HD 108874

HD 108874

Orbits around the star HD108874
Observation data
Epoch J2000      Equinox J2000
Constellation Coma Berenices
Right ascension 12h 30m 26.882s[1]
Declination +22° 52′ 47.38″[1]
Apparent magnitude (V) 8.76
Characteristics
Spectral type G5 V
B−V color index 0.764
V−R color index 0.4
Variable type ”None”
Astrometry
Radial velocity (Rv)–30.7 km/s
Proper motion (μ) RA: 127.11 ± 0.96[1] mas/yr
Dec.: –89.47 ± 0.84[1] mas/yr
Parallax (π)16.87 ± 0.24[2] mas
Distance193 ± 3 ly
(59.3 ± 0.8 pc)
Absolute magnitude (MV)3.72
Details
Mass1 M☉
Radius1.22 R☉
Luminosity1.14 L☉
Temperature5407 K
Metallicity [Fe/H]0.14 dex
Rotation37.82 days
Age7.26 Gyr
Other designations
BD+23°2466, HIP 61028, SAO 82344
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

HD 108874 is a yellow dwarf star (spectral type G5 V) in the constellation of Coma Berenices. It is 200 light years from Earth[1] and has two extrasolar planets that are possibly in a 4:1 orbital resonance.

Star

HD 108874 is 2.7 billion years older than our Sun. The star has a temperature of 5407 K and luminosity 1.14 solar. Its metallicity is 1.38 times solar, meaning it has greater iron abundance relative to hydrogen and helium. It has about the same mass as the Sun, but the radius is 22% greater.

Planetary system

In 2003, the jovian planet HD 108874 b was discovered by the US-based team Paul Butler, Geoffrey Marcy, Steven Vogt, and Debra Fischer.[3] This planet receives the amount of insolation closest to Earth of any extrasolar planet. In 2005, further observations revealed this star has another jovian planet orbiting further out, designated as HD 108874 c.[4] Those two planets are in a 4:1 orbital resonance. This means if HD 108874 b orbits the star four times, then HD 108874 c orbits only once, because the orbital period for planet c is four times longer than planet b.

The HD 108874 planetary system[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >1.34 ± 0.11 MJ 1.053 ± 0.061 394.48 ± 0.60 0.128 ± 0.022 — —
c >1.064 ± 0.099 MJ 2.77 ± 0.16 1680 ± 24 0.273 ± 0.040 — —

See also

References

  1. 1 2 3 4 5 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.Vizier catalog entry
  2. ↑ Martell, Sarah; Sharma, Sanjib; Buder, Sven; Duong, Ly; Schlesinger, Katharine; Simpson, Jeffrey; Lind, Karin; Ness, Melissa; Marshall, Jonathan; et al. (2016). "The GALAH Survey: Observational Overview and Gaia DR1 companion". 1609: arXiv:1609.02822. arXiv:1609.02822Freely accessible. Bibcode:2016arXiv160902822M.
  3. ↑ Butler, R. Paul; et al. (2003). "Seven New Keck Planets Orbiting G and K Dwarfs". The Astrophysical Journal. 582 (1): 455–466. Bibcode:2003ApJ...582..455B. doi:10.1086/344570.
  4. ↑ Vogt, Steven S.; et al. (2005). "Five New Multicomponent Planetary Systems". The Astrophysical Journal. 632 (1): 638–658. Bibcode:2005ApJ...632..638V. doi:10.1086/432901.
  5. ↑ Wright, J. T.; et al. (2009). "Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems". The Astrophysical Journal. 693 (2): 1084–1099. arXiv:0812.1582Freely accessible. Bibcode:2009ApJ...693.1084W. doi:10.1088/0004-637X/693/2/1084.

Coordinates: 12h 30m 26.8829s, +22° 52′ 47.383″

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