62 Andromedae

Last updated
62 Andromedae
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 02h 19m 16.79693s [1]
Declination +47° 22′ 47.9132″ [1]
Apparent magnitude  (V)5.31 [2]
Characteristics
Spectral type A0V [3]
B−V color index 0.00425 [4]
Astrometry
Radial velocity (Rv)−29.6±2.8 [5]  km/s
Proper motion (μ)RA: –60.03 [6]   mas/yr
Dec.: –5.61 [6]   mas/yr
Parallax (π)11.9531 ± 0.1640  mas [1]
Distance 273 ± 4  ly
(84 ± 1  pc)
Absolute magnitude  (MV)0.93 [7]
Details
Mass 2.42±0.02 [8]   M☉
Radius 1.8 [2]   R☉
Luminosity 45.2+2.1
−1.9 [8]   L☉
Temperature 9,572+133
−131 [8]   K
Rotational velocity (v sin i)86 [9]  km/s
Other designations
c Andromedae [10] , 62 And, BD+46°552, FK5  1063, HD  14212, HIP  10819, HR  670, SAO  37948 [11]
Database references
SIMBAD data

62 Andromedae, abbreviated 62 And, is a single [12] star in the northern constellation Andromeda. 62 Andromedae is the Flamsteed designation; it also bears the Bayer designation of c Andromedae. [10] 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 (84 parsecs) from Earth. [1] The star is moving closer to the Earth with a heliocentric radial velocity of −30 km/s, [5] and is predicted to come to within 144.6 light-years in 1,6 million years. [7]

This is an A-type main-sequence star with a stellar classification of A0 V. [13] Abt and Morrel (1995) gave it a class of A1 III, [14] [7] matching a more evolved giant star. The star has 2.42 [8] times the mass of the Sun, about 1.8 [2] times the Sun's radius, and is spinning with a projected rotational velocity of 86 km/s. [8] It is radiating 45 [8] times the Sun's luminosity from its photosphere at an effective temperature of 9,572 K. [8]

Related Research Articles

<span class="mw-page-title-main">70 Virginis</span> Star in the constellation Virgo

70 Virginis is a binary star located 58 light years from the Sun in the equatorial constellation of Virgo, near the northern constellation border with Coma Berenices. 70 Virginis is its Flamsteed designation. The star is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of +4.97. It is drifting further away with a heliocentric radial velocity of +4.4 km/s and has a high proper motion, traversing the celestial sphere at the rate of 0.621 arc seconds per annum.

<span class="mw-page-title-main">Lambda Serpentis</span> Star in the constellation Serpens

Lambda Serpentis, Latinized from λ Serpentis, is a star in the constellation Serpens, in its head. It has an apparent visual magnitude of 4.43, making it visible to the naked eye. Based upon parallax measurements, this star lies at a distance of about 38.9 light-years from Earth. Lambda Serpentis is moving toward the Solar System with a radial velocity of 66.4 km s−1. In about 166,000 years, this system will make its closest approach of the Sun at a distance of 7.371 ± 0.258 light-years, before moving away thereafter.

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

Tau Andromedae, Latinized from τ Andromedae, is the Bayer designation for a single star in the northern constellation of Andromeda. It has an apparent visual magnitude of +4.94, which is bright enough to be viewed from dark suburban skies. From parallax measurements made during the Gaia mission, the distance to this star can be estimated as roughly 680 light-years from Earth. The brightness of this star is diminished by 0.24 in magnitude due to extinction caused by intervening gas and dust. It is drifting closer to the Sun with a radial velocity of −14 km/s.

<span class="mw-page-title-main">8 Andromedae</span> Mulitple star system in the constellation Andromeda

8 Andromedae, abbreviated 8 And, is a probable triple star system in the northern constellation of Andromeda. 8 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.82. Based upon an annual parallax shift of 5.7 mas, it is located about 570 light years from the Earth. It is moving closer with a heliocentric radial velocity of −8 km/s.

23 Andromedae, abbreviated 23 And, is a presumed single star in the constellation Andromeda, although it has been a suspected spectroscopic binary. 23 Andromedae is the Flamsteed designation. Its apparent visual magnitude is 5.71, 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, is 121.6 light years. The star is moving further from the Earth with a heliocentric radial velocity of −27 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.191″ per year.

<span class="mw-page-title-main">26 Andromedae</span> Star in the constellation Andromeda

26 Andromedae, abbreviated 26 And, is a binary star system in the constellation Andromeda. 26 Andromedae is the Flamsteed designation. It has a combined apparent visual magnitude of 6.10, which is near the lower limit of visibility to the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.35 mas, which yields a distance of about 600 light years. At that distance, the visual magnitude of the stars is diminished from an extinction of 0.04 due to interstellar dust. The system is moving further from the Earth with a heliocentric radial velocity of +3.3 km/s.

22 Aurigae is a star located 537 light years away from the Sun in the northern constellation Auriga. It is just bright enough to be barely visible to the naked eye under good viewing conditions, appearing as a blue-white hued star with an apparent visual magnitude of 6.45. At the distance of this object, the brightness is diminished by an extinction of 0.57 due to interstellar dust. The star is moving further from the Earth with a heliocentric radial velocity of +10 km/s, and it is a member of the Taurion OB association, located between Orion and Taurus.

10 Boötis is a suspected astrometric binary star system in the northern constellation of Boötes, located around 528 light years away from the Sun. It is visible to the naked eye under suitable viewing conditions as a dim, white-hued star with an apparent visual magnitude of 5.76. Its magnitude is diminished by an extinction of 0.17 due to interstellar dust. This system is moving away from the Earth with a heliocentric radial velocity of +6 km/s.

29 Cancri is a star in the zodiac constellation of Cancer, located 370 light years from the Sun. It is just visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.94. The star is situated near the ecliptic, which means it is subject to lunar occultations.

μ Lyrae, Latinized as Mu Lyrae, is a solitary star in the northern constellation Lyra. It has the traditional name Alathfar, from the Arabic الأظفارal-ʼaẓfār "the talons ", a name it shares with Eta Lyrae. This white-hued object is visible to the naked eye as faint point of light with an apparent visual magnitude of 5.11. It is located approximately 412 light years distant from the Sun based on parallax, but is drifting closer with a radial velocity of −24 km/s.

HD 4628 is a main sequence star in the equatorial constellation of Pisces. It has a spectral classification of K2.5 V and an effective temperature of 5,055 K, giving it an orange-red hue with a slightly smaller mass and girth than the Sun. HD 4628 lies at a distance of approximately 24.3 light years from the Sun based on parallax. The apparent magnitude of 5.7 is just sufficient for this star to be viewed with the unaided eye. The star appears to be slightly older than the Sun—approximately 5.4 billion years in age. The surface activity is low and, based upon the detection of UV emission, it may have a relatively cool corona with a temperature of one million K.

Gliese 673 is an orange dwarf star in the constellation Ophiuchus. It has a stellar classification of K7V. Main sequence stars with this spectra have a mass in the range of 60–70% of solar mass (M☉).

<span class="mw-page-title-main">Omega Cassiopeiae</span> Binary star system in constellation Cassiopeia

Omega Cassiopeiae is a binary star system in the northern constellation of Cassiopeia. It has a combined apparent visual magnitude of +4.99, which means it is a faint star but visible to the naked eye. Based upon an annual parallax shift of 4.65 mas as seen from Earth, this system is located roughly 730 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.16 due to interstellar dust.

HD 11964 is a binary star system located 110 light-years away from the Sun in the equatorial constellation of Cetus. It is visible in binoculars or a telescope but is too faint to be seen with the naked eye, having an apparent visual magnitude of 7.51. The system is drifting closer to the Sun with a radial velocity of −9 km/s. Two extrasolar planets have been confirmed to orbit the primary.

<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.

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

KK Andromedae, also known as HD 9531, is a variable star in the northern constellation of Andromeda. It has an apparent visual magnitude of 5.90, which places it near the lower limit of visibility to the naked eye even under good viewing conditions. An Alpha2 Canum Venaticorum variable, it varies in brightness by 0.012 magnitude every 0.66 days. Based upon an annual parallax shift of 7.5 mas as seen from Earth, it is located around 437 light years from the Sun. At that distance, the brightness of the star is diminished by an extinction of 0.26 magnitude due to interstellar dust.

Tau2 Serpentis, Latinized from τ2 Serpentis, is a star in the constellation of Serpens, located approximately 480 light-years from the Sun. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.22. The star is drifting closer with a radial velocity of −19 km/s.

67 Aquarii is a star located 484 light years away from the Sun in the zodiac constellation of Aquarius. 67 Aquarii is its Flamsteed designation. It is a dim, blue-white hued star near the lower limit of visibility to the naked eye with an apparent visual magnitude of 6.40. At the distance of this star, its visual magnitude is diminished by an extinction of 0.11 due to interstellar dust. The position of this star near the ecliptic means it is subject to lunar eclipses.

<span class="mw-page-title-main">55 Persei</span> Star in the constellation Perseus

55 Persei is a single, blue-white hued star in the northern constellation Perseus. It is faintly visible to the naked eye under good seeing conditions, having an apparent visual magnitude of 5.73. Based upon an annual parallax shift of 8.50±0.38 mas as seen from Earth's orbit, the star is located about 380 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.39 due to interstellar dust.

<span class="mw-page-title-main">Nu Leonis</span> Binary star system in the constellation Leo

ν Leonis, Latinised as Nu Leonis, is a binary star system in the zodiac constellation of Leo. It is faintly visible to the naked eye with an apparent visual magnitude of 5.15; parallax measurements indicate it is around 500 light years away. At this distance, the visual extinction from interstellar dust is 0.33 magnitudes.

References

  1. 1 2 3 4 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 Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy & Astrophysics, 367 (2): 521–524, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi: 10.1051/0004-6361:20000451 .
  3. ↑ van Belle, Gerard T.; von Braun, Kaspar (2009), "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars", The Astrophysical Journal, 694 (2): 1085–1098, arXiv: 0901.1206 , Bibcode:2009ApJ...694.1085V, doi:10.1088/0004-637X/694/2/1085, S2CID   18370219.
  4. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
  5. 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.
  6. 1 2 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600. Vizier catalog entry
  7. 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.
  8. 1 2 3 4 5 6 7 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, A120.
  9. ↑ Royer, F.; et al. (2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy & Astrophysics, 393: 897–911, arXiv: 1201.2052 , Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID   14070763.
  10. 1 2 Tirion, Wil; Rappaport, Barry (1987), Remaklus, Will (ed.), Uranometria 2000.0 - Volume II - The Southern Hemisphere to +6°, Richmond, Virginia, USA, ISBN   0-943396-15-8.
  11. ↑ "62 And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved October 4, 2018.
  12. ↑ 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.
  13. ↑ van Belle, Gerard T.; von Braun, Kaspar (2009), "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars", The Astrophysical Journal (abstract), 694 (2): 1085–1098, arXiv: 0901.1206 , Bibcode:2009ApJ...694.1085V, doi:10.1088/0004-637X/694/2/1085, S2CID   18370219
  14. ↑ Abt, Helmut A.; Morrell, Nidia I. (July 1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi: 10.1086/192182 .
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.