Astronomy:WD 0032−317
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 00h 34m 49.8573s |
| Declination | −31° 29′ 52.686″ |
| Characteristics | |
| Evolutionary stage | White dwarf |
| Astrometry | |
| Parallax (π) | 2.320±0.053 mas |
| Distance | 431.1±9.8 pc |
| Orbit | |
| Primary | WD 0032−317 |
| 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 | |
WD 0032−317 is a low mass white dwarf star orbited by brown dwarf WD 0032−317 b.
WD 0032−317
The white dwarf WD 0032−317 is located about 1,400 light years from Earth.[1] It is notable for its extreme temperature. WD 0032−317 has 40% of the Sun's mass, but has a much higher temperature of 37,000 Kelvin, compared to the suns temperature of 5778 Kelvin.[inconsistent] 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
The orbiting brown dwarf, WD 0032−317 b, was massive enough to survive the red giant's nova event.[2] 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 Kelvin and a night temperature of about 2000 Kelvin 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.[3][4][5]
References
- ↑ Atkinson, Nancy (2023-08-17). "This Brown Dwarf is 2,000 Degrees Hotter Than the Sun" (in en-US). https://www.universetoday.com/162810/this-brown-dwarf-is-2000-degrees-hotter-than-the-sun/.
- ↑ Yirka, Bob; Phys.org. "Discovery of a Brown Dwarf Hotter Than the Sun" (in en). https://phys.org/news/2023-06-discovery-brown-dwarf-hotter-sun.html.
- ↑ Hallakoun, Na’ama; Maoz, Dan; Istrate, Alina G.; Badenes, Carles; Breedt, Elmé; Gänsicke, Boris T.; Jha, Saurabh W.; Leibundgut, Bruno et al. (2023-08-14). "An Irradiated-Jupiter Analogue Hotter Than the Sun" (in en). Nature Astronomy: 1–12. doi:10.1038/s41550-023-02048-z. ISSN 2397-3366. https://www.nature.com/articles/s41550-023-02048-z.
- ↑ Gamillo, Elizabeth (15 August 2023). "Astronomers Find a Brown Dwarf That’s Hotter Than the Sun | Astronomy.com". https://www.astronomy.com/science/astronomers-find-a-brown-dwarf-thats-hotter-than-the-sun/.
- ↑ "A Brown Dwarf Star Serves as an Ultrahot-Jupiter Analogue". https://pubs.aip.org/physicstoday/online/42662/A-brown-dwarf-star-serves-as-an-ultrahot-Jupiter.
 |  |
