| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 12h 13m 53.3962s[1] |
| Declination | −00° 23′ 36.5534″[1] |
| Apparent magnitude (V) | 8.951[2] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | F5V[3] |
| B−V color index | 0.45[2] |
| Astrometry | |
| Radial velocity (Rv) | −3.2±0.3[1] km/s |
| Proper motion (μ) | RA: −2.36±0.03 mas/yr[1] Dec.: 11.943±0.019 mas/yr[1] |
| Parallax (π) | 9.1725 ± 0.0221 mas[1] |
| Distance | 355.6 ± 0.9 ly (109.0 ± 0.3 pc) |
| Details | |
| Mass | 1.105+0.028 −0.036[4] M☉ |
| Radius | 1.286+0.049 −0.040[4] R☉ |
| Luminosity | 2.432+0.057 −0.234[4] L☉ |
| Surface gravity (log g) | 4.261+0.027 −0.024[4] cgs |
| Temperature | 6,300±37[4] K |
| Metallicity [Fe/H] | −0.268+0.060 −0.071[4] dex |
| Rotation | 4.78±0.15[5] |
| Rotational velocity (v sin i) | 12.9±0.4[4] km/s |
| Age | 3.987+0.802 −0.516[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 106315, or K2-109, is a single star with a pair of close-orbiting exoplanets, located in the constellation of Virgo. Based on parallax measurements, this system lies at a distance of 356 light years from the Sun.[1] At that range, the star is too faint to be seen with the naked eye, as it has an apparent visual magnitude of 8.95.[2] But it is slowly drifting closer with a radial velocity of −3 km/s.[1] As of 2020[update], multiplicity surveys have not detected any stellar companions to HD 106315.[5]
The spectrum of HD 106315 presents as an ordinary F-type main-sequence star with a stellar classification of F5V,[3] indicating it is generating energy through hydrogen fusion at its core. It is estimated to be roughly four[4] billion years old but is spinning quickly with a rotation period of 5 days. The star is relatively metal-poor, having 60% of solar concentration of iron. It has only a low level of magnetic activity in its chromosphere, showing a minimal level of star spot coverage.[5] The star has 11% more mass and a 29% larger radius than the Sun. It is radiating 2.4 times the luminosity of the Sun from its photosphere at an effective temperature of 6,300 K.[4]
Planetary system
Two planets were detected by the transit method in 2017,[4] using data from the extended Kepler mission (K2). Their large planetary radii imply both planets have a massive steam atmosphere for planet b and hydrogen-helium atmosphere for planet c.[5] The planetary system of HD 106315 is rather unstable and current planetary orbits are the outcome of violent dynamical history,[7] strongly affected by relativistic effects.[8] The orbits of planets are nearly coplanar, and orbit of c is well aligned with the equatorial plane of the star, misalignment been equal to -10+3.6
−3.8°.[9]
Since 2017, a third outer planet with mass above 45ME is suspected to exist in the system.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 10.5±3.1[5] M🜨 | 0.0924+0.0011 −0.0012 |
9.55288±0.00021 | 0 | 87.6+3.0 −1.7° |
2.4±0.2 R🜨 |
| c | 12.0±3.8[5] M🜨 | 0.1565+0.0019 −0.0020 |
21.05652±0.00012 | 0 | 88.89+0.69 −0.51° |
4.379±0.086 R🜨 |
References
- ^ a b c d e f g 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.
- ^ a b c d Crossfield, Ian J. M.; et al. (2017). "Two Small Transiting Planets and a Possible Third Body Orbiting HD 106315". The Astronomical Journal. 153 (6): 255. arXiv:1701.03811. Bibcode:2017AJ....153..255C. doi:10.3847/1538-3881/aa6e01. S2CID 55601944.
- ^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- ^ a b c d e f g h i j k Rodriguez, Joseph E.; et al. (2017). "A Multi-planet System Transiting the V = 9 Rapidly Rotating F-Star HD 106315". The Astronomical Journal. 153 (6): 256. arXiv:1701.03807. Bibcode:2017AJ....153..256R. doi:10.3847/1538-3881/aa6dfb. S2CID 118983037.
- ^ a b c d e f Kosiarek, Molly R.; et al. (2021). "Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827". The Astronomical Journal. 161 (1): 47. arXiv:2009.03398. Bibcode:2021AJ....161...47K. doi:10.3847/1538-3881/abca39. S2CID 221534625.
- ^ "HD 106315", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 26 July 2022
- ^ Turrini, D.; et al. (2020). "Normalized angular momentum deficit: A tool for comparing the violence of the dynamical histories of planetary systems". Astronomy and Astrophysics. 636: A53. arXiv:2003.05366. Bibcode:2020A&A...636A..53T. doi:10.1051/0004-6361/201936301. S2CID 212657397.
- ^ Marzari, F.; Nagasawa, M. (2020). "Secular evolution of close-in planets: The effects of general relativity". Monthly Notices of the Royal Astronomical Society. 493 (1): 427. arXiv:2001.09801. Bibcode:2020MNRAS.493..427M. doi:10.1093/mnras/staa271.
- ^ Zhou, George; et al. (2018). "The Warm Neptunes around HD 106315 Have Low Stellar Obliquities". The Astronomical Journal. 156 (3): 93. arXiv:1807.00024. Bibcode:2018AJ....156...93Z. doi:10.3847/1538-3881/aad085. S2CID 118864208.
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This page was last edited on 11 January 2024, at 21:42