HD 213240
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Grus[1] |
| Right ascension | 22h 31m 00.36634s[2] |
| Declination | −49° 25′ 59.7690″[2] |
| Apparent magnitude (V) | 6.81[3] |
| Characteristics | |
| Spectral type | G0/G1V[4] + M5-5.5[5] |
| B−V color index | 0.603±0.005[3] |
| Astrometry | |
| Radial velocity (Rv) | −0.37±0.12[2] km/s |
| Proper motion (μ) | RA: −135.912 mas/yr[2] Dec.: −193.844 mas/yr[2] |
| Parallax (π) | 24.4247±0.0208 mas[2] |
| Distance | 133.5 ± 0.1 ly (40.94 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.77[3] |
| Details | |
| Mass | 1.57±0.02[6] M☉ |
| Radius | 1.56+0.03 −0.04[7] R☉ |
| Luminosity | 2.687+0.007 −0.006[7] L☉ |
| Surface gravity (log g) | 4.17±0.02[8] cgs |
| Temperature | 5,921+70 −58[7] K |
| Metallicity [Fe/H] | 0.14±0.01[3] dex |
| Rotational velocity (v sin i) | 3.5[9] km/s |
| Age | 4.6±0.6[8] Gyr |
| Other designations | |
| CD−50° 13701, HD 213240, HIP 111143, SAO 231175, LTT 9047[10] | |
| Database references | |
| SIMBAD | data |
HD 213240 is a possible binary star[11] system in the constellation Grus. It has an apparent visual magnitude of 6.81,[3] 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.[3]
This is an ordinary G-type main-sequence star with a stellar classification of G0/G1V.[4] It is a metal-rich star with an age that has been calculated as being anywhere from 2.7 to 4.6 billion years.[11] The star has 1.6[6] times the mass of the Sun and 1.56[7] times the Sun's radius. It is spinning with a projected rotational velocity of 3.5 km/s.[9] The star is radiating 2.69[7] times the luminosity of the Sun from its photosphere at an effective temperature of 5,921 K.[7]
A red dwarf companion star was detected in 2005 with a projected separation of 3,898 AU.[11]
Planetary system
[edit]The Geneva extrasolar planet search team discovered a planet orbiting this star in 2001.[12] 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.[11] In 2023, the inclination and true mass of HD 213240 b were determined via astrometry, confirming its planetary nature.[13]
| 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
[edit]References
[edit]- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- 1 2 3 4 5 6 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.
- 1 2 3 4 5 6 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.
- 1 2 Houk, N. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 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. arXiv:1408.1208. Bibcode:2014A&A...569A.120L. doi:10.1051/0004-6361/201424210. S2CID 118516214. A120.
- 1 2 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. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. S2CID 119219062. 136.
- 1 2 3 4 5 6 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.
- 1 2 Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5, 14 pp. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692.
- 1 2 Delgado Mena, E.; et al. (April 2015), "Li abundances in F stars: planets, rotation, and Galactic evolution", Astronomy & Astrophysics, 576: 24, arXiv:1412.4618, Bibcode:2015A&A...576A..69D, doi:10.1051/0004-6361/201425433, S2CID 56051637, A69
- ↑ "HD 213240". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.
- 1 2 3 4 Mugrauer, M.; et al. (2005). "Four New Wide Binaries Among Exoplanet Host Stars". Astronomy and Astrophysics. 440 (3): 1051–1060. arXiv:astro-ph/0507101. Bibcode:2005A&A...440.1051M. doi:10.1051/0004-6361:20042297. S2CID 14065040.
- ↑ 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. arXiv:astro-ph/0106255. Bibcode:2001A&A...379..999S. doi:10.1051/0004-6361:20011366. S2CID 59061741.
- 1 2 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. S2CID 257663647.
