HD 114762

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Double star
HD 114762
AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation Berenike's hair
Right ascension 13 h 12 m 19.75 s
declination + 17 ° 31 ′ 1.6 ″
Apparent brightness 7.3 likes
Typing
Spectral class F9 V
Astrometry
Radial velocity (51.03 ± 0.14) km / s
parallax (24.85 ± 0.27)  mas
distance (131 ± 1)  ly
(40.2 ± 0.4)  pc
Proper movement 
Rec. Share: (−586.29 ± 0.71)  mas / a
Dec. portion: (2.26 ± 0.24)  mas / a
Physical Properties
Dimensions (0.80 ± 0.06)  M ☉
Metallicity [Fe / H] −0.72   +0.05−0.07
Age 12 ± 4 billion  a
Other names
and catalog entries
Bonn survey BD + 18 ° 2700
Henry Draper Catalog HD 114762 [1]
Hipparcos catalog HIP 64426 [2]
SAO catalog SAO 100458 [3]
Tycho catalog TYC 1454-315-1 [4]Template: Infobox star / maintenance / specification of the TYC catalog
2MASS catalog 2MASS J13121982 + 1731016 [5]
Other names LHS 2693, FK5  5165, G 63-9

HD 114762 is the name of a star system in the constellation Haar der Berenike . It is about 130 light years from Earth. The central star is a low-metal main sequence star of the spectral class F9, which is orbited by two companions.

The companions

HD 114762 Ab

The closer companion HD 114762 Ab (also called "HD 114762 b") orbits the central star at a distance of around 53 million kilometers (≈ 0.353  AU ) and takes around 84 days to do so. Since the orbit inclination of the companion was not known for a long time, its mass could not be precisely determined. Estimates indicated that it was a substellar object, with a minimum mass of about 10 Jupiter's masses . This would have made it possible to classify it as a planetary gas giant , but planetologists thought it more likely that the companion was a brown dwarf . HD 114762 Ab was discovered in 1989 using the radial velocity method and was the first candidate for an exoplanet discovered in this way . A work from 2019 combined the data from the radial velocity method with the astrometric data from the Gaia mission . The mass of HD 114762b became 107   +31−27 M J determines what the object would probably even be a low-mass red dwarf instead of a planet.

HD 114762 B

The more distant companion is about 3.3 arc seconds (approx. 20 billion km or 130 AU) away from the central star. This is probably an object of the spectral class M or L.

Individual evidence

  1. ↑ a b c d HD 114762. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed on November 24, 2019 .
  2. ↑ ARICNS page for HD 114762
  3. ↑ a b c Patience et al .: Stellar Companions to Stars with Planets. In: The Astrophysical Journal , Vol. 581, Issue 1, pp. 654ff. (2002), bibcode : 2002ApJ ... 581..654P
  4. ↑ a b c d Flavien Kiefer: Determining the mass of the planetary candidate HD 114762b using Gaia . In: arXiv . arxiv : 1910.07835 .
  5. ↑ a b HD 114762 b (English) - Entry in the EPE , last change on January 10, 2016.
  6. ↑ Mazeh et al. : Spectroscopic Orbits for Three Binaries with Low-Mass Companions and the Distribution of Secondary Masses near the Substellar Limit (English); in: Astrophysical Journal, Vol. 466 , pp. 415ff. (1996), bibcode : 1996ApJ ... 466..415M