2MASS J22282889−4310262
Artist's representation of 2MASS J22282889−4310262 | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Grus[1] |
| Right ascension | 22h 28m 28.894s[2] |
| Declination | −43° 10′ 26.27″[2] |
| Characteristics | |
| Spectral type | T6[3] |
| Apparent magnitude (J) | 15.662[2] |
| Apparent magnitude (H) | 15.363[2] |
| Apparent magnitude (K) | 15.296[2] |
| Astrometry | |
| Proper motion (μ) | RA: +51.7[4] mas/yr Dec.: −301.3[4] mas/yr |
| Parallax (π) | 94.0±7.0 mas[5] |
| Distance | 35 ± 3 ly (10.6 ± 0.8 pc) |
| Details[6] | |
| Radius | 0.94±0.16[7] RJup |
| Surface gravity (log g) | 5.0 cgs |
| Temperature | 900 K |
| Rotation | 1.41±0.01 h |
| Age | 1[7] Gyr |
| Other designations | |
| 2MASS J22282889−4310262, WISEP J222829.00−431029.4 | |
| Database references | |
| SIMBAD | data |
2MASS J22282889−4310262 is a brown dwarf discovered by the Hubble Space Telescope and The Spitzer Space Telescope in 2013. Using Hubble and Spitzer, NASA astronomers were able to develop the most detailed 'weather map' for brown dwarfs, utilizing different wavelengths of infrared light to show changing light patterns and different layers of material in the windstorms (the layers were generated because water and methane vapors are visible at different infrared wavelengths). This observation was the first time that researchers were able to probe such variability at different altitudes in a brown dwarf.[8] In the outer layers of its atmosphere, gases condense into raindrop-like particles made up of sand and iron which fall into the interior.[9]
Researchers also determined that the object's temperature ranges from 1,100 to 1,300 degrees Fahrenheit (600 to 700 degrees Celsius). The brown dwarf is rotating extremely rapidly, with 1.41 hours rotation period being the smallest reliably measured rotation period of the brown dwarf as of 2021.[3]
In 2026 a team of researchers used archival data by the Very Large Array to detect radio emission from the brown dwarf. T-dwarfs with detected radio emissions are rare and are caused by auroral processes. The radio emission at 2MASS 2228-4310 showed highly polarised bursts at intervals of around 47 and 58 minutes, or around half the rotation period. This emission comes from electron cyclotron maser emission and the magnetic field strength is constrained to around B ≥ 1.4 kG.[10]
See also
Other T-dwarfs with detected radio emission
- SIMP J013656.5+093347.3 T2.5, planetary-mass object
- 2MASS J10475385+2124234 T6.5
- WISEPA J101905.63+652954.2 T5.5+T7.0
- WISEPA J062309.94-045624.6 T8
- 2MASS 1237+6526 T6.5
- WISEPC J112254.73+255021.5 T6
References
- ^ 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.
- ^ a b c d e Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
- ^ a b Tannock, Megan E.; Metchev, Stanimir; Heinze, Aren; Miles-Páez, Paulo A.; Gagné, Jonathan; Burgasser, Adam; Marley, Mark S.; Apai, Dániel; Suárez, Genaro; Plavchan, Peter (2021), "Weather on Other Worlds. V. The Three Most Rapidly Rotating Ultra-cool Dwarfs", The Astronomical Journal, 161 (5): 224, arXiv:2103.01990, Bibcode:2021AJ....161..224T, doi:10.3847/1538-3881/abeb67, S2CID 232105126
- ^ a b "2MASS J22282889-4310262". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 19 December 2016.
- ^ Faherty, Jacqueline K. (2012). "The Brown Dwarf Kinematics Project (BDKP). III. Parallaxes for 70 Ultracool Dwarfs". The Astrophysical Journal. 752 (1): 56. arXiv:1203.5543. Bibcode:2012ApJ...752...56F. doi:10.1088/0004-637X/752/1/56. S2CID 18160586.
- ^ Esther Buenzli; et al. (24 October 2012). "Vertical Atmospheric Structure in a Variable Brown Dwarf: Pressure-dependent Phase Shifts in Simultaneous Hubble Space Telescope-Spitzer Light Curves". The Astrophysical Journal. 760 (2): L31. arXiv:1210.6654. Bibcode:2012ApJ...760L..31B. doi:10.1088/2041-8205/760/2/L31. S2CID 5954599.
- ^ a b Vos, Johanna M.; Biller, Beth A.; Allers, Katelyn N.; Faherty, Jacqueline K.; Liu, Michael C.; Metchev, Stanimir; Eriksson, Simon; Manjavacas, Elena; Dupuy, Trent J.; Janson, Markus; Radigan-Hoffman, Jacqueline; Crossfield, Ian; Bonnefoy, Mickaël; Best, William M. J.; Homeier, Derek; Schlieder, Joshua E.; Brandner, Wolfgang; Henning, Thomas; Bonavita, Mariangela; Buenzli, Esther (2020), "Spitzer Variability Properties of Low-gravity L Dwarfs", The Astronomical Journal, 160 (1): 38, arXiv:2005.12854, Bibcode:2020AJ....160...38V, doi:10.3847/1538-3881/ab9642, S2CID 218889787
- ^ "NASA Telescopes See Weather Patterns in Brown Dwarf". NASA/JPL. Retrieved 2015-12-03.
- ^ "2MASSJ22282889-431026: The Hybrid Planet-Star With A Stormy Atmosphere". Science 2.0. 27 August 2014. Retrieved 2015-12-03.
- ^ Wandia, Kelvin (7 Jan 2026). "Radio Activity from the Rapidly Rotating T dwarf 2MASS 2228-4310". arXiv:2601.04158 [astro-ph.SR].