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HD 213240 is a possible binary star[9] 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]

HD 213240
Observation data
Epoch J2000      Equinox J2000
Constellation Grus
Right ascension 22h 31m 00.36652s[1]
Declination −49° 25′ 59.7675″[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)−0.52±0.18[1] km/s
Proper motion (μ) RA: −136.026±0.047[1] mas/yr
Dec.: −193.926±0.052[1] mas/yr
Parallax (π)24.4385 ± 0.0372 mas[1]
Distance133.5 ± 0.2 ly
(40.92 ± 0.06 pc)
Absolute magnitude (MV)3.77[2]
Details
Mass1.57±0.02[5] M☉
Radius1.56+0.03
−0.04[1] R☉
Luminosity2.687+0.007
−0.006[1] L☉
Surface gravity (log g)4.17±0.02[6] cgs
Temperature5,921+70
−58[1] K
Metallicity [Fe/H]0.14±0.01[2] dex
Rotational velocity (v sin i)3.5[7] km/s
Age4.6±0.6[6] Gyr
Other designations
CPD−50° 13701, HD 213240, HIP 111143, SAO 231175, LTT 9047[8]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

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 has been calculated as being anywhere from 2.7 to 4.6 billion years.[9] The star has 1.6[5] times the mass of the Sun and 1.56[1] times the Sun's radius. It is spinning with a projected rotational velocity of 3.5 km/s.[7] The star is radiating 2.69[1] times the luminosity of the Sun from its photosphere at an effective temperature of 5,921 K.[1]

A red dwarf companion star was detected in 2005 with a projected separation of 3,898 AU.[9]


Planetary system


The Geneva extrasolar planet search team discovered a planet orbiting this star in 2001.[10] There is a 5% chance this is actually a brown dwarf.[9]

The HD 213240 planetary system[11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥4.72±0.40 MJ 1.92±0.11 882.7±7.6 0.421±0.015 — —

See also



References


  1. 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.
  2. 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.
  3. 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.
  4. 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. A120.
  5. 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.
  6. 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.
  7. 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
  8. "HD 213240". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.
  9. 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.
  10. 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.
  11. Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.


На других языках

[de] HD 213240

HD 213240 ist ein Stern mit einem Planetensystem, der sich in ca. 40,75 Parsec Entfernung vom Sonnensystem befindet. Der Stern hat mindestens einen Planeten.
- [en] HD 213240

[es] HD 213240

HD 213240 (HIP 111143 / CD-50 13701 / GC 31437)[1] es una estrella en la constelación de Grus, la grulla, de magnitud aparente +6,80. Se encuentra a 133 años luz de distancia del Sistema Solar. Desde 2001 se conoce la existencia de un planeta extrasolar orbitando alrededor de esta estrella.[2]


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