WD 0032−317
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| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Sculptor[1] |
| Right ascension | 00h 34m 49.8573s |
| Declination | −31° 29′ 52.686″ |
| Apparent magnitude (V) | 16.17[2] |
| Characteristics | |
| Evolutionary stage | White dwarf |
| Astrometry | |
| Parallax (π) | 2.320±0.053 mas |
| Distance | 431.1±9.8 pc |
| Orbit | |
| Primary | WD 0032−317 |
| Period (P) | 8340.9090±0.0013 s |
| Semi-amplitude (K1) (primary) | 53.4±1.7 km/s |
| Details | |
| WD 0032−317 | |
| Mass | 0.4187±0.0047 (He-core) 0.386±0.014 (Hybrid-core) M☉ |
| Radius | 0.0266±0.0012 R☉ |
| Temperature | 36965±100 K |
| WD 0032−317 b | |
| Mass | 0.0812±0.0029 (He-core) 0.0750±0.0037 (Hybrid-core) M☉ |
| Radius | 0.0789+0.0085 −0.0083 (He-core) 0.0747+0.0085 −0.0079 (Hybrid-core) R☉ |
| Temperature | 5126±28 (He-core) 5111±41 (Hybrid-core) (equilibrium temperature) K |
| Other designations | |
| WD 0032−317, MCT 0032-3146, EC 00323-3146, GALEX J003449.8-312952, 2MASS J00344984-3129524, TIC 251857373, USNO-B1.0 0585-00006922, Gaia DR3 2317319612801004416, Gaia DR2 2317319612801004416 | |
| Database references | |
| SIMBAD | data |
WD 0032−317 is a low mass white dwarf star orbited by brown dwarf WD 0032−317 b.
WD 0032−317
[edit]The white dwarf WD 0032−317 is located about 1,400 light years from Earth.[3] WD 0032−317 formed about three billion years ago when a low mass star (possibly of 1.3 solar masses) expanded into its red giant phase. The star then blew out its outer layers leaving behind the helium-rich core (which is WD 0032−317).
WD 0032−317 b
[edit]The orbiting brown dwarf, WD 0032−317 b, was massive enough to survive the red giant's nova event.[4] It is an extremely hot and very large (75-88 Jupiter masses) brown dwarf that orbits WD 0032−317. One orbit from WD 0032−317 b takes only 2.5 hours. This object is tidally locked to its star with a day side temperature of 8,000 K (7,730 °C; 13,940 °F) and a night temperature of about 2,000 K (1,730 °C; 3,140 °F) making its temperature equivalent to a planet orbiting close to a late stage B-type star. The intense ultraviolet (UV) exposure can break down the molecules in WD 0032−317's atmosphere and vaporize materials from the surface of the brown dwarf.[5][6][7]
References
[edit]- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- ↑ Gaia Collaboration; et al. (2023). "Gaia Data Release 3. The Galaxy in your preferred colours: Synthetic photometry from Gaia low-resolution spectra". Astronomy and Astrophysics. 674. arXiv:2206.06215. Bibcode:2023A&A...674A..33G. doi:10.1051/0004-6361/202243709.
- ↑ Atkinson, Nancy (2023-08-17). "This Brown Dwarf is 2,000 Degrees Hotter Than the Sun". Universe Today. Retrieved 2023-08-28.
- ↑ Yirka, Bob; Phys.org. "Discovery of a Brown Dwarf Hotter Than the Sun". phys.org. Retrieved 2023-08-28.
- ↑ Hallakoun, Na’ama; Maoz, Dan; Istrate, Alina G.; Badenes, Carles; Breedt, Elmé; Gänsicke, Boris T.; Jha, Saurabh W.; Leibundgut, Bruno; Mannucci, Filippo; Marsh, Thomas R.; Nelemans, Gijs; Patat, Ferdinando; Rebassa-Mansergas, Alberto (2023-08-14). "An Irradiated-Jupiter Analogue Hotter Than the Sun". Nature Astronomy: 1–12. arXiv:2306.08672. doi:10.1038/s41550-023-02048-z. ISSN 2397-3366.
- ↑ Gamillo, Elizabeth (15 August 2023). "Astronomers Find a Brown Dwarf That's Hotter Than the Sun | Astronomy.com". Astronomy Magazine. Retrieved 28 August 2023.
- ↑ "A Brown Dwarf Star Serves as an Ultrahot-Jupiter Analogue". pubs.aip.org. Retrieved 28 August 2023.
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