Astronomy:TVLM 513-46546
File:TVLM 513-46546 as seen by SDSS.jpg TVLM 513-46546 (the red dot in the center), as seen by the Sloan Digital Sky Survey. | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Boötes[1] |
| Right ascension | 15h 01m 08.18646s[2] |
| Declination | +22° 50′ 02.1379″[2] |
| Apparent magnitude (V) | 15.09[3] |
| Characteristics | |
| Evolutionary stage | Brown dwarf[4] |
| Spectral type | M9[5] |
| Astrometry | |
| Proper motion (μ) | RA: −43.120±0.111[2] mas/yr Dec.: −65.138±0.140[2] mas/yr |
| Parallax (π) | 93.1655 ± 0.1355[2] mas |
| Distance | 35.01 ± 0.05 ly (10.73 ± 0.02 pc) |
| Details | |
| Mass | 0.06–0.08[4][6] M☉ |
| Radius | 0.097 – 0.109[6] R☉ |
| Luminosity | 0.00026[6] L☉ |
| Temperature | 2242±55[7] K |
| Rotation | 1.96 h[6] |
| Rotational velocity (v sin i) | 60[6] km/s |
| Age | >400[6][5] Myr |
| Other designations | |
2MASS J15010818+2250020, 2MASSI J1501081+225001, 2MUCD 20596 | |
| Database references | |
| SIMBAD | data |
TVLM 513-46546 is an M9 ultracool dwarf at the red dwarf/brown dwarf mass boundary in the constellation Boötes. It exhibits flare star activity, which is most pronounced at radio wavelengths. The star has a mass approximately 80 times the mass of Jupiter (or 8 percent of the Sun's mass). The radio emission is broadband and highly circularly polarized, similar to planetary auroral radio emissions.[9] The radio emission is periodic, with bursts emitted every 7054 s, with nearly one hundredth of a second precision. Subtle variations in the radio pulses could suggest that the ultracool dwarf rotates faster at the equator than the poles (differential rotation) in a manner similar to the Sun.[10]
Planetary system
On 4 August 2020 astronomers announced the discovery of a Saturn-like planet TVLM 513b around this star with a period of 221±5 days, a mass of between 0.35 and 0.42 MJ, a circular orbit (e≃0), a semi-major axis of between 0.28 and 0.31 AU and an inclination angle of 71−88°. The companion was detected by the radio astrometry method.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.35−0.42 MJ | 0.28−0.31 | 221±5 | 0 | 71−88° | — |
References
- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R Constellation record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ "TVLM 513-46". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=TVLM+513-46.
- ↑ 4.0 4.1 Gawroński, Marcin P.; Goździewski, Krzysztof; Katarzyński, Krzysztof (2016-12-22). "Physical properties and astrometry of radio-emitting brown dwarf TVLM 513-46546 revisited" (in en). Monthly Notices of the Royal Astronomical Society 466 (4): 4211–4220. doi:10.1093/mnras/stw3329. ISSN 0035-8711.
- ↑ 5.0 5.1 5.2 Curiel, Salvador; Ortiz-León, Gisela N.; Mioduszewski, Amy J.; Torres, Rosa M. (2020). "An Astrometric Planetary Companion Candidate to the M9 Dwarf TVLM 513–46546". The Astronomical Journal 160 (3): 97. doi:10.3847/1538-3881/ab9e6e. Bibcode: 2020AJ....160...97C.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Hallinan, G.; Antonova, A.; Doyle, J. G.; Bourke, S.; Lane, C.; Golden, A. (2008-09-01). "Confirmation of the Electron Cyclotron Maser Instability as the Dominant Source of Radio Emission from Very Low Mass Stars and Brown Dwarfs" (in en). The Astrophysical Journal 684 (1): 644. doi:10.1086/590360. ISSN 0004-637X. Bibcode: 2008ApJ...684..644H.
- ↑ Filippazzo, Joseph C.; Rice, Emily L.; Faherty, Jacqueline; Cruz, Kelle L.; Van Gordon, Mollie M.; Looper, Dagny L. (2015-09-10). "Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime". The Astrophysical Journal 810 (2): 158. doi:10.1088/0004-637X/810/2/158. ISSN 1538-4357. Bibcode: 2015ApJ...810..158F.
- ↑ Harding, L. K.; Hallinan, G.; Boyle, R. P.; Golden, A.; Singh, Navtej; Sheehan, B.; Zavala, R. T.; Butler, R. F. (December 2013). "Periodic Optical Variability of Radio-detected Ultracool Dwarfs". The Astrophysical Journal 779 (2): 101. doi:10.1088/0004-637X/779/2/101. Bibcode: 2013ApJ...779..101H.
- ↑ Hallinan, G. (2006). "Rotational Modulation of the Radio Emission from the M9 Dwarf TVLM 513-46546: Broadband Coherent Emission at the Substellar Boundary?". The Astrophysical Journal 653 (1): 690–699. doi:10.1086/508678. Bibcode: 2006ApJ...653..690H.
- ↑ Wolszczan, A.; Route, M. (2014). "Timing Analysis of the Periodic Radio and Optical Brightness Variations of the Ultracool Dwarf, TVLM 513-46546". The Astrophysical Journal 788 (1): 23. doi:10.1088/0004-637X/788/1/23. Bibcode: 2014ApJ...788...23W.
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