HD 89307

In the world of HD 89307, there has always been great interest and curiosity on the part of society. For centuries, HD 89307 has been a topic of debate and discussion in different areas, whether in politics, science, culture or everyday life. The influence of HD 89307 is undeniable and its impact has been felt in all spheres of human life. In this article, we will thoroughly explore the role of HD 89307 in history and its relevance in the present, analyzing its different aspects and delving into its importance to better understand the world around us.

HD 89307
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Leo
Right ascension 10h 18m 21.28771s[1]
Declination +12° 37′ 15.9909″[1]
Apparent magnitude (V) 7.02[2]
Characteristics
Spectral type G0V[3]
B−V color index 0.594±0.003[2]
Astrometry
Radial velocity (Rv)+23.27±0.13[1] km/s
Proper motion (μ) RA: −272.659 mas/yr[1]
Dec.: −39.333 mas/yr[1]
Parallax (π)31.4134±0.0226 mas[1]
Distance103.83 ± 0.07 ly
(31.83 ± 0.02 pc)
Absolute magnitude (MV)4.57[4]
Details[4]
Mass1.028±0.04 M☉
Radius1.08+0.01
−0.02[5] R☉
Luminosity1.354±0.003[5] L☉
Surface gravity (log g)4.414±0.10 cgs
Temperature5,950±44 K
Metallicity −0.15±0.02[2] dex
Rotation23.7 d
Rotational velocity (v sin i)3.21±0.50 km/s
Age5.3+2.7
−2.9 Gyr[2]
6.76[4] Gyr
Other designations
BD+13 2237, GC 14140, HD 1835, HIP 50473, SAO 99049, PPM 127289[6]
Database references
SIMBADdata

HD 89307 is a star in the equatorial constellation of Leo. It is too faint to be viewed with the naked eye except under ideal conditions, having an apparent visual magnitude of 7.02.[2] The star is located at a distance of 104 light-years (32 parsecs) from the Sun based on parallax, and is drifting further away with a radial velocity of +23 km/s.[1]

This is an ordinary G-type main-sequence star with a stellar classification of G0V.[3] It is chromospherically inactive and appears older than the Sun with a rotation period of 23.7 days.[4] The star has about the same mass[4] as the Sun and is 8% larger. It is radiating 1.35[5] times the Sun's luminosity from its photosphere at an effective temperature of 5,950 K.[4]

Planetary system

In December 2004, using the radial velocity method, it was found to have a long-period giant planet in orbit around it.[4] The parameters of HD 89307 b were updated in 2012,[7] and in 2023 its inclination and true mass were determined via astrometry.[8]

The HD 89307 planetary system[8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(years) 		Eccentricity Inclination Radius
b 2.02+0.27
−0.15 MJ 		3.331+0.052
−0.053 		5.991+0.081
−0.078 		0.174+0.041
−0.043 		72+13
−15 or 108+15
−13° 		—

See also

References

  1. ^ a b c d e f 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 d e Anderson, 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. S2CID 119257644.
  3. ^ a b Harlan, E. A. (September 1969). "MK classifications for F- and G-type stars. I". Astronomical Journal. 74: 916–919. Bibcode:1969AJ.....74..916H. doi:10.1086/110881.
  4. ^ a b c d e f g Fischer, Debra; et al. (2009). "Five planets and an independent confirmation of HD 196885 Ab from Lick Observatory". The Astrophysical Journal. 703 (2): 1545–1556. arXiv:0908.1596. Bibcode:2009ApJ...703.1545F. doi:10.1088/0004-637X/703/2/1545. S2CID 15524804.
  5. ^ a b c 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.
  6. ^ "9 Cet". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-03-27.
  7. ^ Boisse, Isabelle; Pepe, Francesco; Perrier, Christian; Queloz, Didier; Bonfils, Xavier; Bouchy, François; Santos, Nuno C.; Arnold, Luc; Beuzit, Jean-Luc; Dìaz, Rodrigo F.; Delfosse, Xavier; Eggenberger, Anne; Ehrenreich, David; Forveille, Thierry; Hébrard, Guillaume; Lagrange, Anne-Marie; Lovis, Christophe; Mayor, Michel; Moutou, Claire; Naef, Dominique; Santerne, Alexandre; Ségransan, Damien; Sivan, Jean-Pierre; Udry, Stéphane (2012), "The SOPHIE search for northern extrasolar planets V. Follow-up of ELODIE candidates: Jupiter-analogs around Sun-like stars", Astronomy and Astrophysics, 545: A55, arXiv:1205.5835, Bibcode:2012A&A...545A..55B, doi:10.1051/0004-6361/201118419, S2CID 119109836
  8. ^ a b Xiao, Guang-Yao; Liu, Yu-Juan; et al. (March 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics. 23 (5). arXiv:2303.12409. Bibcode:2023RAA....23e5022X. doi:10.1088/1674-4527/accb7e.