HD 114386
In today's world, HD 114386 has become a topic of great relevance and interest to a wide range of people. Whether due to its impact on society, its relevance in the workplace or its influence on popular culture, HD 114386 has acquired a prominent place in the public conversation. As we delve into this article, we will explore the various facets of HD 114386 and examine its importance in different contexts. From its impact on the global economy to its role in the evolution of technology, HD 114386 continues to be a highly relevant topic in the modern world. Through detailed analysis, we will attempt to shed light on the complexities and nuances surrounding HD 114386, in hopes of providing a deeper and more complete understanding of this phenomenon.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 10m 39.824s[1] |
| Declination | −35° 03′ 17.21″[1] |
| Apparent magnitude (V) | 8.73[2] |
| Characteristics | |
| Spectral type | K3 V[2] |
| B−V color index | 0.982[2] |
| Astrometry | |
| Radial velocity (Rv) | 33.350±0.0004[3] km/s |
| Proper motion (μ) | RA: −137.143 mas/yr[1] Dec.: −324.874 mas/yr[1] |
| Parallax (π) | 35.7355±0.0200 mas[1] |
| Distance | 91.27 ± 0.05 ly (27.98 ± 0.02 pc) |
| Absolute magnitude (MV) | 6.49[2] |
| Details | |
| Mass | 0.76±0.01[4] M☉ |
| Radius | 0.73±0.01[4] R☉ |
| Luminosity | 0.28±0.01[4] L☉ |
| Surface gravity (log g) | 4.58±0.02[4] cgs |
| Temperature | 4,926±13[4] K |
| Metallicity | −0.012[5] dex |
| Rotational velocity (v sin i) | 3.06[5] km/s |
| Age | 8.8±2.8[4] Gyr |
| Other designations | |
| CD−34°8698, HD 114386, HIP 64295, SAO 204193, PPM 291056, LTT 5041, NLTT 33118[6] | |
| Database references | |
| SIMBAD | data |
HD 114386 is a star with a pair of orbiting exoplanets in the southern constellation of Centaurus. It has an apparent visual magnitude of 8.73,[2] which means it cannot be viewed with the naked eye but can be seen with a telescope or good binoculars. Based on parallax measurements, the system is located at a distance of 91 light years from the Sun. It is receding with a radial velocity of 33.4 km/s.[3] The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.318 arcsec yr−1.[7]
The spectrum of HD 114386 yields a stellar classification of K3 V,[2] matching a K-type main-sequence star, or orange dwarf. It has 76% of the mass of the Sun and 73% of the Sun's radius. HD 114386 is a much older star than the Sun with an estimated age of roughly nine billion years.[4] The abundance of iron in the stellar atmosphere, a measure of the star's metallicity, is nearly solar.[5] It is rather dim compared to the Sun, radiating just 28% of the luminosity of the Sun from its photosphere at an effective temperature of 4,926 K.[4]
Planetary system
In 2004, the Geneva Extrasolar Planet Search Team announced the discovery of an extrasolar planet orbiting the star.[2] The preliminary data for a second exoplanet was released in 2011.[8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.37 MJ | 1.65[9] | 445 | 0.12 | — | — |
| c | ≥1.19 MJ | – | 1,046 | 0.06 | — | — |
See also
References
- ^ a b c d 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 e f g h Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv:astro-ph/0310316. Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID 5233877.
- ^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
- ^ a b c d e f g h Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692. A5.
- ^ a b c Rice, Malena; Brewer, John M. (August 2020). "Stellar Characterization of Keck HIRES Spectra with The Cannon". The Astrophysical Journal. 898 (2): 119. arXiv:2007.02942. Bibcode:2020ApJ...898..119R. doi:10.3847/1538-4357/ab9f96. 119.
- ^ "HD 114386". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-01-09.
- ^ Luyten, W. J. (June 1995). "NLTT Catalogue (Luyten, 1979)". VizieR Online Data Catalog. Bibcode:1995yCat.1098....0L.
- ^ a b Mayor, M.; et al. (September 2011). "The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets". arXiv:1109.2497 .
- ^ "Confirmed Planets". NASA Exoplanet Archive. California Institute of Technology. Archived from the original on 12 December 2012.
