ROXs 42Bb
| Exoplanet | List of exoplanets | |
|---|---|---|
| 300px |
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| Parent star | ||
| Star | ROXs 42B | |
| Constellation | Ophiuchus | |
| Right ascension | (α) | 16h 31m 15.0s |
| Declination | (δ) | −24° 32′ 43.7″ |
| Apparent magnitude | (mV) | 14.27 |
| Distance | 440 ± 16 ly (135 ± 5 pc) |
|
| Spectral type | M0V | |
| Age | 0.002+.002 −.0001 Gyr |
|
| Observed separation Observation epoch 2011 Jun 22 |
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| Angular separation | (ρ) | 1169 ± 5 mas |
| Position angle | (θ) | 269.25 ± 0.25° |
| Projected separation | (d) | 157 AU |
| Physical characteristics | ||
| Mass | (m) | 9.0+3 −3 MJ |
| Surface gravity | (g) | 3.8 ± 0.2 g |
| Temperature | (T) | 1950-2000 |
| Discovery information | ||
| Discovery date | October 17, 2013 | |
| Discoverer(s) | Currie et al.[1] | |
| Discovery method | Direct imaging | |
| Discovery site | Keck Telescope, Very Large Telescope, Subaru Telescope | |
| Discovery status | Published[1] | |
ROXs 42Bb is a directly imaged planetary-mass companion[1] to the binary M star ROXs 42B,[2] a likely member of the Rho Ophiuchi cloud complex. The companion was announced/discovered on October 17, 2013 by University of Toronto astronomer Thayne Currie.
The object has an estimated mass between 6 and 12 Jupiter masses, depending on the age of the star,[1] similar to the masses of directly imaged planets around HR 8799 and beta Pictoris. However, it is unclear whether ROXs 42Bb formed like these planets via core accretion, formed by disk (gravitational) instability, or formed more like a binary star. Preliminary fits of the spectra and broadband photometry to atmospheric models imply an effective temperature of about 2000 K.[3] Like Beta Pictoris b, ROXs 42Bb's atmosphere is likely very cloudy and dusty.[3]
References
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