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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 69.5 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −20.9 km/s.[5]

HD 210277
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 22h 09m 29.86572s[1]
Declination −07° 32′ 55.1630″[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: 85.462[1] mas/yr
Dec.: −450.544[1] mas/yr
Parallax (π)46.9229 ± 0.0481 mas[1]
Distance69.51 ± 0.07 ly
(21.31 ± 0.02 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, GCRV 13920, 2MASS J22092985-0732548[10]
Database references
SIMBADdata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

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 — —

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. 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. arXiv:1902.02127. Bibcode:2019A&A...624A..78D. doi:10.1051/0004-6361/201834783. S2CID 90259810. A78.
  3. 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. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID 119417105.
  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. Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
  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. Bibcode:1999ApJ...511L.111G. doi:10.1086/311847.
  7. 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. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533.
  8. Krivov, A. V.; Eiroa, C.; Löhne, T.; Marshall, J. P.; Montesinos, B.; Del Burgo, C.; Absil, O.; Ardila, D.; Augereau, J.-C.; Bayo, A.; Bryden, G.; Danchi, W.; Ertel, S.; Lebreton, J.; Liseau, R.; Mora, A.; Mustill, A. J.; Mutschke, H.; Neuhäuser, R.; Pilbratt, G. L.; Roberge, A.; Schmidt, T. O. B.; Stapelfeldt, K. R.; Thébault, Ph.; Vitense, Ch.; White, G. J.; Wolf, S. (2013), "HERSCHEL's "COLD DEBRIS DISKS": BACKGROUND GALAXIES OR QUIESCENT RIMS OF PLANETARY SYSTEMS?", The Astrophysical Journal, 772: 32, arXiv:1306.2855, doi:10.1088/0004-637X/772/1/32, S2CID 11877636
  9. 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. S2CID 16827678.
  10. "HD 210277". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-29.
  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. 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. Bibcode:2012MNRAS.423.3074F. doi:10.1111/j.1365-2966.2012.21121.x.
  13. 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.
  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. arXiv:astro-ph/0412265. Bibcode:2005ApJ...622.1160B. doi:10.1086/428115. S2CID 6633656.
  15. 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.
  16. Eiroa, C.; et al. (December 2011). "Herschel discovery of a new class of cold, faint debris discs". Astronomy & Astrophysics. 536: L4. arXiv:1110.4826. Bibcode:2011A&A...536L...4E. doi:10.1051/0004-6361/201117797. S2CID 14234038.
  17. 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. S2CID 119067572.



На других языках

[de] HD 210277

HD 210277 ist ein Stern der Helligkeit 7 mag im Sternbild Wassermann. Der gelbe Zwergstern vom Spektraltyp G0V ähnelt in seiner Größe, Leuchtkraft und Durchmesser unserer Sonne. Das Alter von HD 210277 beträgt schätzungsweise 12 Milliarden Jahre[1] (die Sonne ist weniger als 5 Milliarden Jahre alt). Aufgrund seiner Entfernung vom Sonnensystem von 69 Lichtjahren ist der Stern nur mit Teleskopen und Ferngläsern sichtbar. 1998 wurde spektroskopisch ein Begleiter entdeckt, der den Stern in einer Entfernung von 1,138 ± 0,066 AU umkreist und die systematische Bezeichnung HD 210277 b trägt.
- [en] HD 210277

[es] HD 210277

HD 210277 es una estrella de magnitud 7 en la constelación Acuario. Es una enana amarilla del tipo G0V, similar al Sol. Posee una masa de aproximadamente 0,92 masas solares, y se estima que la edad de la estrella es de 12 mil millones de años. La estrella no es visible a siemple vista, ya que se encuentra a 69 años luz de la Tierra. Sin embargo, es fácilmente visible con unos prismáticos.

[ru] HD 210277

HD 210277 — одиночная звезда в созвездии Водолея на расстоянии приблизительно 69,5 световых лет (около 21,3 парсеков) от Солнца. Видимая звёздная величина звезды — +8,57m[2]. Возраст звезды оценивается как около 6,93 млрд лет[7].


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