2MASS 1237+6526
File:2MASS 1237+6526 legacy dr10.jpg T-type brown dwarf 2MASS 1237+6526 (faint red "star" in the center) imaged by legacy surveys | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | +16.05 |
| Characteristics | |
| Spectral type | T6.5[2] |
| Astrometry | |
| Parallax (π) | 96.07±4.78 mas[3] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Details | |
| Mass | 0.035 Template:Solar mass |
| Radius | 0.11 Template:Solar radius |
| Luminosity | 6.25x10−6 Template:Solar luminosity |
| Temperature | 850[4] K |
| Age | ≥2-10[4] billion years |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| 2MASS J12373919+6526148, 2MASSI J1237392+652615, 2MASSW J1237392+652615 | |
| Database references | |
| SIMBAD | data |
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2MASS J12373919+6526148 (hereafter 2MASS 1237+6526) is a brown dwarf object with late spectral type T in the constellation of Draco, nearly 34 light-years away from the Sun.[3] The substellar object could likely host a very low-mass companion (yet undetected but inferred), possibly in the planetary regime.[2] This has been inferred from unusual Hα emission that it exhibited in the past.[5]
Radio observations with the Very Large Array detected the brown dwarf. The strong detection is due to weakly circularly polarized (~35%) quiescent emission as well as pulsed emission, including a strong pulse that was highly circularly polarized (~80%). Two weaker pulses occurred before and after this strong pulse. This constrained the rotation period to Script error: No such module "val"..[6] 2MASS 1237+6526 may potentially show aurorae, which would be significant since extrasolar aurorae have not been detected, but this has not been conclusively demonstrated.[5]
Possible planetary companion
Burgasser et al. (2003)[2] have inferred the presence of a low-mass companion orbiting the brown dwarf 2MASS 1237+6526. Such object would yield a mass between 3 and 12 times that of Jupiter and take nearly 4.56 hours (0.19 days) to revolve around its dim primary. If confirmed it would be one of the shortest period exoplanets and orbiting one of the faintest hosts so far. Accounting very faint luminosity of the primary (6.25/1,000,000th of Sun's luminosity), the habitable zone is located within 0.0025 astronomical units, so the putative planet could likely retain great amounts of water and ammonia. Moreover, both the objects would appear the same size.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥3-12 MJ | ≤0.003 | ≥0.19 | 0? | — | — |
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See also
Other T-dwarfs with detected radio emission:
- SIMP J013656.5+093347.3 T2.5, planetary-mass object
- 2MASS J10475385+2124234 T6.5
- WISEPC J112254.73+255021.5 T6
- WISEPA J101905.63+652954.2 T5.5+T7.0
- WISEPA J062309.94-045624.6 T8
References
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