23 Librae

Last updated
23 Librae
Observation data
Epoch J2000       Equinox J2000
Constellation Libra
Right ascension 15h 13m 28.6669s [1]
Declination −25° 18′ 33.6534″ [1]
Apparent magnitude  (V)6.45 [2]
Characteristics
Spectral type G5 V [3]
B−V color index +0.70 [2]
Astrometry
Radial velocity (Rv)+4.7 [4]  km/s
Proper motion (μ)RA: −400.147(26)  mas/yr [1]
Dec.: −75.253(27)  mas/yr [1]
Parallax (π)38.1946 ± 0.0370  mas [1]
Distance 85.39 ± 0.08  ly
(26.18 ± 0.03  pc)
Details
Mass 1.07+0.03
−0.08 [3]   M☉
Radius 1.25±0.04 [3]   R☉
Surface gravity (log g)4.30 [5]   cgs
Temperature 5585±50 [3]   K
Metallicity [Fe/H]0.25±0.02 [3]   dex
Rotational velocity (v sin i)2.17 [3]  km/s
Age 8.4+1.6
−1.4 to 11.1+1.5
−3.7 [3]   Gyr
Other designations
CD−24° 11928, GJ  579.4, HD  134987, HIP  74500, HR  5657, SAO  183275 [6]
Database references
SIMBAD data
Exoplanet Archive data

23 Librae (23 Lib) is a star in the zodiac constellation Libra, making it visible from most of the Earth's surface. With an apparent visual magnitude of 6.45, [2] it requires dark skies and good seeing conditions to see this star with the naked eye. It has a planetary system with two confirmed extrasolar planets. [3]

Contents

Properties

Based upon parallax measurements, this star is located at a distance of 85 light-years (26 parsecs ) from the Earth. The spectral properties of 23 Librae identify it as stellar class G5 V, with the luminosity class of 'V' indicating that this is a main sequence star that is generating energy through the thermonuclear fusion of hydrogen at its core. This energy is being radiated from the outer envelope at an effective temperature of about 5,585 K, giving it the yellow hue typical of G-type stars. [7] Estimates of the age of 23 Librae range from 8.4 to 11.1 billion years, making it much older than the Sun. [3]

23 Librae is slightly larger than the Sun, with an estimated 107% of the Sun's mass and 125% of the Sun's radius. The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is higher than in the Sun. It appears to be rotating slowly, with the projected rotational velocity of 2.2 km∙s−1 giving a lower bound to the actual azimuthal velocity along the equator. [3]

Planetary system

In November 1999 an exoplanet 23 Librae b was announced orbiting 23 Librae, [8] [9] and in 2009 an additional planet was detected. [3] Examination of the system in the infrared using the Spitzer Space Telescope did not reveal any excess emission, which might otherwise suggest the presence of a circumstellar debris disk of orbiting dust. [10]

The 23 Librae planetary system [3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥ 1.59±0.02  MJ 0.81±0.02258.19±0.070.233±0.002——
c ≥ 0.82±0.03  MJ 5.8±0.55000±4000.12±0.02——

In the Halo franchise, the star system is home to the planets Hesiod, farther away from the star, and Madrigal in the habitable zone.

See also

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References

  1. 1 2 3 4 5 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.
  2. 1 2 3 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J
  3. 1 2 3 4 5 6 7 8 9 10 11 12 Jones, Hugh R. A.; et al. (April 2010), "A long-period planet orbiting a nearby Sun-like star", Monthly Notices of the Royal Astronomical Society , 403 (4): 1703–1713, arXiv: 0912.2716 , Bibcode:2010MNRAS.403.1703J, doi: 10.1111/j.1365-2966.2009.16232.x , S2CID   15911991
  4. ↑ Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv: 0811.3982 , Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID   118577511
  5. ↑ Sousa, S. G.; et al. (August 2007), "Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes", Astronomy and Astrophysics, 487 (1): 373–381, arXiv: 0805.4826 , Bibcode:2008A&A...487..373S, doi:10.1051/0004-6361:200809698, S2CID   18173201
  6. ↑ "23 Lib". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-05-24.
  7. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on February 22, 2012, retrieved 2012-01-16
  8. ↑ "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
  9. ↑ Vogt, Steven S.; et al. (2000), "Six New Planets from the Keck Precision Velocity Survey", The Astrophysical Journal, 536 (2): 902–914, arXiv: astro-ph/9911506 , Bibcode:2000ApJ...536..902V, doi:10.1086/308981, S2CID   119375519
  10. ↑ Dodson-Robinson, Sarah E.; et al. (January 2011). "A Spitzer Infrared Spectrograph Study of Debris Disks Around Planet-host Stars". The Astronomical Journal. 141 (1): 11. arXiv: 1010.3292 . Bibcode:2011AJ....141...11D. doi:10.1088/0004-6256/141/1/11. S2CID   118645999.
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