HD 11964

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HD 11964
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Right ascension 01h 57m 09.61s[1]
Declination −10° 14′ 32.7″[1]
Apparent magnitude (V) 6.415
Spectral type G5IV
Apparent magnitude (U) 7.705
Apparent magnitude (B) 7.255
Apparent magnitude (R) 5.960
Apparent magnitude (I) 5.555
Apparent magnitude (J) 5.023
Apparent magnitude (H) 4.637
Apparent magnitude (K) 4.491
U−B color index 0.450
B−V color index 0.840
V−R color index 0.455
R−I color index 0.405
Variable type Suspected
Radial velocity (Rv) -6.9 km/s
Proper motion (μ) RA: -366.23 ± 0.49[1] mas/yr
Dec.: -242.39 ± 0.49[1] mas/yr
Parallax (π) 30.44 ± 0.60[1] mas
Distance 107 ± 2 ly
(32.9 ± 0.6 pc)
Absolute magnitude (MV) +3.76[citation needed]
Mass 1.12 ± 0.03[2] M
Radius 2.234 ± 0.304[3] R
Luminosity 2.9[2] L
Temperature 5552 K
Metallicity [Fe/H] +0.17 dex
Age 7.02 ± 0.67[2] Gyr
Other designations
BD-10°403, GC 2351, Gl 81.1A, Wo 9063A, HIP 9094, SAO 148123
Database references
Exoplanet Archive data
Extrasolar Planets

HD 11964 is a yellow subgiant star approximately 107 light-years away in the constellation of Cetus. The star is more massive and luminous than our Sun and is barely visible to the naked eye. A wide binary companion star was discovered in 2000.[4] Two extrasolar planets have been confirmed to orbit the star.

Planetary system[edit]

In August 2005, two planets were discovered orbiting the star, the innermost like Neptune and another like Jupiter orbiting at 3.34 AU. However, the second planet (HD 11964 b) was not confirmed until May 2007. In September 2007, P.C. Gregory claimed that there was a third planet in the system on the basis of Bayesian analysis of the radial velocity data. The planet was claimed to have a mass similar to that of Saturn and located in a 360-day orbit. Gregory cautioned that the close match between the period of this planet to being exactly a year meant that the radial velocity variations may have been caused by insufficient correction for the motion of the Earth in orbit around the Sun.[5] The planet was not detected in re-reduced data in an analysis published in the Astrophysical Journal in 2009.[6]

The HD 11964 planetary system[6]
(in order from star)
Mass Semimajor axis
Orbital period
Eccentricity Inclination Radius
c ≥0.11 MJ 0.229 37.82 0.15
b ≥0.61 ± 0.1 MJ 3.34 ± 0.4 2110 ± 70 0.06 ± 0.2

See also[edit]


  1. ^ a b c d e van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.  Vizier catalog entry
  2. ^ a b c Ghezzi, L.; et al. (December 2010), "Metallicities of Planet-hosting Stars: A Sample of Giants and Subgiants", The Astrophysical Journal, 725 (1): 721–733, arXiv:1008.3539Freely accessible, Bibcode:2010ApJ...725..721G, doi:10.1088/0004-637X/725/1/721. 
  3. ^ van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal. 694 (2): 1085–1098. arXiv:0901.1206Freely accessible. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. 
  4. ^ Allen; et al. (2000). "Wide binaries among high-velocity and metal-poor stars". Astronomy and Astrophysics. 356 (2): 529–540. Bibcode:2000A&A...356..529A. 
  5. ^ Gregory, P.C. (2007). "A Bayesian periodogram finds evidence for three planets in HD 11964". MNRAS. 381 (4): 1607–1616. arXiv:0709.0970Freely accessible. Bibcode:2007MNRAS.381.1607G. doi:10.1111/j.1365-2966.2007.12361.x. 
  6. ^ a b Wright, J. T.; et al. (2009). "Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems". The Astrophysical Journal. 693 (2): 1084–1099. arXiv:0812.1582Freely accessible. Bibcode:2009ApJ...693.1084W. doi:10.1088/0004-637X/693/2/1084. 

External links[edit]

Coordinates: Sky map 01h 57m 09.6064s, −10° 14′ 32.739″