HD 132406 is a star in the northern constellation of Boötes. With an apparent visual magnitude of 8.45,[2] it is invisible to the naked eye. The distance to this star is 230 light-years (71 parsecs) based on parallax, but it is drifting closer with a radial velocity of −37.8 km/s. The star has an absolute magnitude of 4.30.[2] It has one confirmed exoplanet companion.[3]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h 56m 54.65138s[1] |
| Declination | +53° 22′ 55.8065″[1] |
| Apparent magnitude (V) | 8.45[2] |
| Characteristics | |
| Spectral type | G0V[3] |
| B−V color index | 0.650±0.015[2] |
| Astrometry | |
| Radial velocity (Rv) | −37.80±0.13[1] km/s |
| Proper motion (μ) | RA: −14.122 mas/yr[1] Dec.: −280.330 mas/yr[1] |
| Parallax (π) | 14.1756 ± 0.0191 mas[1] |
| Distance | 230.1 ± 0.3 ly (70.54 ± 0.10 pc) |
| Absolute magnitude (MV) | 4.30[2] |
| Details | |
| Mass | 1.02+0.03 −0.02[4] M☉ |
| Radius | 1.36+0.03 −0.01[5] R☉ |
| Luminosity | 1.827±0.006[5] L☉ |
| Surface gravity (log g) | 4.22±0.05[4] cgs |
| Temperature | 5,754+29 −51[5] K |
| Metallicity [Fe/H] | 0.07±0.04[4] dex |
| Rotational velocity (v sin i) | 1.7[3] km/s |
| Age | 8.79+1.13 −1.51[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The stellar classification of HD 132406 is G0V, matching an ordinary G-type main-sequence star like the Sun. It is an older star with an age of up to nine billion years[4] and is spinning with a leisurely projected rotational velocity of 1.7 km/s.[3] It appears to have a similar mass[4] as the Sun but is about 36% greater in girth.[5] The metallicity, or chemical abundance of heavier elements, appears slightly higher than in the Sun.[4] The star is radiating 1.8 times the luminosity of the Sun from its photosphere at an effective temperature of 5,754 K.[5]
A planetary companion was announced in 2007, based on the radial velocity variation of the host star as measured using the ELODIE spectrograph instrument. This super Jupiter has an orbital period of 2.67 years with an eccentricity of 0.34.[3] An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3,[7] and this was updated in 2023.[8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 6.2+2.2 −1.1 MJ |
1.969+0.06 −0.064 |
2.64±0.11 | 0.303+0.093 −0.077 |
116+19 −18° |
— |
References
edit- ^ a b c d e 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 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 c d e da Silva, Ronaldo; Udry, Stéphane; Bouchy, François; Moutou, Claire; Mayor, Michel; Beuzit, Jean-Luc; Bonfils, Xavier; Delfosse, Xavier; Desort, Morgan; Forveille, Thierry; Galland, Franck; Hébrard, Guillaume; Lagrange, Anne-Marie; Loeillet, Benoit; Lovis, Christophe; Pepe, Francesco; Perrier, Christian; Pont, Frédéric; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Sivan, Jean-Pierre; Vidal-Madjar, Alfred; Zucker, Shay (October 2007). "ELODIE metallicity-biased search for transiting Hot Jupiters IV. Intermediate period planets orbiting the stars HD 43691 and HD 132406". Astronomy and Astrophysics. 473 (1): 323–328. arXiv:0707.0958. Bibcode:2007A&A...473..323D. doi:10.1051/0004-6361:20077314. S2CID 18805775.
- ^ a b c d e f g Aguilera-Gómez, Claudia; et al. (June 2018). "Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert". Astronomy & Astrophysics. 614: 15. arXiv:1803.05922. Bibcode:2018A&A...614A..55A. doi:10.1051/0004-6361/201732209. S2CID 62799777. A55.
- ^ a b c d e 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.
- ^ "HD 132406". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-04-05.
- ^ Gaia Collaboration; et al. (2022). "Gaia Data Release 3: Stellar multiplicity, a teaser for the hidden treasure". arXiv:2206.05595 [astro-ph.SR].
- ^ a b Xiao, Guang-Yao; Liu, Yu-Juan; et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics. 23 (5): 055022. arXiv:2303.12409. Bibcode:2023RAA....23e5022X. doi:10.1088/1674-4527/accb7e.
External links
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