HD 18262

Last updated
HD 18262
Observation data
Epoch J2000       Equinox J2000
Constellation Cetus
Right ascension 02h 56m 13.767s [1]
Declination +08° 22′ 53.62″ [1]
Apparent magnitude  (V)5.963 [1]
Characteristics
Evolutionary stage Subgiant to giant star
Spectral type F6III-IVs [1]
Apparent magnitude  (B)6.431±0.015 [1]
Apparent magnitude  (G)5.861±0.003 [1]
Apparent magnitude  (J)5.134±0.037 [1]
Apparent magnitude  (H)4.934±0.098 [1]
Apparent magnitude  (K)4.845±0.02 [1]
B−V color index 0.437 [2]
Astrometry
Radial velocity (Rv)27.38±0.15 [3]  km/s
Proper motion (μ)RA: 111.39  mas/yr [3]
Dec.: -89.435  mas/yr [3]
Parallax (π)23.1485 ± 0.0873  mas [3]
Distance 142.766  ly
(43.7931  pc) [3]
Absolute magnitude  (MV)2.79 [4]
Details
Mass 1.54±0.03 [5]   M☉
Radius 1.996 [6]   R☉
Luminosity 6.017 [6]   L☉
Surface gravity (log g)4.19 [7]   cgs
Temperature 6404 [6]   K
Metallicity [Fe/H]0.358 [7]   dex
Rotational velocity (v sin i)8.26 [7]  km/s
Age 1.64+0.29
−0.22 [5]   Gyr
Other designations
BD+07 450, Gaia DR2  8810116091022208, Gaia DR3  8810116091022208, HD  18262, HIP  13679, HR  870, SAO  110851, PPM  146068, TIC  387541497, TYC  641-763-1, GSC  00641-00763, IRAS 02535+0810, 2MASS J02561376+0822534, WISE J025613.80+082252.8
Database references
SIMBAD data

HD 18262 (HR 870, HIP 13679) is an F-type giant or subgiant star located in the constellation Cetus. It has an apparent magnitude of 5.963, which makes it faintly visible to the naked eye. According to the Gaia spacecraft, HD 18262 is located at a distance of 43.79 parsecs (142.8 light-years ) and is moving away from Earth at a velocity of 27.4 km/s. Considering the apparent magnitude and the distance, its absolute magnitude is equivalent to 2.79. It belongs to the thin disk population of the Milky Way.

Contents

Characteristics

It is an evolved F-type star that has left the main sequence and is now between a giant star and a subgiant, based on its spectral type of F6III-IVs. [1] [8] The star is 1.54 times more massive than the Sun [5] and has expanded to 2 times its size. [6] It is emitting six times the solar luminosity from its photosphere at an effective temperature of 6,400 K, [6] which is around 630 degrees hotter than the Sun's photosphere. The age of HD 18262 is estimated at 1.64 billion years, [5] equivalent to 36% of the Solar System's age. The star is metal-enriched compared to the Sun, the abundance of iron [ Fe/H ] on its surface is 2.3 higher than that of the Sun, while the oxygen abundance [ O/H ] is 2.9 times higher. [7] [lower-alpha 1] Its B-V color index is 0.437, [2] giving it the yellowish-white color of a F-type star.

The distance to HD 18262, based on information from the Gaia spacecraft, is of 43.79 parsecs (142.8 light-years ). [3] The apparent magnitude of the star is of 5.96 m , [1] which is bright enough to be seen to the naked eye under dark sites, far away from light pollution. [9] The absolute magnitude, i.e. its brightness if it was seen at a distance of 10 parsecs (32.6 ly), is of 2.79. [4] HD 18262 is moving away from Earth at a velocity of 27.38 km/s. [1] It is part of the thin disk population of the Milky Way. [10] Its orbit around the galaxy has a low eccentricity of 0.06 and its distance from the galactic center varies from 7.14 to 8.11 kiloparsecs (23,280 to 26,440 light-years). [11]

No debris disks have been detected around this star as of 2016 [12] and no exoplanets have been detected around it as of 2012. [10] A 2019 study analysed the possibility of HD 18262 hosting a giant planet, in five ensembles, analysing five different compositions. The highest possibity was in the second ensemble, where the planet would be formed by volatiles, lithophiles, and sderophiles. In this case, the possibility is of 23%. [13] HD 18262's habitable zone is located at a mean distance of 2.44 astronomical units from it. [14]

Notes

    1. ↑ from logarithms of 0.358 and 0.46 respectively.

    Related Research Articles

    83 Leonis, abbreviated 83 Leo, is a binary star system approximately 59 light-years away in the constellation of Leo. The primary star of the system is a cool orange subgiant star, while the secondary star is an orange dwarf star. The two stars are separated by at least 515 astronomical units from each other. Both stars are presumed to be cooler than the Sun.

    HD 88133 is a yellow star with an orbiting exoplanet in the equatorial constellation of Leo. It has an apparent visual magnitude of 8.01, which is too faint to be visible to the naked eye. With a small telescope it should be easily visible. The distance to this system, as measured through parallax, is 240 light years, but it is slowly drifting closer with a radial velocity of −3.6 km/s.

    HD 63454, formally named Ceibo, is a star located in the southern circumpolar constellation Chamaeleon near the border with Mensa. To see the star, one needs a small telescope because it has an apparent magnitude of 9.36, which is below the limit for naked eye visibility. The object is located relatively close at a distance of 123 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 33.8 km/s. At its current distance, HD 63454's brightness is diminished by two tenths of a magnitude due to interstellar dust. It has an absolute magnitude of +6.68.

    HD 40979 is a triple star system in the northern constellation of Auriga. The combined brightness of this group lies below the typical limit of visibility to the naked eye at an apparent visual magnitude of 6.74. It is located at a distance of approximately 108 light years from the Sun based on parallax. The system is receding with a radial velocity of +32 km/s. It has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.182″ per year.

    HD 20782 is the primary of a wide binary system located in the southern constellation Fornax. It has an apparent magnitude of 7.38, making it readily visible in binoculars but not to the naked eye. The system is located relatively close at a distance of 117 light-years based on Gaia DR3 parallax measurements, but it is receding with a heliocentric radial velocity of 40.7 km/s. At its current distance, HD 20782's brightness is diminished by 0.12 magnitudes due to interstellar extinction and it has an absolute magnitude of +4.61.

    <span class="mw-page-title-main">HD 136118</span> Star in the constellation Serpens

    HD 136118 is a star in the Serpens Caput section of the Serpens constellation. The star is too dim to be readily visible to the naked eye, having an apparent visual magnitude of 6.93. It is located at a distance of 165 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −3 km/s.

    HD 68988 is a star in the northern constellation of Ursa Major. It has been given the proper name Násti, which means star in the Northern Sami language. The name was selected in the NameExoWorlds campaign by Norway, during the 100th anniversary of the IAU. HD 68988 is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.20. The star is located at a distance of 199 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −69 km/s and is predicted to come as close as 78 light-years in 617,000 years.

    HD 117207 is a star in the southern constellation Centaurus. With an apparent visual magnitude of 7.24, it is too dim to be visible to the naked eye but can be seen with a small telescope. Based upon parallax measurements, it is located at a distance of 105.4 light-years from the Sun. The star is drifting closer with a radial velocity of −17.4 km/s. It has an absolute magnitude of 4.67.

    HD 179079 is a star with an exoplanetary companion in the equatorial constellation of Aquila. It has an apparent visual magnitude of approximately 7.96, making it too faint to be readily visible to the naked eye. The distance to this star can be determine using parallax measurements, which yields an estimate of approximately 228 light years. It is drifting further away with a radial velocity of +20 km/s.

    HD 30562 is a star in the equatorial constellation of Eridanus. It has a golden hue and can be viewed with the naked eye under good seeing conditions, having an apparent visual magnitude of 5.77. The distance to this star is 85 light years based on parallax. It is drifting further away with a high radial velocity of +77 km/s, having come to within 46.8 light-years some 236,000 years ago.

    HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

    <span class="mw-page-title-main">HD 179070</span> Star in the constellation Lyra

    HD 179070, also known as Kepler-21, is a star with a closely orbiting exoplanet in the northern constellation of Lyra. At an apparent visual magnitude of 8.25 this was the brightest star observed by the Kepler spacecraft to host a validated planet until the discovery of an exoplanet orbiting HD 212657 in 2018. This system is located at a distance of 354 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −18.2 km/s.

    HD 99706 is an orange-hued star in the northern circumpolar constellation of Ursa Major. With an apparent visual magnitude of 7.65, it is too dim to be visible to the naked eye but can be viewed with a pair of binoculars. Parallax measurements provide a distance estimate of approximately 480 light years from the Sun, and the Doppler shift shows it is drifting closer with a radial velocity of −30 km/s. It has an absolute magnitude of 2.12, indicating it would be visible to the naked eye as a 2nd magnitude star if it were located 10 parsecs away.

    HD 212771, also named Lionrock, is a solitary star in the southern zodiac constellation Aquarius. It has an apparent magnitude of 7.60, making it readily visible with binoculars but not the naked eye. Parallax measurements place the object at a distance of 364 light years, and is currently receding with a radial velocity of 15 km/s.

    <span class="mw-page-title-main">HD 193307</span> Star in the constellation Telescopium

    HD 193307 is the primary of a binary star located the southern constellation Telescopium. It has an apparent magnitude of 6.27, placing it near the limit for naked eye visibility, even under ideal conditions. The star is located relatively close at a distance of 102 light years based on Gaia DR3 parallax measurements, but it is receding with a heliocentric radial velocity of 16.9 km/s. At its current distance, HD 193307's brightness is diminished by 0.18 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of +3.80. HD 193307 has a relatively high proper motion, moving at a rate of 437 mas/yr.

    HD 194012 is a star in the equatorial constellation Delphinus. It has an apparent magnitude of 6.15, making it visible to the naked eye under ideal conditions. The star is relatively close at a distance of only 85 light years but is receding with a heliocentric radial velocity of 4.5 km/s.

    HD 200779 is a solitary star located in the equatorial constellation Equuleus, the foal. It has an apparent magnitude of 8.27, making it readily visible in binoculars but not to the naked eye. The object is located relatively close at a distance of 49 light years based on Gaia DR3 parallax measurements, and it is approaching rapidly with a heliocentric radial velocity of −67 km/s. It is classified as a high proper motion star, with a total proper motion of 569 mas/yr.

    <span class="mw-page-title-main">HD 10390</span> B-type main-sequence star; Triangulum

    HD 10390 is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a bluish-white hued point of light with an apparent magnitude of 5.64. The object is located relatively close at a distance of 292 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −1.9 km/s. At its current distance, HD 10390's brightness is diminished by an interstellar extinction of only five-hundredths of a magnitude and it has an absolute magnitude of +1.00.

    HD 37320 is a star located in the constellation Orion. It is an evolved blue giant star, based on its spectral type of B8III. The distance to HD 37320 is calculated at 285.5 parsecs, based on a parallax from Gaia EDR3. The apparent magnitude of the star is 5.852, which is above the limiting magnitude for naked-eye vision (6.5m), making it faintly visible to the naked eye.

    HD 85945 is a star in the constellation Ursa Major. It is a yellow giant star with a spectral type of G6III:Fe-0.5. Based on information from Gaia DR3, it is located 132.54 parsecs (432.3 ly) from Earth and is moving towards Earth at a velocity of 47 km/s. It has an apparent magnitude of 5.96, which makes it faintly visible to the naked eye.

    References

    1. 1 2 3 4 5 6 7 8 9 10 11 12 "HD 18262". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved May 8, 2024.
    2. 1 2 Isaacson, Howard; Fischer, Debra (2010-12-01). "Chromospheric Activity and Jitter Measurements for 2630 Stars on the California Planet Search". The Astrophysical Journal. 725 (1): 875–885. arXiv: 1009.2301 . Bibcode:2010ApJ...725..875I. doi:10.1088/0004-637X/725/1/875. ISSN   0004-637X. Data about this star is avaliable here at VizieR.
    3. 1 2 3 4 5 6 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 .
    4. 1 2 Ford, Dominic. "HIP-13679 (Star)". In-The-Sky.org. Retrieved 2024-05-08.
    5. 1 2 3 4 Aguilera-Gómez, Claudia; Ramírez, Iván; Chanamé, Julio (2018-06-01). "Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert". Astronomy and Astrophysics. 614: A55. arXiv: 1803.05922 . Bibcode:2018A&A...614A..55A. doi:10.1051/0004-6361/201732209. ISSN   0004-6361. Data about this star is avaliable here at VizieR.
    6. 1 2 3 4 5 Schofield, Mathew; Chaplin, William J.; Huber, Daniel; Campante, Tiago L.; Davies, Guy R.; Miglio, Andrea; Ball, Warrick H.; Appourchaux, Thierry; Basu, Sarbani; Bedding, Timothy R.; Christensen-Dalsgaard, Jørgen; Creevey, Orlagh; García, Rafael A.; Handberg, Rasmus; Kawaler, Steven D. (2019-03-01). "The Asteroseismic Target List for Solar-like Oscillators Observed in 2 minute Cadence with the Transiting Exoplanet Survey Satellite". The Astrophysical Journal Supplement Series. 241 (1): 12. arXiv: 1901.10148 . Bibcode:2019ApJS..241...12S. doi: 10.3847/1538-4365/ab04f5 . ISSN   0067-0049. Data about this star is avaliable here at VizieR.
    7. 1 2 3 4 Rice, Malena; Brewer, John M. (2020-08-01). "Stellar Characterization of Keck HIRES Spectra with The Cannon". The Astrophysical Journal. 898 (2): 119. arXiv: 2007.02942 . Bibcode:2020ApJ...898..119R. doi: 10.3847/1538-4357/ab9f96 . ISSN   0004-637X. Data about this star is avaliable here at VizieR.
    8. ↑ "The Classification of Stellar Spectra". www.star.ucl.ac.uk. Retrieved 2024-05-08.
    9. ↑ "Determining the Limiting Magnitude – Saguaro Astronomy Club". www.saguaroastro.org. Retrieved 2024-05-08.
    10. 1 2 Ramírez, I.; Fish, J. R.; Lambert, D. L.; Allende Prieto, C. (2012-09-01). "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets". The Astrophysical Journal. 756 (1): 46. arXiv: 1207.0499 . Bibcode:2012ApJ...756...46R. doi:10.1088/0004-637X/756/1/46. hdl:2152/34872. ISSN   0004-637X. Data about this star is avaliable here at VizieR.
    11. ↑ Casagrande, L.; Schönrich, R.; Asplund, M.; Cassisi, S.; Ramírez, I.; Meléndez, J.; Bensby, T.; Feltzing, S. (2011-06-01). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey". Astronomy and Astrophysics. 530: A138. arXiv: 1103.4651 . Bibcode:2011A&A...530A.138C. doi:10.1051/0004-6361/201016276. ISSN   0004-6361. Data about this star is avaliable here at VizieR.
    12. ↑ Gáspár, András; Rieke, George H.; Ballering, Nicholas (2016-08-01). "The Correlation between Metallicity and Debris Disk Mass". The Astrophysical Journal. 826 (2): 171. arXiv: 1604.07403 . Bibcode:2016ApJ...826..171G. doi: 10.3847/0004-637X/826/2/171 . ISSN   0004-637X. Data about this star is avaliable here at VizieR.
    13. ↑ Hinkel, Natalie R.; Unterborn, Cayman; Kane, Stephen R.; Somers, Garrett; Galvez, Richard (2019-07-01). "A Recommendation Algorithm to Predict Giant Exoplanet Host Stars Using Stellar Elemental Abundances". The Astrophysical Journal. 880 (1): 49. arXiv: 1805.12144 . Bibcode:2019ApJ...880...49H. doi: 10.3847/1538-4357/ab27c0 . ISSN   0004-637X. Data about this star is avaliable here at VizieR.
    14. ↑ Reiners, Ansgar; Zechmeister, Mathias (2020-03-01). "Radial Velocity Photon Limits for the Dwarf Stars of Spectral Classes F-M". The Astrophysical Journal Supplement Series. 247 (1): 11. arXiv: 1912.04120 . Bibcode:2020ApJS..247...11R. doi: 10.3847/1538-4365/ab609f . ISSN   0067-0049. Data about this star is avaliable here at VizieR.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.