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HD 35759

From Wikipedia, the free encyclopedia
Star in the constellation Camelopardlis
HD 35759
Observation data
Epoch J2000      Equinox J2000
ConstellationCamelopardalis[1]
Right ascension05h 31m 33.349s[2]
Declination+64° 19′ 07.59″[2]
Apparent magnitude (V)7.74±0.01[3]
Characteristics
Evolutionary stagesubgiant[2]
Spectral typeG0[4]
B−Vcolor index0.602±0.015[1]
Astrometry
Radial velocity (Rv)−12.620±0.0025[5] km/s
Proper motion (μ)RA: −29.318mas/yr[2]
Dec.: −92.726mas/yr[2]
Parallax (π)14.0772±0.0217 mas[2]
Distance231.7 ± 0.4 ly
(71.0 ± 0.1 pc)
Absolute magnitude (MV)3.45[1]
Details
Mass1.15±0.08[6] M
Radius1.76+0.06
−0.04
[5] R
Luminosity3.445+0.015
−-0.014
[5] L
Surface gravity (log g)4.0159+0.0740
−0.0818
[7] cgs
Temperature5,927+67
−93
[5] K
Metallicity[Fe/H]0.04±0.02[8] dex
Rotational velocity (v sin i)3[9] km/s
Age4.2[10] Gyr
Other designations
BD+64 532,HD 35759,HIP 25883,SAO 13524,WDS J05316+6419A[11]
Database references
SIMBADdata
Exoplanet Archivedata

HD 35759 is astar with an orbitingexoplanet located in the circumpolar constellationCamelopardalis. With an apparent magnitude of 7.74, it's impossible to see with theunaided eye, but can be seen with binoculars. The distance to this system is 232 light years based onparallax measurements,[2] and it is drifting closer with a heliocentricradial velocity of −12.6 km/s.[5]

This is aG-type star with 15% more mass than theSun, but has 1.76 times the radius. It radiates at about 3solar luminosities, and has aneffective temperature of 5,927K, which gives it a yellow hue. HD 35759 is slightly enriched in metals, with having 9.6% more iron abundance than the Sun. Like many older G-type stars, HD 35759 rotates rather slowly, with aprojected rotational velocity of 3 km/s.

Planetary System

[edit]

In 2016, asuper-jovian exoplanet was discovered orbiting the star on aneccentric orbit. Since the planet was discovered usingdoppler spectroscopy, its radius and true mass is unknown.

The HD 35759 planetary system[8]
Companion
(in order from star)
MassSemimajor axis
(AU)
Orbital period
(days)
EccentricityInclinationRadius
b≥ 3.76±0.17 MJ0.389±0.0982.467±0.0190.389±0.006

References

[edit]
  1. ^abcAnderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38 (5): 331.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015. XHIP record for this object atVizieR.
  2. ^abcdefVallenari, 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 atVizieR.
  3. ^Høg, E.; et al. (2000-03-01). "The Tycho-2 catalogue of the 2.5 million brightest stars".Astronomy and Astrophysics.355:L27–L30.Bibcode:2000A&A...355L..27H.ISSN 0004-6361.
  4. ^Cannon, A. J.; Pickering, E. C. (1993-10-01). "VizieR Online Data Catalog: Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989)".VizieR Online Data Catalog.3135.Bibcode:1993yCat.3135....0C.
  5. ^abcdeBrown, 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. 287622247440034688 Gaia DR2 record for this source atVizieR.
  6. ^Winter, Andrew J.; et al. (2020-10-01)."Stellar clustering shapes the architecture of planetary systems".Nature.586 (7830):528–532.arXiv:2010.10531.Bibcode:2020Natur.586..528W.doi:10.1038/s41586-020-2800-0.ISSN 0028-0836.PMC 7116760.PMID 33087913.
  7. ^Stassun, Keivan G.; et al. (2019-10-01)."The Revised TESS Input Catalog and Candidate Target List".The Astronomical Journal.158 (4): 138.arXiv:1905.10694.Bibcode:2019AJ....158..138S.doi:10.3847/1538-3881/ab3467.hdl:1721.1/124721.ISSN 0004-6256.S2CID 166227927.
  8. ^abHébrard, Guillaume; et al. (2016-04-01). "The SOPHIE search for northern extrasolar planets. X. Detection and characterization of giant planets by the dozen".Astronomy and Astrophysics.588: A145.arXiv:1602.04622.Bibcode:2016A&A...588A.145H.doi:10.1051/0004-6361/201527585.ISSN 0004-6361.S2CID 55138055.
  9. ^Nordström, B.; et al. (2004-05-01). "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14 000 F and G dwarfs".Astronomy and Astrophysics.418:989–1019.arXiv:astro-ph/0405198.Bibcode:2004A&A...418..989N.doi:10.1051/0004-6361:20035959.ISSN 0004-6361.S2CID 11027621.
  10. ^Casagrande, L.; et al. (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.S2CID 56118016.
  11. ^"HD 35759".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2023-12-15.
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