HD 210277

HD 210277 is a 7th magnitude star in the constellation of Aquarius. It is a yellow dwarf star (spectral type G0V) with a mass around 9% larger than that of our Sun.[2] Since its distance is about 70 light years, it is not visible to the unaided eye. With binoculars it is easily visible.

HD 210277
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension  22h 09m 29.8657s[1]
Declination −07° 32′ 55.1630″[1]
Apparent magnitude (V) 6.63
Characteristics
Spectral type G0V
U−B color index 0.43
B−V color index 0.773
Astrometry
Radial velocity (Rv)−24.1 km/s
Proper motion (μ) RA: 85.462±0.072[1] mas/yr
Dec.: −450.544±0.067[1] mas/yr
Parallax (π)46.9229 ± 0.0481[1] mas
Distance69.51 ± 0.07 ly
(21.31 ± 0.02 pc)
Absolute magnitude (MV)4.99
Details
Mass1.09 M☉
Radius1.1 ± 0.05 R☉
Luminosity1.2 L☉
Temperature5532 ± 14 K
Metallicity0.19 ± 0.04
Age6.93 G years
Other designations
NLTT 53073, SAO 145906, BD-08° 5818, Gl 848.4, HIP 109378, GJ 9769, LTT 8887, GCRV 13920, PPM 206033
Database references
SIMBADdata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

The star has an extrasolar planet that has a minimum mass greater than Jupiters orbiting it in 442 days.[3] Claims were made in 1999 that a dust disk around the star HD 210277, similar to that produced by the Kuiper Belt had been imaged, lying between 30 and 62 AU from the star.[4] However, observations with the Spitzer Space Telescope failed to detect any infrared excess at 70 micrometres or at 24 micrometres wavelengths.[5][6]

Planetary system

The only known planet was discovered using 34 radial velocity measurements taken from 1996 to 1998 at W. M. Keck Observatory.[3]

The HD 210277 planetary system[7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >1.29 ± 0.11 MJ 1.138 ± 0.066 442.19 ± 0.50 0.476 ± 0.017 — —
gollark: Your parent does sound somewhat crazy.
gollark: Just 3D-print replacements. Obviously. Or duct-tape it back on.
gollark: Solution: reinstall the door in secret.
gollark: we mostly only have outages here for a few hours after/during stormy weather.
gollark: You may also want to check the starboard.

See also
  • List of extrasolar planets

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Gonzalez; et al. (1999). "Parent Stars of Extrasolar Planets. IV. 14 Herculis, HD 187123, and HD 210277". The Astrophysical Journal Letters. 511 (2): L111–L114. Bibcode:1999ApJ...511L.111G. doi:10.1086/311847.
  3. Marcy, Geoffrey W.; et al. (1999). "Two New Planets in Eccentric Orbits". The Astrophysical Journal. 520 (1): 239–247. arXiv:astro-ph/9904275. Bibcode:1999ApJ...520..239M. doi:10.1086/307451.
  4. Trilling, D. E.; et al. (2000). "Circumstellar Dust Disks around Stars with Known Planetary Companions". The Astrophysical Journal. 529 (1): 499–505. Bibcode:2000ApJ...529..499T. doi:10.1086/308280.
  5. Beichman, C. A.; et al. (2005). "Planets and Infrared Excesses: Preliminary Results from a Spitzer MIPS Survey of Solar-Type Stars". The Astrophysical Journal. 622 (2): 1160–1170. arXiv:astro-ph/0412265. Bibcode:2005ApJ...622.1160B. doi:10.1086/428115.
  6. Bryden, G.; et al. (2009). "Planets and Debris Disks: Results from a Spitzer/MIPS Search for Infrared Excess" (PDF). The Astrophysical Journal. 705 (2): 1226–1236. Bibcode:2009ApJ...705.1226B. doi:10.1088/0004-637X/705/2/1226.
  7. Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.


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