Langbahn Team – Weltmeisterschaft

HD 222582

HD 222582
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 23h 41m 51.5301s[1]
Declination –05° 59′ 08.729″[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: −145.492(29) mas/yr[1]
Dec.: −111.458(21) mas/yr[1]
Parallax (π)23.7955 ± 0.0238 mas[1]
Distance137.1 ± 0.1 ly
(42.02 ± 0.04 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°
Projected separation4637±59 AU AU
Details
A
Mass0.993±0.035[7] M☉
Radius1.137±0.017[7] R☉
Luminosity1.302+0.005
−0.004[8] 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[9] km/s
Age6.7±0.3[4] Gyr
Ba+Bb
Mass0.2[10] M☉
Other designations
BD−06°6262, GC 32912, HD 222582, HIP 116906, SAO 146849, WDS J23419-0559A, NLTT 57682, 2MASS J23415154-0559086[11]
Database references
SIMBADdata
Planet
HD 222582 b Data Simbad
Data ExoPlanet

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.[12] The system is located at a distance of 137 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.[13]

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.[14][4] It is about 6.5[9] billion years old with an inactive chromosphere[14] and is spinning with a low projected rotational velocity of 1.7 km/s.[9] 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[15][16] 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.[10]

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.[17][18]

The HD 222582 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 8.37[19] MJ 1.35 572 0.76 — —

See also

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c 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. ^ a b 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. ^ a b c d e f g h 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. ^ a b c 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. ^ a b 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. ^ a b c 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. S2CID 119107228. A76.
  8. ^ 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.
  9. ^ a b c 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.
  10. ^ a b "HD 222582". Open Exoplanet Catalogue. Retrieved 2020-12-31.
  11. ^ "HD 222582". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-31.
  12. ^ "The astronomical magnitude scale". International Comet Quarterly. Retrieved 2020-12-31.
  13. ^ 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.
  14. ^ a b 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.
  15. ^ 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.
  16. ^ 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.
  17. ^ "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
  18. ^ 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.
  19. ^ "HD 222582 b". Exoplanet Catalogue. NASA Astrophysics Division. Retrieved 2020-12-31.


Quelle: https://en.wikipedia.org/wiki/HD_222582