Astronomy:HD 141937
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[1] mas |
| 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 |
| Extrasolar Planets Encyclopaedia | 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 |♃|J}}}}}}. In 2020, the inclination of the orbit was measured, revealing its true mass to be 27.4 |♃|J}}}}}}, 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
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 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. doi:10.1086/504637. Bibcode: 2006AJ....132..161G.
- ↑ 4.0 4.1 4.2 4.3 Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal 153 (1): 19. doi:10.3847/1538-3881/153/1/21. 21. Bibcode: 2017AJ....153...21L.
- ↑ "HD 117207". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+117207.
- ↑ Delgado Mena, E. et al. (February 2014). "Li depletion in solar analogues with exoplanets. Extending the sample". Astronomy & Astrophysics 562: 17. doi:10.1051/0004-6361/201321493. A92. Bibcode: 2014A&A...562A..92D.
- ↑ "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 29, 2012.
- ↑ 8.0 8.1 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. doi:10.1051/0004-6361/202039168. Bibcode: 2021A&A...645A...7K.
- ↑ 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. doi:10.1051/0004-6361:20020685. Bibcode: 2002A&A...390..267U. http://www.aanda.org/articles/aa/full/2002/28/aa2416/aa2416.html.
- ↑ 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. doi:10.1088/1674-4527/14/11/008. 1447-1457. Bibcode: 2014RAA....14.1447L.
Coordinates: 
15h 52m 17.5474s, −18° 26′ 09.834″
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