HD 106315 C
The spectrum of HD 106315 presents as an ordinary F-type main-sequence star with a stellar classification of F5V, indicating it is generating energy through hydrogen fusion at its core. It is estimated to be roughly four 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. 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.
Planetary system
Two planets were detected by the transit method in 2017, 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. The planetary system of HD 106315 is rather unstable and current planetary orbits are the outcome of violent dynamical history, strongly affected by relativistic effects. 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
−3.8°.
Since 2017, a third outer planet with mass above 45ME is suspected to exist in the system.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 10.5±3.1 M🜨 | 0.0924 −0.0012 |
9.55288±0.00021 | 0 | 87.6 −1.7° |
2.4±0.2 R🜨 |
| c | 12.0±3.8 M🜨 | 0.1565 −0.0020 |
21.05652±0.00012 | 0 | 88.89 −0.51° |
4.379±0.086 R🜨 |
References
- ^ 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.
- ^ 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.
- ^ Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- ^ 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.
- ^ 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.
