Summary
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]
| 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] |
| Distance | 137.1 ± 0.1 ly (42.02 ± 0.04 pc) |
| Absolute magnitude (MV) | 4.44±0.12[2] |
| Position (relative to HD 222582A)[5] | |
| Component | HD 222582B |
| Epoch of observation | 2018 |
| Angular distance | 109.56±0.18″ |
| Position angle | 299.52±0.03° |
| Projected separation | 4637±59 AU AU |
| Details | |
| A | |
| Mass | 0.993±0.035[7] M☉ |
| Radius | 1.137±0.017[7] R☉ |
| Luminosity | 1.302+0.005 −0.004[8] L☉ |
| Surface gravity (log g) | 4.370±0.009[4] cgs |
| Temperature | 5,790±3[4] K |
| Metallicity [Fe/H] | −0.005±0.003[4] dex |
| Rotational velocity (v sin i) | 1.74±0.12[9] km/s |
| Age | 6.7±0.3[4] Gyr |
| Ba+Bb | |
| Mass | 0.2[10] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Planet | |
| HD 222582 b | Data 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.[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 edit
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]
| 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 edit
References edit
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ a b "HD 222582". Open Exoplanet Catalogue. Retrieved 2020-12-31.
- ^ "HD 222582". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-31.
- ^ "The astronomical magnitude scale". International Comet Quarterly. Retrieved 2020-12-31.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
- ^ 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.
- ^ "HD 222582 b". Exoplanet Catalogue. NASA Astrophysics Division. Retrieved 2020-12-31.
External links edit
- "HD 222582 Image". Simbad.