French
DeutschHIP 14810
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aries |
| Right ascension | 03h 11m 14.2302s[1] |
| Declination | +21° 05′ 50.4927″[1] |
| Apparent magnitude (V) | 8.585±0.016[2] |
| Characteristics | |
| Spectral type | G6V[2] |
| B−V color index | 0.777±0.021[3] |
| Astrometry | |
| Radial velocity (Rv) | −5.121±0.681[2] km/s |
| Proper motion (μ) | RA: −3.784±0.087[1] mas/yr Dec.: −53.154±0.070[1] mas/yr |
| Parallax (π) | 19.7810 ± 0.0449 mas[1] |
| Distance | 164.9 ± 0.4 ly (50.6 ± 0.1 pc) |
| Absolute magnitude (MV) | 4.89[3] |
| Details | |
| Mass | 0.98±0.02 M☉[4] M☉ |
| Radius | 1.08±0.03[4] R☉ |
| Luminosity | 0.99±0.01[4] L☉ |
| Surface gravity (log g) | 4.35±0.03[4] cgs |
| Temperature | 5,535±51[4] K |
| Metallicity [Fe/H] | 0.28±0.06[2] dex |
| Rotational velocity (v sin i) | 0.54±0.5[5] km/s |
| Age | 8.7±2.0 Gyr[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HIP 14810 is a star with three exoplanetary companions in the northern constellation of Aries. It positioned about 1.3° to the north of Delta Arietis,[7] but is too faint to be visible to the naked eye with an apparent visual magnitude of 8.6.[2] The system is located at a distance of 165 light-years from the Sun based on parallax measurements,[1] but is drifting closer with a radial velocity of −5 km/s.[2]
This is an ordinary G-type main-sequence star with a stellar classification of G6V.[2] It has a relatively low activity level and a low projected rotational velocity of 0.5 km/s, which indicates it is an old star with an age of around eight billion years.[5] The star has a high metallicity with a mass and luminosity about the same as the Sun.[4]
Planetary system
[edit]Orbiting the star are three confirmed planets. The discovery paper for HIP 14810 b and HIP 14810 c was published in 2007,[8] while that for HIP 14810 d was published in 2009, together with a revision for the orbital parameters for planet c.[5] Simulations suggest that the orbits of these planets do not allow a stable orbit for a hypothetical super-earth in the habitable zone.[9]
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥3.9±0.49 MJ | 0.0696±0.0044 | 6.673892±0.000008 | 0.14399±0.00087 | — | — |
| c | ≥1.31±0.18 MJ | 0.549±0.034 | 147.747±0.029 | 0.1566±0.0099 | — | — |
| d | ≥0.59±0.1 MJ | 1.94±0.13 | 981.8±6.9 | 0.185±0.035 | — | — |
See also
[edit]References
[edit]- ^ a b c d e f 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.
- ^ a b c d e f g Grieves, N.; et al. (December 2018). "Chemo-kinematics of the Milky Way from the SDSS-III MARVELS survey". Monthly Notices of the Royal Astronomical Society. 481 (3): 3244–3265. arXiv:1803.11538. Bibcode:2018MNRAS.481.3244G. doi:10.1093/mnras/sty2431.
- ^ a b 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.
- ^ a b c d e f g Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
- ^ a b c Wright, J. T.; et al. (2009). "A Third Giant Planet Orbiting HIP 14810". The Astrophysical Journal Letters. 699 (2): L97–L101. arXiv:0906.0567. Bibcode:2009ApJ...699L..97W. doi:10.1088/0004-637X/699/2/L97. S2CID 8075527.
- ^ "BD+20 518". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-07.
- ^ Sinnott, Roger W.; Perryman, Michael A. C. (1997). Millennium Star Atlas. Vol. 1. Sky Publishing Corporation and the European Space Agency. p. 189. ISBN 0-933346-84-0.
- ^ Wright, J. T.; et al. (2007). "Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars". The Astrophysical Journal. 657 (1): 533–545. arXiv:astro-ph/0611658. Bibcode:2007ApJ...657..533W. doi:10.1086/510553. S2CID 35682784.
- ^ Elser, S.; et al. (August 2013). "Super-Earths and dynamical stability of planetary systems: first parallel GPU simulations using GENGA". Monthly Notices of the Royal Astronomical Society. 433 (3): 2194–2205. arXiv:1305.4070. Bibcode:2013MNRAS.433.2194E. doi:10.1093/mnras/stt883.
- ^ Ment, Kristo; et al. (2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5). 213. arXiv:1809.01228. Bibcode:2018AJ....156..213M. doi:10.3847/1538-3881/aae1f5. S2CID 119243619.
External links
[edit]- Extrasolar Planet Interactions Archived 2016-05-05 at the Wayback Machine by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
- Image HIP 14810
