HD 16760
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 42m 21s |
| Declination | +38° 37′ 07″ |
| Apparent magnitude (V) | 8.74 |
| Characteristics | |
| Spectral type | G5V[1] |
| B−V color index | 0.715[1] |
| Astrometry | |
| Proper motion (μ) | RA: 82.84 mas/yr Dec.: -110.65 mas/yr |
| Parallax (π) | 22.00 ± 2.35[1][2] mas |
| Distance | approx. 150 ly (approx. 45 pc) |
| Absolute magnitude (MV) | 5.41[1] |
| Details | |
| Mass | 0.78 ± 0.05[1] M☉ |
| Radius | 0.81 ± 0.27[1] R☉ |
| Luminosity (bolometric) | 0.72 ± 0.43[1] L☉ |
| Surface gravity (log g) | 4.47 ± 0.06[1] cgs |
| Temperature | 5629 ± 44[1] K |
| Metallicity | [Fe/H] = +0.067 ± 0.05[1] |
| Rotational velocity (v sin i) | 0.5 ± 0.5[1] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia |
data |
HD 16760 is a binary star system approximately 150 light-years away in the constellation Perseus. The primary star HD 16760 (HIP 12638) is a G-type main sequence star similar to our Sun. The secondary, HIP 12635 is 1.521 magnitudes fainter and located at a separation of 14.6 arcseconds from the primary, corresponding to a physical separation of at least 660 AU. Announced in July 2009, HD 16760 has been confirmed to have a substellar object orbiting it. Whether or not this object is a brown dwarf or an extrasolar planet is currently not understood.[1][3]
Substellar companion
The companion object was discovered independently by the SOPHIE extrasolar planets program[3] and the N2K Consortium.[1] It has a mass exceeding the lower limit required for fusion of deuterium in its interior. This criterion is sometimes used to distinguish between brown dwarfs, which lie above the limit, and planets which lie below the limit.[4] However its orbit is nearly circular, indicating that it may have formed in the same way as planets do, from a circumstellar disc.[3] The formation of massive planets up to 20–25 Jupiter masses has been predicted in some models of the core accretion process.[5] The identity of this object as a brown dwarf or a massive planet was thus unclear.
However, recently data analysed from direct imaging, using ground based telescopes fitted with adaptive optics, on the companion object has revealed that it is aligned in a much more face on orbit than previously realised. Consequently, its mass has been revised upwards. It is now no longer believed to be a large gas giant or even a brown dwarf but with a new mass calculated at around one quarter that of our sun, or nearly 300 Jupiter masses, it easily qualifies as a stellar object, probably a red dwarf.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥13.13 ± 0.56 MJ | 1.084 ± 0.023 | 466.47 ± 0.35 | 0.084 ± 0.003 | — | — |
Notes
- ↑ Both groups quote slightly different parameters for the object, the primary difference being the stellar mass which is given in the SOPHIE paper as 0.88 stellar masses, which leads to a companion mass at least 14.3 times that of Jupiter. The values quoted here are from the N2K consortium, whose modelling of the stellar properties incorporated the distance from most recent reduction of the Hipparcos catalogue.
References
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 Lua error in package.lua at line 80: module 'strict' not found.
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- ↑ 3.0 3.1 3.2 Lua error in package.lua at line 80: module 'strict' not found.
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