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HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7,[2] but can be viewed with binoculars or a small telescope.[11] The system is located at a distance of 138 light years from the Sun based on parallax,[1] and it is drifting further away with a radial velocity of +12 km/s.[6] It is located close enough to the ecliptic that it is subject to lunar occultations.[12]

HD 222582
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 23h 41m 51.52300s[1]
Declination –05° 59′ 08.7315″[1]
Apparent magnitude (V) 7.685±0.005[2]
Characteristics
HD 222582A
Evolutionary stage Main sequence
Spectral type G5V[3]
B−V color index 0.648±0.002[4]
HD 222582B
Spectral type M4.5V[5]
Astrometry
Radial velocity (Rv)+12.020±0.0004[6] km/s
Proper motion (μ) RA: −145.401[1] mas/yr
Dec.: −111.296[1] mas/yr
Parallax (π)23.6913 ± 0.0606 mas[1]
Distance137.7 ± 0.4 ly
(42.2 ± 0.1 pc)
Absolute magnitude (MV)4.44±0.12[2]
Position (relative to HD 222582A)[5]
ComponentHD 222582B
Epoch of observation2018
Angular distance109.56±0.18″
Position angle299.52±0.03°
Observed separation
(projected)		4637±59 AU AU
Details
A
Mass0.993±0.035[7] M☉
Radius1.137±0.017[7] R☉
Luminosity1.302+0.005
−0.004[1] L☉
Surface gravity (log g)4.370±0.009[4] cgs
Temperature5,790±3[4] K
Metallicity [Fe/H]−0.005±0.003[4] dex
Rotational velocity (v sin i)1.74±0.12[8] km/s
Age6.7±0.3[4] Gyr
Ba+Bb
Mass0.2[9] M☉
Other designations
BD−06°6262, GC 32912, HD 222582, HIP 116906, SAO 146849, WDS J23419-0559A, NLTT 57682, 2MASS J23415154-0559086[10]
Database references
SIMBADdata
Planet
HD 222582 bData Simbad
Data ExoPlanet

The primary member of this system, designated component A, is an ordinary G-type main-sequence star with a stellar classification of G5V.[3] The physical properties of the star are similar enough to the Sun that it is considered a candidate solar twin.[13][4] It is about 6.5[8] billion years old with an inactive chromosphere[13] and is spinning with a low projected rotational velocity of 1.7 km/s.[8] The mass[7] and metallicity[4] of this star are essentially the same as the Sun. It has a 14% larger radius and is radiating 1.3 times the luminosity of the Sun from its photosphere at an effective temperature of 5,790 K.[4]

Component B of this system is a close binary[14][15] system with the components designated HD 222582 Ba and Bb. The pair have a combined class of M4.5 V+[5] and about 20% the mass of the Sun.[9]


Planetary system


In November 1999, a dense superjovian planet was announced orbiting the primary by the California and Carnegie Planet Search. Designated component 'b', it was discovered using the radial velocity method, using 24 observations over a period of 1.5 years. The exoplanet is orbiting with a period of 1.57 years and a very large eccentricity of 0.76, ranging in distance from 0.39 AU out to 2.31 AU away from the primary.[16][17]

The HD 222582 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 8.37[18] MJ 1.35 572 0.76 — —

See also



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. Fuhrmann, Klaus (February 2008). "Nearby stars of the Galactic disc and halo - IV". Monthly Notices of the Royal Astronomical Society. 384 (1): 173–224. Bibcode:2008MNRAS.384..173F. doi:10.1111/j.1365-2966.2007.12671.x.
  3. Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  4. Lorenzo-Oliveira, Diego; et al. (November 2018). "The Solar Twin Planet Search. The age-chromospheric activity relation". Astronomy & Astrophysics. 619: 10. arXiv:1806.08014. Bibcode:2018A&A...619A..73L. doi:10.1051/0004-6361/201629294. S2CID 118995412. A73.
  5. Montes, D.; et al. (September 2018). "Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries - I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics". Monthly Notices of the Royal Astronomical Society. 479 (1): 1332–1382. arXiv:1805.05394. Bibcode:2018MNRAS.479.1332M. doi:10.1093/mnras/sty1295. S2CID 119260219.
  6. 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.
  7. Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics. 615: 28. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. A76.
  8. dos Santos, Leonardo A.; et al. (August 2016). "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars". Astronomy & Astrophysics. 592: 8. arXiv:1606.06214. Bibcode:2016A&A...592A.156D. doi:10.1051/0004-6361/201628558. S2CID 53533614. A156.
  9. "HD 222582". Open Exoplanet Catalogue. Retrieved 2020-12-31.
  10. "HD 222582". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-31.
  11. "The astronomical magnitude scale". International Comet Quarterly. Retrieved 2020-12-31.
  12. Richichi, A. (January 2003). "Lunar occultations of stars with exoplanet candidates". Astronomy and Astrophysics. 397 (3): 1123–1127. Bibcode:2003A&A...397.1123R. doi:10.1051/0004-6361:20021585.
  13. Reddy, Arumalla B. S.; Lambert, David L. (August 2017). "Solar Twins and the Barium Puzzle". The Astrophysical Journal. 845 (2): 14. arXiv:1707.07051. Bibcode:2017ApJ...845..151R. doi:10.3847/1538-4357/aa81d6. S2CID 119232784. 151.
  14. Riddle, Reed L.; et al. (2015). "A Survey of the High Order Multiplicity of Nearby Solar-type Binary Stars with Robo-AO". The Astrophysical Journal. 799 (1). 4. arXiv:1411.0682. Bibcode:2015ApJ...799....4R. doi:10.1088/0004-637X/799/1/4. S2CID 5642378.
  15. Raghavan, Deepak; et al. (2006). "Two Suns in the Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal. 646 (1): 523–542. arXiv:astro-ph/0603836. Bibcode:2006ApJ...646..523R. doi:10.1086/504823. S2CID 5669768.
  16. "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
  17. Vogt, Steven S.; et al. (2000). "Six New Planets from the Keck Precision Velocity Survey". The Astrophysical Journal. 536 (2): 902–914. arXiv:astro-ph/9911506. Bibcode:2000ApJ...536..902V. doi:10.1086/308981. S2CID 119375519.
  18. "HD 222582 b". Exoplanet Catalogue. NASA Astrophysics Division. Retrieved 2020-12-31.



На других языках

[de] HD 222582

HD 222582 ist ein Stern im Sternbild Aquarius, welcher von der Erde etwa 42 Parsec (ca. 136 Lichtjahre) entfernt ist. Bereits 1999 wurde von Vogt et al. mit Hilfe der Radialgeschwindigkeitsmethode ein substellarer Begleiter entdeckt, der die Bezeichnung HD 222582 b erhielt und bei dem es sich um einen Exoplaneten-Kandidaten handelt.
- [en] HD 222582


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