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Revision as of 22:32, 31 December 2017 by Mike s (talk | contribs) (update orbitbox and add ref)(diff) ← Previous revision | Latest revision (diff) | Newer revision → (diff) Orbits around the star HD108874 | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Coma Berenices |
| Right ascension | 12 30 26.882 |
| Declination | +22° 52′ 47.38″ |
| 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 mas/yr Dec.: –89.47 ± 0.84 mas/yr |
| Parallax (π) | 16.87 ± 0.24 mas |
| Distance | 193 ± 3 ly (59.3 ± 0.8 pc) |
| Absolute magnitude (MV) | 3.72 |
| Details | |
| Mass | 1 M☉ |
| Radius | 1.22 R☉ |
| Luminosity | 1.14 L☉ |
| Temperature | 5407 K |
| Metallicity | 0.18 dex |
| Rotation | 37.82 days |
| Age | 7.26 Gyr |
| Other designations | |
| BD+23°2466, HIP 61028, SAO 82344 | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | 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 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 lead by Paul Butler, Geoffrey Marcy, Steven Vogt, and Debra Fischer. A total of 20 radial velocity observations, obtained at the W. M. Keck Observatory between 1999 and 2002, were used to make the discovery. In 2005, further observations revealed this star has another jovian planet orbiting further out, designated as HD 108874 c. The orbital parameters of both planets were updated in 2009 with additional observations. 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.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.25±0.10 MJ | 1.05±0.02 | 395.34±0.19 | 0.142±0.011 | — | — |
| c | >1.09±0.16 MJ | 2.81±0.06 | 1732.2±9.8 | 0.229±0.032 | — | — |
See also
References
- ^ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.Vizier catalog entry
- Martell, Sarah; et al. (2016). "The GALAH Survey: Observational Overview and Gaia DR1 companion". Monthly Notices of the Royal Astronomical Society. 465 (3): 3203. arXiv:1609.02822. Bibcode:2017MNRAS.465.3203M. doi:10.1093/mnras/stw2835.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ 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.
- 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.
- 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:0812.1582. Bibcode:2009ApJ...693.1084W. doi:10.1088/0004-637X/693/2/1084.
- Benatti, S.; et al. (2017). "The GAPS Programme with HARPS-N at TNG. XII. Characterization of the planetary system around HD 108874". Astronomy and Astrophysics. 599. A90. arXiv:1611.09873. Bibcode:2017A&A...599A..90B. doi:10.1051/0004-6361/201629484.
External links
- Extrasolar Planet Interactions by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
