Gil; R. L. M. Corradi; D. Jones; B. Miszalski; H. M. J. Boffin; M. M. Rubio-Dıez; M. M. Kotze (2 September 2014). "The double-degenerate, super-Chandrasekhar nucleus of the planetary nebula Henize 2-428" (PDF). Nature. 519 (7541) (published 9 February 2015): 63–65. arXiv:1609.00178. Bibcode:2015Natur.519...63S. doi:10.1038/nature14124. PMID 25686608. S2CID 4407536.
References[edit]
- ^ a b c d e f g h i j k l m "PN M 4-12 -- Planetary Nebula". SIMBAD. Hen 2-428. Retrieved 12 February 2015.
- ^ a b c Calla Cofield (11 February 2015). "Doomed White Dwarf Stars to Spawn Supernova in Colossal Crash". SPACE.com.
- ^ a b c "Two White Dwarf Stars At Center Of Planetary Nebula Henize-2-428 Will Explode Into Supernova". Tech Times. 10 February 2015.
- ^ a b c "First pair of merging stars destined to become a supernova found". Astronomy Now. 10 February 2015.
- ^ a b c "Stellar partnership doomed to end in catastrophe". Science Daily. 9 February 2015.
- ^ Miguel Santander-García (9 February 2015). "Dying with style: merging white dwarfs can do it too". Mapping Ignorance.
See also[edit]
- All double-degenerate binary stars known in 2015