HD 30479

Last updated
HD 30479
Observation data
Epoch J2000       Equinox J2000
Constellation Mensa
Right ascension 04h 38m 21.7254s [1]
Declination −77° 39′ 21.6185″ [1]
Apparent magnitude  (V)6.04 ± 0.01 [2]
Characteristics
Spectral type K2 III [3]
U−B color index +0.95 [4]
B−V color index +1.10 [4]
Astrometry
Radial velocity (Rv)10.3 ± 0.1 [5]  km/s
Proper motion (μ)RA: −6.975 [1]   mas/yr
Dec.: −11.166 [1]   mas/yr
Parallax (π)6.0377 ± 0.0223  mas [1]
Distance 540 ± 2  ly
(165.6 ± 0.6  pc)
Absolute magnitude  (MV)−0.05
Details
Mass 1.28 [6]   M☉
Radius 17.99 [7]   R☉
Luminosity 116 [8]   L☉
Surface gravity (log g)2 [9]   cgs
Temperature 4,390 [9]   K
Metallicity [Fe/H]−0.15 [10]   dex
Rotational velocity (v sin i)<1 [11]  km/s
Other designations
13 G. Mensae, CPD−77°181, FK5  2350, GC  5750, HD  30479, HIP  21611, HR  1531, SAO  256116
Database references
SIMBAD data

HD 30479 (HR 1531) is a solitary star in the southern circumpolar constellation Mensa. It has an apparent magnitude of 6.04, [2] making it barely visible to the naked eye even under ideal conditions. It is located at a distance of 540 light years [1] but is receding with a heliocentric radial velocity of 10.3  km/s . [5]

HD 30479 has a stellar classification of K2 III, [3] indicating that it is an early K-type giant star and has an angular diameter of 1.01±0.07  mas [9] (after limb darkening correction). This yields a radius 17.99 [7] times that of the Sun at its estimated distance. At present it has 1.28 [6] times the mass of the Sun and radiates at 116 [8] times the luminosity of the Sun at an effective temperature of 4,390 [9] K from its enlarged photosphere, which gives it an orange glow. HD 30479 is believed to be one of the metal-deficient members of the young disk population [10] with an iron abundance 71% [10] that of the Sun. Currently, it spins leisurely with a projected rotational velocity less than 1  km/s , [11] common for giants.

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Omega Andromedae Binary star system in the constellation Andromeda

Omega Andromedae is the Bayer designation for a slowly co-rotating binary star system in the northern constellation of Andromeda. Parallax measurements made during the Gaia mission make this system to be approximately 93.9 light-years from Earth. Its apparent visual magnitude is +4.83, which makes it bright enough to be seen with the naked eye.

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6 Canis Minoris is a star in the equatorial constellation of Canis Minor, located around 570 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of +4.55. This object is moving closer to the Earth with a heliocentric radial velocity of −16.3 km/s. Kinematically, it is a member of an outlying group belonging to the Ursa Major flow of the Sirius supercluster.

Tau<sup>4</sup> Eridani Star in the constellation Eridanus

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Tau Puppis Star in the southern constellation of Puppis

Tau Puppis, Latinized from τ Puppis, is a star in the southern constellation of Puppis, near the southern constellation boundary with Carina. It is visible to the naked with an apparent visual magnitude of +2.95 and is located at a distance of about 182 light-years from Earth. The variable radial velocity of this system was detected by H. D. Curtis and H. K. Palmer in 1908, based on observations made at the D. O. Mills Observatory. It is a spectroscopic binary star system, with the presence of the secondary component being revealed by the shifts of absorption lines in the spectrum resulting from the Doppler effect. The two components orbit each other with a period of 1,066.0 days and a low eccentricity of 0.090.

HD 197036 is a single star in the northern constellation Cygnus. It has an absolute magnitude of −1.15 and an apparent magnitude of 6.61, below the max naked eye visibility. Located 1,310 light years away, it is approaching Earth with a heliocentric radial velocity of −15 km/s.

HD 88809 is a star located in the southern constellation Antlia. With an apparent magnitude of 5.89 it is barely visible to the naked eye under ideal conditions. The star is located at a distance of around 451 light years but is drifting away at a heliocentric radial velocity of almost 20 km/s.

24 Vulpeculae is a single, yellow-hued star in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.30. The distance to this star can be estimated from its annual parallax shift of 7.9700±0.0674, which yields a separation of roughly 409 light years. It is moving further away with a heliocentric radial velocity of +15 km/s.

Lambda Mensae, Latinized from λ Mensae, is an orange-hued star in the southern constellation of Mensa. It has an apparent visual magnitude of 6.53, which places it at or near the limit on stars visible to the naked eye. According to the Bortle scale, it requires a dark night from rural skies for this star to be viewed. Though it has the designation Lambda, it is actually the twenty-fourth-brightest star in the constellation and not the eleventh-brightest.

HD 200661 is a solitary star in the equatorial constellation Equuleus. It has an apparent magnitude of 6.41, placing it near the max naked eye visibility. The star is situated at a distance of 430 light years but is approaching with a heliocentric radial velocity of −12.1 km/s.

HD 10550 is a single star in the equatorial constellation of Cetus. It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.98. Based upon an annual parallax shift of 2.9564 mas, it is located around 1,100 light years from the Sun. The star is moving closer with a heliocentric radial velocity of −33 km/s. It has a high peculiar velocity of 72.7+5.7
−4.3 km/s and may be a runaway star.

HD 81799 is a suspected astrometric binary star system in the equatorial constellation of Hydra. It is visible to the naked eye with an apparent visual magnitude of 4.69. The distance to this system, as determined from an annual parallax shift of 19.9 mas, is 164 light years. It is moving further away from the Earth with a heliocentric radial velocity of 29 km/s. The system has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 233±19 mas/yr along a position angle of 136°.

GZ Velorum Star in the constellation Vela

GZ Velorum is a single, orange-hued star in the southern constellation of Vela. It is a faint star but visible to the naked eye, having an apparent visual magnitude of 4.58. The star is located around 1,300 light years from Earth, as determined from its annual parallax shift of 2.4 mas. It is moving further away with a heliocentric radial velocity of +13 km/s.

HD 89998 is a single star in the southern constellation of Vela. It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.82. The distance to HD 89998, as determined from its annual parallax shift of 15.9 mas, is 205 light years. The star is moving further from the Earth with a heliocentric radial velocity of +21 km/s, having come within 140 ly some 1.552 million years ago.

3 Piscis Austrini, also known as HD 201901, is a suspected astrometric binary star system that, despite its Flamsteed designation, is actually located in the constellation Microscopium. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.41. The system is moving closer to the Earth with a heliocentric radial velocity of −46 km/s. It is following a highly elliptical orbit around the Galactic Center, moving between a pericenter of 2.6 kpc out to an apocenter of 7.6 kpc, with an orbital eccentricity of 0.49.

HD 32515 is a solitary star located in the southern constellation Caelum. It has an apparent magnitude of 5.9, making it faintly visible to the naked eye under ideal conditions. The star is situated at a distance of 326 light years but is recceding with a heliocentric radial velocity of 29.4 km/s.

HD 166006 is a double star in the southern constellation Telescopium. With an apparent magnitude of around 6, it is barely visible to the naked eye under ideal conditions. The star is located 582 light-years based on parallax, but is drifting closer with a heliocentric radial velocity of 16.5 km/s.

Iota Octantis, Latinized, from ι Octantis is a double star in the southern circumpolar constellation Octans. The "A" component has an apparent magnitude of 5.83, making it faintly visible to the naked eye under ideal conditions, but the "B" component can't be seen due to its faintness. The system is located at a distance of 350 light years based on its annual parallax shift, but is drifting away at a rate of 53.4 km/s.

HD 196775 is a solitary star in the equatorial constellation Delphinus. It has an apparent magnitude of 5.98, allowing it to be faintly seen with the naked eye. The object is relatively far at a distance of 1,050 light years but is approaching the Solar System with a heliocentric radial velocity of −4.6 km/s. HD 196775 has a high peculiar velocity of 21.8+1.9
−4.1 km/s compared to neighboring stars, indicating that it may be a runaway star.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  3. 1 2 Houk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations -90_ to -53_ƒ0. Bibcode:1975mcts.book.....H.
  4. 1 2 Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
  5. 1 2 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.
  6. 1 2 Anders, F.; et al. (1 August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi: 10.1051/0004-6361/201935765 . ISSN   0004-6361. S2CID   131780028.
  7. 1 2 Lang, Kenneth R. (2006). Astrophysical formulae. Astronomy and astrophysics library. Vol. 1 (3 ed.). Birkhäuser. ISBN   3-540-29692-1.. The radius (R*) is given by:
  8. 1 2 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017). "Fundamental parameters and infrared excesses of Tycho-Gaia stars". Monthly Notices of the Royal Astronomical Society. 471 (1): 770. arXiv: 1706.02208 . Bibcode:2017MNRAS.471..770M. doi: 10.1093/mnras/stx1433 .
  9. 1 2 3 4 Lafrasse, Sylvain; Mella, Guillaume; Bonneau, Daniel; Duvert, Gilles; Delfosse, Xavier; Chesneau, Olivier; Chelli, Alain (16 July 2010). "Building the 'JMMC Stellar Diameters Catalog' using SearchCal". Optical and Infrared Interferometry II. Vol. 7734. pp. 77344E. arXiv: 1009.0137 . Bibcode:2010SPIE.7734E..4EL. doi:10.1117/12.857024. S2CID   32097037.
  10. 1 2 3 Eggen, O. J. (February 1994). "Evolved GK stars near the Sun. 2: The young disk population". The Astronomical Journal. 107: 594. Bibcode:1994AJ....107..594E. doi: 10.1086/116879 . ISSN   0004-6256.
  11. 1 2 De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014). "A catalog of rotational and radial velocities for evolved stars: V. Southern stars⋆⋆⋆". Astronomy & Astrophysics. 561: A126. arXiv: 1312.3474 . Bibcode:2014A&A...561A.126D. doi: 10.1051/0004-6361/201220762 . ISSN   0004-6361.
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