WD 1054–226
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Crater |
| Right ascension | 10h 56m 38.63s |
| Declination | −22° 52′ 56.08″ |
| Apparent magnitude (V) | 16.0 |
| Characteristics | |
| Evolutionary stage | white dwarf |
| Spectral type | DAZ[1] |
| Astrometry | |
| Proper motion (μ) | RA: -78.865 ±0.047 mas/yr[2] Dec.: 298.019 ±0.051 mas/yr[2] |
| Parallax (π) | 27.6511 ± 0.0511 mas[2] |
| Distance | 118.0 ± 0.2 ly (36.16 ± 0.07 pc) |
| Details[1] | |
| Mass | 0.62 ±0.05 M☉ |
| Radius | 0.012 ±0.001 R☉ |
| Surface gravity (log g) | -3.27 ±0.09 cgs |
| Temperature | 7910 ±120 K |
| Age | cooling age: 1.3 ±0.2 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
WD 1054–226, also known as LP 849-31, is a relatively cool magnitude 16 white dwarf star with a hydrogen atmosphere, in the small southern constellation of Crater[3] located approximately 117 light years away at right ascension 10h57' and declination −22°53' (J2000 epoch). The name WD 1054–226 is based on the coordinates in the J1950 epoch. The star was recognized as a white dwarf along with 32 other nearby white dwarfs (or double white dwarfs) in 2007.[4]
In 2022 it was reported that the flux of light coming from the star varies continually due to partial obscuring by a ring. The pattern of variation repeats with little change every 25.02 hours. There are dips in the light flux every 23 minutes, exactly 65 per period of 25.02 hours. The explanation of this strong 65th harmonic is unknown and the authors of the paper say that the phenomenon is puzzling. It seems to be caused by clumps of matter orbiting the star.[5][1] The researchers have hypothesized that the clumps are being influenced by a moon-sized object, possibly an exoplanet. If it has a period of 25 hours then it is orbiting in the habitable zone of the system. If this is confirmed, it would be the first time that a planet has been found orbiting in the habitable zone of a white dwarf.[5][6]
See also
[edit]- List of exoplanets and planetary debris around white dwarfs
- WD 1145+017 is the first white dwarf with transiting debris discovered
References
[edit]- ^ a b c d Farihi, J. (April 2022). "Relentless and complex transits from a planetesimal debris disc". Monthly Notices of the Royal Astronomical Society. 511 (2): 1647–1666. arXiv:2109.06183. Bibcode:2022MNRAS.511.1647F. doi:10.1093/mnras/stab3475. hdl:10023/24937.
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Staff, News (2022-02-11). "Astronomers Find Planetary Bodies in Habitable Zone of White Dwarf | Sci.News". Sci.News: Breaking Science News. Retrieved 2024-01-29.
- ^ John Subasavage; et al. (May 23, 2007). "The Solar Neighborhood. XIX. Discovery and Characterization of 33 New Nearby White Dwarf Systems". The Astronomical Journal. 134: 252–261. arXiv:0704.0894. Bibcode:2007AJ....134..252S. doi:10.1086/518739.
- ^ a b "Planetary bodies observed in habitable zone of dead star". February 9, 2022. Retrieved February 11, 2022.
- ^ "Debris in dead star's Goldilocks orbit suggests possible new planet". February 10, 2022. Retrieved February 11, 2022.
External links
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