HD 141937
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Libra |
| Right ascension | 15h 52m 17.54814s[1] |
| Declination | −18° 26′ 09.7939″[1] |
| Apparent magnitude (V) | 7.25[2] |
| Characteristics | |
| Spectral type | G1V[3] |
| B−V color index | +0.628±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | −2.20±0.68[2] km/s |
| Proper motion (μ) | RA: +97.231±0.133[1] mas/yr Dec.: +19.113±0.116[1] mas/yr |
| Parallax (π) | 29.9453 ± 0.0640 mas[1] |
| Distance | 108.9 ± 0.2 ly (33.39 ± 0.07 pc) |
| Absolute magnitude (MV) | 4.71[2] |
| Details | |
| Mass | 1.03[4] M☉ |
| Radius | 1.05[1] R☉ |
| Luminosity | 1.202±0.003[1] L☉ |
| Surface gravity (log g) | 4.44[4] cgs |
| Temperature | 5,890+15 −30[1] K |
| Metallicity [Fe/H] | +0.10±0.01[2] dex |
| Rotational velocity (v sin i) | 6.0[2] km/s |
| Age | 3.82[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 141937 is a star in the southern zodiac constellation of Libra, positioned a couple of degrees to the north of Lambda Librae. It is a yellow-hued star with an apparent visual magnitude of 7.25,[2] which means it is too faint to be seen with the naked eye. This object is located at a distance of 108.9 light years from the Sun based on parallax,[1] but is drifting closer with a radial velocity of −2.2 km/s.[2] It has an absolute magnitude of 4.71.[2]
This is a G-type main-sequence star with a stellar classification of G1V.[3] It is a solar-type star with slightly higher mass and radius compared to the Sun. The metallicity is higher than solar. It is an estimated 3.8[4] billion years old and is spinning with a projected rotational velocity of 6 km/s.[6] The star is radiating 1.2 times the luminosity of the Sun from its photosphere at an effective temperature of 5,890 K.[1]
The star has a substellar companion (HD 141937 b) announced in April 2001 by the European Southern Observatory. It has a minimum mass of 9.7 MJ. In 2020, the inclination of the orbit was measured, revealing its true mass to be 27.4 MJ, which makes it a brown dwarf. A 653-day orbit places the orbital distance 1.5 times farther away from the star as Earth is from the Sun, with a high eccentricity of 41%.[7][8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 27.42+6.78 −9.86 MJ |
1.4877±0.0018 | 653.22±1.21 | 0.41±0.01 | 20.52+12.47 −4.16° |
— |
See also
[edit]References
[edit]- ^ a b c d e f g h i j 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 h i 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 Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
- ^ a b c d Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal. 153 (1): 19. arXiv:1611.02897. Bibcode:2017AJ....153...21L. doi:10.3847/1538-3881/153/1/21. S2CID 119511744. 21.
- ^ "HD 117207". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-23.
- ^ Delgado Mena, E.; et al. (February 2014). "Li depletion in solar analogues with exoplanets. Extending the sample". Astronomy & Astrophysics. 562: 17. arXiv:1311.6414. Bibcode:2014A&A...562A..92D. doi:10.1051/0004-6361/201321493. S2CID 56104807. A92.
- ^ "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 29, 2012.
- ^ a b Kiefer, F.; et al. (January 2021). "Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets". Astronomy & Astrophysics. 645 A7. arXiv:2009.14164. Bibcode:2021A&A...645A...7K. doi:10.1051/0004-6361/202039168. S2CID 221995447.
- ^ Udry, S.; et al. (2002). "The CORALIE survey for southern extra-solar planets VIII. The very low-mass companions of HD141937, HD162020, HD168443, HD202206: brown dwarfs or superplanets?". Astronomy and Astrophysics. 390 (1): 267–279. arXiv:astro-ph/0202458. Bibcode:2002A&A...390..267U. doi:10.1051/0004-6361:20020685. S2CID 9389274.
- ^ Liu, Kang; et al. (November 2014). "Precise determination of fundamental parameters of six exoplanet host stars and their planets". Research in Astronomy and Astrophysics. 14 (11): 1447–1457. arXiv:1406.2173. Bibcode:2014RAA....14.1447L. doi:10.1088/1674-4527/14/11/008. S2CID 118779573. 1447-1457.
