Astronomy:HD 210277

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Short description: Star in the constellation Aquarius
HD 210277
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aquarius
Right ascension  22h 09m 29.8658s[1]
Declination −07° 32′ 55.162″[1]
Apparent magnitude (V) 6.54[2]
Characteristics
Spectral type G8V[3] or G8/K0V[4]
U−B color index 0.43
B−V color index 0.773
Astrometry
Radial velocity (Rv)−20.855±0.0003[5] km/s
Proper motion (μ) RA: 85.407(29)[1] mas/yr
Dec.: −450.617(23)[1] mas/yr
Parallax (π)46.8515 ± 0.0283[1] mas
Distance69.61 ± 0.04 ly
(21.34 ± 0.01 pc)
Absolute magnitude (MV)4.90±0.05[6]
Details[7]
Mass1.007+0.040
−0.039 M☉
Radius1.087+0.015
−0.016 R☉
Luminosity1.002[8] L☉
Surface gravity (log g)4.369±0.020 cgs
Temperature5,705±35 K
Metallicity [Fe/H]0.170±0.097 dex
Rotation40.8 d[9]
Rotational velocity (v sin i)1.888±0.158 km/s
Age6.471+1.744
−1.643[7]
8.929±2.671[2] Gyr
Other designations
BD−08°5818, GJ 9769, HD 210277, HIP 109378, SAO 145906, PPM 206033, LTT 8887, NLTT 53073, 2MASS J22092985-0732548[10]
Database references
SIMBADdata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

HD 210277 is a single[9] star in the equatorial constellation of Aquarius. It has an apparent visual magnitude of 6.54,[2] which makes it a challenge to view with the naked eye, but it is easily visible in binoculars. The star is located at a distance of 69.6 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −20.9 km/s.[5]

An early classification of this star was a G0 dwarf,[11] and some sources still use this value.[12] More modern classification surveys list it as G8V,[3] matching a late G-type main-sequence star.[9] It is older than the Sun with a very low level of chromospheric activity[3] and is spinning with a projected rotational velocity of 1.9 km/s. The star has a slightly higher mass and larger radius than the Sun.[7]

Planetary system

In 1999 it was announced that a dust disk orbiting HD 210277, similar to that produced by the Kuiper Belt, had been imaged, lying between 30 and 62 AU from the star.[13] However, observations with the Spitzer Space Telescope failed to detect any infrared excess at 70 micrometres or at 24 micrometres wavelengths.[14][15] Subsequent measurements by the Herschel Space Observatory did detect an excess at 100 and 160 micrometres. A model fit to the emission matches a disk orbiting at 160 AU with a mean temperature of 22 K.[16] The disk signal is fairly strong, with S/N equal to 6.6.[8]

The only known exoplanet was discovered using 34 radial velocity measurements taken from 1996 to 1998 at W. M. Keck Observatory. It has a minimum mass greater than Jupiter orbiting the star in 442 days.[9] The high eccentricity (ovalness) of the exoplanet's orbit means it is unlikely that there is a companion planet co-orbiting the star at a trojan point.[12]

The HD 210277 planetary system[17]
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 — —
debris disk 160[16] AU — —

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 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.
  2. ↑ 2.0 2.1 2.2 Delgado Mena, E. et al. (April 2019). "Abundance to age ratios in the HARPS-GTO sample with Gaia DR2. Chemical clocks for a range of [Fe/H]". Astronomy & Astrophysics 624: 24. doi:10.1051/0004-6361/201834783. A78. Bibcode: 2019A&A...624A..78D. 
  3. ↑ 3.0 3.1 3.2 Gray, R. O. et al. (October 2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.". The Astronomical Journal 126 (4): 2048–2059. doi:10.1086/378365. Bibcode: 2003AJ....126.2048G. 
  4. ↑ Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey 5. Bibcode: 1999MSS...C05....0H. 
  5. ↑ 5.0 5.1 Soubiran, C. et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics 616: A7. doi:10.1051/0004-6361/201832795. Bibcode: 2018A&A...616A...7S. 
  6. ↑ Gonzalez, Guillermo et al. (1999). "Parent Stars of Extrasolar Planets. IV. 14 Herculis, HD 187123, and HD 210277". The Astrophysical Journal Letters 511 (2): L111–L114. doi:10.1086/311847. Bibcode: 1999ApJ...511L.111G. http://www.iop.org/EJ/article/1538-4357/511/2/L111/985725.html. 
  7. ↑ 7.0 7.1 7.2 Soto, M. G.; Jenkins, J. S. (2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy and Astrophysics 615: A76. doi:10.1051/0004-6361/201731533. Bibcode: 2018A&A...615A..76S. 
  8. ↑ 8.0 8.1 Krivov, A. V.; Eiroa, C.; Löhne, T.; Marshall, J. P.; Montesinos, B.; Del Burgo, C.; Absil, O.; Ardila, D. et al. (2013), "HERSCHEL's "COLD DEBRIS DISKS": BACKGROUND GALAXIES OR QUIESCENT RIMS OF PLANETARY SYSTEMS?", The Astrophysical Journal 772 (1): 32, doi:10.1088/0004-637X/772/1/32, Bibcode: 2013ApJ...772...32K 
  9. ↑ 9.0 9.1 9.2 9.3 Marcy, Geoffrey W. et al. (1999). "Two New Planets in Eccentric Orbits". The Astrophysical Journal 520 (1): 239–247. doi:10.1086/307451. Bibcode: 1999ApJ...520..239M. 
  10. ↑ "HD 210277". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+210277. 
  11. ↑ Cannon, A. J.; Pickering, E. C. (October 1993). "Henry Draper Catalogue and Extension". VizieR On-Line Data Catalog: III/135A. Bibcode: 1993yCat.3135....0C.  Originally published in: Harv. Ann. 91-100 (1918-1924)
  12. ↑ 12.0 12.1 Funk, B.; Schwarz, R.; Süli, Á.; Érdi, B. (July 2012). "On the stability of possible Trojan planets in the habitable zone: an application to the systems HD 147513 and HD 210277". Monthly Notices of the Royal Astronomical Society 423 (4): 3074–3082. doi:10.1111/j.1365-2966.2012.21121.x. Bibcode: 2012MNRAS.423.3074F. 
  13. ↑ Trilling, D. E. et al. (2000). "Circumstellar Dust Disks around Stars with Known Planetary Companions". The Astrophysical Journal 529 (1): 499–505. doi:10.1086/308280. Bibcode: 2000ApJ...529..499T. 
  14. ↑ 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. doi:10.1086/428115. Bibcode: 2005ApJ...622.1160B. 
  15. ↑ Bryden, G. et al. (2009). "Planets and Debris Disks: Results from a Spitzer/MIPS Search for Infrared Excess". The Astrophysical Journal 705 (2): 1226–1236. doi:10.1088/0004-637X/705/2/1226. Bibcode: 2009ApJ...705.1226B. http://authors.library.caltech.edu/16665/1/Bryden2009p6285Astrophys_J.pdf. 
  16. ↑ 16.0 16.1 Eiroa, C. et al. (December 2011). "Herschel discovery of a new class of cold, faint debris discs". Astronomy & Astrophysics 536: L4. doi:10.1051/0004-6361/201117797. Bibcode: 2011A&A...536L...4E. 
  17. ↑ Butler, R. P. et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646 (1): 505–522. doi:10.1086/504701. Bibcode: 2006ApJ...646..505B. 

External links

Coordinates: Sky map 22h 09m 29.8657s, −07° 32′ 55.155″



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