23 Andromedae

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23 Andromedae
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 00h 13m 30.83962s [1]
Declination +41° 02′ 07.3315″ [1]
Apparent magnitude  (V)5.71 [2]
Characteristics
Spectral type F0 IV [3]
B−V color index +0.331±0.004 [2]
Astrometry
Radial velocity (Rv)−27.1±1.2 [4]  km/s
Proper motion (μ)RA: −123.289 [1]   mas/yr
Dec.: −146.201 [1]   mas/yr
Parallax (π)26.8161 ± 0.0858  mas [1]
Distance 121.6 ± 0.4  ly
(37.3 ± 0.1  pc)
Absolute magnitude  (MV)+3.01 [5]
Details
Mass 1.43 [6]   M☉
Luminosity 49.9+5.5
−4.9 [3]   L☉
Surface gravity (log g)4.25 [6]   cgs
Temperature 7,089±241 [6]   K
Metallicity [Fe/H]−0.13±0.07 [7]   dex
Rotational velocity (v sin i)36 [3]  km/s
Age 759 [6]   Myr
Other designations
23 And, BD+40° 29, FK5  2010, HD  905, HIP  1086, HR  41, SAO  36173, PPM  42707 [8]
Database references
SIMBAD data

23 Andromedae, abbreviated 23 And, is a presumed single [9] star in the constellation Andromeda, although it has been a suspected spectroscopic binary. [10] 23 Andromedae is the Flamsteed designation. Its apparent visual magnitude is 5.71, [2] which indicates it is dimly visible to the naked eye under good viewing conditions. The distance to 23 And, as determined from its annual parallax shift of 26.8  mas , [1] is 121.6  light years. The star is moving further from the Earth with a heliocentric radial velocity of −27 km/s. [4] It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.191″ per year. [11]

The stellar classification of 23 And is F0 IV, [3] matching an F-type subgiant star that is in the process of evolving into a red giant. It displays a slight microvariability with a frequency of 0.85784 d−1 and an amplitude of 0.0062 magnitude. [12] The star is around 759 [6] million years old with a projected rotational velocity of 36 km/s. [3] It has 1.43 [6] times the mass of the Sun and is radiating 50 [3] times the Sun's luminosity from its photosphere at an effective temperature of 7,089 K. [6]

Related Research Articles

21 Tauri, formally known as Asterope, is a component of the Asterope double star in the Pleiades open cluster. 21 Tauri is the stars' Flamsteed designation. This star is potentially faintly visible to the naked eye with an apparent visual magnitude of 5.76 in ideal conditions, although anybody viewing the object is likely to instead see the pair as a single elongated form of magnitude 5.6. The distance to 21 Tauri can be estimated from its annual parallax shift of 7.6 mas, yielding a range of around 431 light years. It is moving further from the Earth with a heliocentric radial velocity of +6 km/s.

<span class="mw-page-title-main">Nu Tauri</span> Star in the constellation Taurus

ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.

58 Andromedae, abbreviated 58 And, is a single star in the northern constellation Andromeda. 58 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.78 The distance to this star, as determined from its annual parallax shift of 17.5 mas, is 186 light years. 58 And is moving further from the Earth with a heliocentric radial velocity of +8 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.159″ per year.

<span class="mw-page-title-main">28 Andromedae</span> Star in the constellation Andromeda

28 Andromedae is a Delta Scuti variable star in the constellation Andromeda. 28 Andromedae is the Flamsteed designation. It also bears the variable star name GN Andromedae. Its apparent magnitude is 5.214, varying by less than 0.1 magnitudes.

62 Andromedae, abbreviated 62 And, is a single star in the northern constellation Andromeda. 62 Andromedae is the Flamsteed designation; it also bears the Bayer designation of c Andromedae. It is bright enough to be seen by the naked eye, with an apparent magnitude of 5.31. Based upon parallax measurements made during the Gaia mission, it is at a distance of roughly 273 light-years from Earth. The star is moving closer to the Earth with a heliocentric radial velocity of −30 km/s, and is predicted to come to within 144.6 light-years in 1,6 million years.

59 Andromedae, abbreviated 59 And, is a sixth-magnitude binary star system in the northern constellation of Andromeda. 59 Andromedae is the Flamsteed designation. As of 2017, the pair had an angular separation of 16.60″ along a position angle (PA) of 36°. Compare this to a separation of 15.3″ along a PA of 35°, as measured in 1783. The two stars have an estimated physical separation of 1,370 AU.

39 Aurigae is a single star in the constellation of Auriga. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. The star is just barely visible to the naked eye, having an apparent visual magnitude of 5.90. Based upon an annual parallax shift of 20.11 mas as seen from Earth, it is located 112 light years away. 5 Andromedae is moving further from the Sun with a radial velocity of +34 km/s. It has a relatively high proper motion, advancing across the celestial sphere at the rate of 0.151 arc seconds per year.

Sigma2 Cancri, Latinized from σ2 Cancri, is the Bayer designation for a solitary, white-hued star in the constellation Cancer. It is faintly visible to the naked eye, with an apparent visual magnitude of +5.44. Based upon an annual parallax shift of 16.79 mas as seen from Earth, this star is located around 194 light years from the Sun.

19 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, located approximately 238 light years from Sun based on its parallax. It is dimly visible to the naked eye as a white-hued star with an apparent visual magnitude of 5.77. The pair orbit each other with a period of 219.2 years and an eccentricity of 0.686. The system is moving closer to the Earth with a heliocentric radial velocity of −21 km/s.

<span class="mw-page-title-main">50 Cassiopeiae</span> Star in the constellation Cassiopeia

50 Cassiopeiae is a white star in the northern constellation of Cassiopeia. In the past, it had been misidentified as a suspected nebula, and given the number NGC 771. The star is visible to the naked eye, having an apparent visual magnitude of +3.95. Based upon an annual parallax shift of 20.76 mas, it is located 157 light years away. It is moving closer, having a heliocentric radial velocity of −18 km/s, and will approach to within 82 ly in 1.879 million years.

<span class="mw-page-title-main">Upsilon Piscium</span> A-type main sequence star in the constellation Pisces

Upsilon Piscium is a solitary, white-hued star in the zodiac constellation of Pisces. It is faintly visible to the naked eye, having an apparent visual magnitude of +4.75. Based upon an annual parallax shift of 10.59 mas as seen from Earth, it is located about 308 light years from the Sun. The star is drifting further away with a heliocentric radial velocity of +6 km/s.

HD 88955 is a single, white-hued star in the southern constellation of Vela. It can be viewed with the naked eye, having an apparent visual magnitude of 3.85. The distance to HD 88955 can be determined from its annual parallax shift of 32.7 mas, which yields a separation of 100 light years from the Sun. It is moving further from the Earth with a heliocentric radial velocity of +7 km/s. Bayesian analysis suggests HD 88955 is a member of the Argus Association, a group of co-moving stars usually associated with the IC 2391 open cluster.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 108 parsecs (350 ly) distant.

<span class="mw-page-title-main">CL Draconis</span> Star in the constellation Draco

CL Draconis is a single star in the northern circumpolar constellation of Draco. It can be viewed with the naked eye, having an apparent visual magnitude of 4.96. The distance to this star, as determined from its annual parallax shift of 29.9 mas, is 109 light years. It is moving closer to the Earth with a heliocentric radial velocity of −11 km/s. The star has a relatively high proper motion, traversing the celestial sphere at the rate of 0.185″/yr.

HD 16754 is a binary or triple-star system in the constellation Eridanus. It has the Bayer designation s Eridani; HD 16754 is the designation from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of +4.74. It is located at a distance of approximately 132 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +18 km/s. The system is a member of the Columba association of co-moving stars.

<span class="mw-page-title-main">64 Eridani</span> Single, yellow-white hued star in the constellation Eridanus

64 Eridani is a single, yellow-white hued star in the constellation Eridanus having variable star designation S Eridani. It is faintly visible to the naked eye with an apparent visual magnitude of 4.77. The annual parallax shift is measured at 12.01 mas, which equates to a distance of about 272 light years. In addition to its proper motion, it is moving closer to the Sun with a radial velocity of around −9 km/s.

HD 125442 is a single star in the southern constellation of Lupus. Its apparent visual magnitude is 4.78, which can be seen with the naked eye. The distance to HD 125442, as determined from its annual parallax shift of 22.1 mas, is 147 light years.

134 Tauri is a single star in the zodiac constellation of Taurus. Its apparent magnitude is 4.89, which is bright enough to be faintly visible to the naked eye. The distance to this star, based upon an annual parallax shift of 13.11±0.33 mas, is around 249 light years. The star is moving further from the Sun with a heliocentric radial velocity of +20.5 km/s, having made its closest approach some three million years ago at a distance of 107 ly (32.7 pc).

<span class="mw-page-title-main">TU Corvi</span> Star in the constellation Corvus

TU Corvi is a yellow-white hued star in the southern constellation of Corvus. It is a dimly visible to the naked eye with an apparent visual magnitude of 6.20. The distance to this star can be estimated from its annual parallax shift of 13.3 mas, yielding a range of about 246 light years. Based upon measured changes in its proper motion, it may be a close binary system.

53 Virginis is a single, yellow-white hued star in the zodiac constellation of Virgo. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.04. Based upon an annual parallax shift of 29.49±0.29 mas, it is located 111 light years away. The star is moving closer to the Sun with a heliocentric radial velocity of −12.7 km/s. It has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 284±18 mas/yr along a position angle of 162.2°.

References

  1. 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 .
  2. 1 2 3 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. 1 2 3 4 5 6 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv: 1201.2052 , Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID   55586789.
  4. 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048 , Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID   59451347, A61.
  5. ↑ Holmberg, J.; et al. (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   1185775111
  6. 1 2 3 4 5 6 7 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv: 1501.03154 , Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID   33401607.
  7. ↑ Gáspár, András; et al. (August 2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 14, arXiv: 1604.07403 , Bibcode:2016ApJ...826..171G, doi: 10.3847/0004-637X/826/2/171 , S2CID   119241004, 171.
  8. ↑ "23 And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved September 21, 2018.
  9. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society , 389 (2): 869–879, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x , S2CID   14878976.
  10. ↑ Blanco, C.; et al. (November 1982), "Chromospheric MG II emission in A5 to K5 main sequence stars from high resolution IUE spectra", Astronomy and Astrophysics, 115 (2): 280–292, Bibcode:1982A&A...115..280B.
  11. ↑ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv: astro-ph/0412070 , Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID   2603568.
  12. ↑ Koen, Chris; Eyer, Laurent (2002), "New periodic variables from the Hipparcos epoch photometry", Monthly Notices of the Royal Astronomical Society, 331 (1): 45–59, arXiv: astro-ph/0112194 , Bibcode:2002MNRAS.331...45K, doi: 10.1046/j.1365-8711.2002.05150.x , S2CID   10505995
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