2MASS J0523−1403
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Lepus[1] |
| Right ascension | 05h 23m 38.2236s[2] |
| Declination | −14° 03′ 02.018″[2] |
| Apparent magnitude (V) | 21.05[3] |
| Characteristics | |
| Evolutionary stage | Main sequence[3] |
| Spectral type | L2.5[3][4] |
| Astrometry | |
| Radial velocity (Rv) | +12.21±0.09[5] km/s |
| Proper motion (μ) | RA: +107.484 mas/yr[2] Dec.: +161.468 mas/yr[2] |
| Parallax (π) | 78.5273±0.1469 mas[2] |
| Distance | 41.53 ± 0.08 ly (12.73 ± 0.02 pc) |
| Absolute magnitude (MV) | 20.6[3] |
| Details | |
| Mass | 0.07[6] M☉ |
| Radius | 0.09±0.01[6] R☉ |
| Luminosity | 0.000131±0.000008[6] L☉ |
| Surface gravity (log g) | 5.5[7] cgs |
| Temperature | 1939±68[4] K |
| Rotational velocity (v sin i) | 21[8] km/s |
| Other designations | |
| 2MASS J05233822−1403022, 2MUCD 10390, 2MASSI J0523382−140302, USNO-B1.0 0759−00062850 | |
| Database references | |
| SIMBAD | data |
2MASS J0523−1403 is a very-low-mass red dwarf about 40 light-years from Earth in the southern constellation of Lepus, with a very faint visual magnitude of 21.05 and a low effective temperature of about 2000 K. It is visible primarily in large telescopes sensitive to infrared light. 2MASS J0523−1403 was first observed as part of the Two Micron All-Sky Survey (2MASS).[9]
Characteristics
2MASS J0523−1403 has a bolometric luminosity of 0.000131 L☉,[6] a radius of 0.09 R☉,[6] and an effective temperature of 1939 K.[4] This makes this star one of the smallest and coolest main sequence stars.[3] It has a stellar classification of L2.5 and a V−K color index of 9.42.[3] Observation with the Hubble Space Telescope has detected no companion beyond 0.15 arcsecond.[10] Sporadic radio emissions were detected by the VLA in 2004.[11] H-alpha (Hα) emissions have also been detected, a sign of chromospheric activity.[8]
Members of the RECONS group have identified 2MASS J0523−1403 as representative of the smallest possible stars.[12] Its small radius is at the local minimums of the radius–luminosity and radius–temperature trends.[3] This local minimum is predicted to occur at the hydrogen burning limit due to differences in the radius-mass relationships of stars and brown dwarfs. Unlike hydrogen-burning stars, brown dwarfs decrease in radius as mass increases due to their cores being supported by degeneracy pressure. As the mass increases an increasing fraction of the brown dwarf is degenerate causing the radius to shrink as mass increases.[12] The minimum stellar mass is estimated to be between 0.07 and 0.077 M☉,[3] comparable to the estimated mass of 2MASS J0523−1403 of 0.07 M☉.[6]
See also
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 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g h Dieterich, Sergio B.; Henry, Todd J.; Jao, Wei-Chun; Winters, Jennifer G.; Hosey, Altonio D.; Riedel, Adric R.; Subasavage, John P. (May 2014). "The Solar Neighborhood XXXII. The Hydrogen Burning Limit". The Astronomical Journal. 147 (5). article id 94. arXiv:1312.1736. Bibcode:2014AJ....147...94D. doi:10.1088/0004-6256/147/5/94. S2CID 21036959.
- ^ a b c Kirkpatrick, J. Davy; Marocco, Federico; Gelino, Christopher R.; Raghu, Yadukrishna; Faherty, Jacqueline K.; Bardalez Gagliuffi, Daniella C.; Schurr, Steven D.; Apps, Kevin; Schneider, Adam C.; Meisner, Aaron M.; Kuchner, Marc J.; Caselden, Dan; Smart, R. L.; Casewell, S. L.; Raddi, Roberto (2024-04-01). "The Initial Mass Function Based on the Full-sky 20 pc Census of ∼3600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series. 271 (2): 55. arXiv:2312.03639. Bibcode:2024ApJS..271...55K. doi:10.3847/1538-4365/ad24e2. ISSN 0067-0049.
- ^ Blake, Cullen H.; Charbonneau, David; White, Russel J. (2010). "The NIRSPEC Ultracool Dwarf Radial Velocity Survey". The Astrophysical Journal. 723 (1): 684–706. arXiv:1008.3874. Bibcode:2010ApJ...723..684B. doi:10.1088/0004-637X/723/1/684. S2CID 119271941.
- ^ a b c d e f Sebastian, D.; Gillon, M.; Ducrot, E.; Pozuelos, F. J.; Garcia, L. J.; Günther, M. N.; Delrez, L.; Queloz, D.; Demory, B. O.; Triaud, A. H. M. J.; Burgasser, A.; de Wit, J.; Burdanov, A.; Dransfield, G.; Jehin, E. (January 2021). "SPECULOOS: Ultracool dwarf transit survey: Target list and strategy". Astronomy & Astrophysics. 645: A100. arXiv:2011.02069. Bibcode:2021A&A...645A.100S. doi:10.1051/0004-6361/202038827. ISSN 0004-6361.
- ^ Cifuentes, C.; Caballero, J. A.; Cortés-Contreras, M.; Montes, D.; Abellán, F. J.; Dorda, R.; Holgado, G.; Zapatero Osorio, M. R.; Morales, J. C.; Amado, P. J.; Passegger, V. M.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Sanz-Forcada, J. (October 2020). "CARMENES input catalogue of M dwarfs: V. Luminosities, colours, and spectral energy distributions". Astronomy & Astrophysics. 642: A115. arXiv:2007.15077. Bibcode:2020A&A...642A.115C. doi:10.1051/0004-6361/202038295. ISSN 0004-6361.
- ^ a b Reiners, Ansgar; Basri, Gibor (2008). "Chromospheric Activity, Rotation, and Rotational Braking in M and L Dwarfs". The Astrophysical Journal. 684 (2): 1390–1403. arXiv:0805.1059v2. Bibcode:2008ApJ...684.1390R. doi:10.1086/590073. S2CID 17635923.
- ^ Cruz, Kelle L.; Reid, I. Neill; Liebert, James; Kirkpatrick, J. Davy; Lowrance, Patrick J. (2003). "Meeting the Cool Neighbors. V. A 2MASS-Selected Sample of Ultracool Dwarfs". The Astronomical Journal. 126 (5): 2421–2448. arXiv:astro-ph/0307429. Bibcode:2003AJ....126.2421C. doi:10.1086/378607. S2CID 119445748.
- ^ Reid, I. Neill; Lewitus, E.; Allen, P. R.; Cruz, Kelle L.; Burgasser, Adam J. (2006). "A Search for Binary Systems among the Nearest L Dwarfs". The Astronomical Journal. 132 (2): 891–901. arXiv:astro-ph/0606331. Bibcode:2006AJ....132..891R. doi:10.1086/505626. S2CID 28828906.
- ^ Antonova, A.; Doyle, J. G.; Hallinan, G.; Golden, A.; Koen, C. (2 September 2007). "Sporadic long-term variability in radio activity from a brown dwarf". Astronomy and Astrophysics. 472 (1): 257–260. arXiv:0707.0634. Bibcode:2007A&A...472..257A. doi:10.1051/0004-6361:20077231. S2CID 14185434.
- ^ a b Garmany, Katy (9 December 2013). "NOAO/SOAR: Where do stars end and brown dwarfs begin?" (Press release). National Optical Astronomy Observatory. Archived from the original on 12 January 2020. Retrieved 14 December 2013.
