Astronomy:HD 213240
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Grus |
| Right ascension | 22h 31m 00.36634s[1] |
| Declination | −49° 25′ 59.7690″[1] |
| Apparent magnitude (V) | 6.81[2] |
| Characteristics | |
| Spectral type | G0/G1V[3] + M5-5.5[4] |
| B−V color index | 0.603±0.005[2] |
| Astrometry | |
| Radial velocity (Rv) | −0.37±0.12[1] km/s |
| Proper motion (μ) | RA: −135.912[1] mas/yr Dec.: −193.844[1] mas/yr |
| Parallax (π) | 24.4247 ± 0.0208[1] mas |
| Distance | 133.5 ± 0.1 ly (40.94 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.77[2] |
| Details | |
| Mass | 1.57±0.02[5] M☉ |
| Radius | 1.56+0.03 −0.04[6] R☉ |
| Luminosity | 2.687+0.007 −0.006[6] L☉ |
| Surface gravity (log g) | 4.17±0.02[7] cgs |
| Temperature | 5,921+70 −58[6] K |
| Metallicity [Fe/H] | 0.14±0.01[2] dex |
| Rotational velocity (v sin i) | 3.5[8] km/s |
| Age | 4.6±0.6[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Extrasolar Planets Encyclopaedia | data |
HD 213240 is a possible binary star[10] system in the constellation Grus. It has an apparent visual magnitude of 6.81,[2] which lies below the limit of visibility for normal human sight. The system is located at a distance of 133.5 light years from the Sun based on parallax. The primary has an absolute magnitude of 3.77.[2]
This is an ordinary G-type main-sequence star with a stellar classification of G0/G1V.[3] It is a metal-rich star with an age that has been calculated as being anywhere from 2.7 to 4.6 billion years.[10] The star has 1.6[5] times the mass of the Sun and 1.56[6] times the Sun's radius. It is spinning with a projected rotational velocity of 3.5 km/s.[8] The star is radiating 2.69[6] times the luminosity of the Sun from its photosphere at an effective temperature of 5,921 K.[6]
A red dwarf companion star was detected in 2005 with a projected separation of 3,898 AU.[10]
Planetary system
The Geneva extrasolar planet search team discovered a planet orbiting this star in 2001.[11] Since this planet was discovered by radial velocity, only its minimum mass was initially known, and there was a 5% chance of it being massive enough to be a brown dwarf.[10] In 2023, the inclination and true mass of HD 213240 b were determined via astrometry, confirming its planetary nature.[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 5.21+1.5 −0.49 MJ |
1.92±0.026 | 2.4071+0.008 −0.0083 |
0.4201+0.01 −0.0093 |
63+17 −20 or 117+20 −17° |
— |
See also
- HD 212301
- List of extrasolar planets
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 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 Houk, N. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 2, Dept. of Astronomy, University of Michigan, Bibcode: 1978mcts.book.....H.
- ↑ Lodieu, N. et al. (September 2014). "Binary frequency of planet-host stars at wide separations. A new brown dwarf companion to a planet-host star". Astronomy & Astrophysics 569: 14. doi:10.1051/0004-6361/201424210. A120. Bibcode: 2014A&A...569A.120L.
- ↑ 5.0 5.1 Stassun, Keivan G. et al. (March 2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal 153 (3): 20. doi:10.3847/1538-3881/aa5df3. 136. Bibcode: 2017AJ....153..136S.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 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.
- ↑ 7.0 7.1 Bonfanti, A. et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics 585: A5, 14 pp. doi:10.1051/0004-6361/201527297. Bibcode: 2016A&A...585A...5B.
- ↑ 8.0 8.1 Delgado Mena, E. et al. (April 2015), "Li abundances in F stars: planets, rotation, and Galactic evolution", Astronomy & Astrophysics 576: 24, doi:10.1051/0004-6361/201425433, A69, Bibcode: 2015A&A...576A..69D
- ↑ "HD 213240". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+213240.
- ↑ 10.0 10.1 10.2 10.3 Mugrauer, M. et al. (2005). "Four New Wide Binaries Among Exoplanet Host Stars". Astronomy and Astrophysics 440 (3): 1051–1060. doi:10.1051/0004-6361:20042297. Bibcode: 2005A&A...440.1051M.
- ↑ Santos, N. C. et al. (2001). "The CORALIE survey for southern extra-solar planets VI. New long period giant planets around HD 28185 and HD 213240". Astronomy and Astrophysics 379 (3): 999–1004. doi:10.1051/0004-6361:20011366. Bibcode: 2001A&A...379..999S.
- ↑ 12.0 12.1 Xiao, Guang-Yao et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics 23 (5): 055022. doi:10.1088/1674-4527/accb7e. Bibcode: 2023RAA....23e5022X.
Coordinates: 
22h 31m 00.3672s, −49° 25′ 59.773″
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