HD 66920

Last updated
HD 66920
Observation data
Epoch J2000       Equinox J2000
Constellation Volans
Right ascension 07h 59m 15.7648s [1]
Declination −73° 14′ 39.0155″ [1]
Apparent magnitude  (V)6.33±0.01 [2]
Characteristics
Evolutionary stage main sequence [1]
Spectral type A3 V [3]
U−B color index +0.13 [4]
B−V color index +0.14 [4]
Astrometry
Radial velocity (Rv)23.8±1.7 [5]  km/s
Proper motion (μ)RA: −5.984  mas/yr [1]
Dec.: −20.295  mas/yr [1]
Parallax (π)7.6204 ± 0.0251  mas [1]
Distance 428 ± 1  ly
(131.2 ± 0.4  pc)
Absolute magnitude  (MV)+0.76 [6]
Details
Mass 2.33 [7]   M☉
Radius 3.53+0.13
−0.11 [8]   R☉
Luminosity 42±2 [9]   L☉
Surface gravity (log g)3.65±0.08 [8]   cgs
Temperature 8,247±95 [10]   K
Metallicity [Fe/H]−0.01 [11]   dex
Age 711 [1]   Myr
Other designations
20 G. Volantis [12] , CD−72°431, CPD−72°654, GC  10898, HD  66920, HIP  39041, HR  3171, SAO  256463 [13]
Database references
SIMBAD data

HD 66920, also known as HR 3171, is a solitary, white hued star located in the southern circumpolar constellation Volans, the flying fish. It has an apparent magnitude of 6.33, [2] placing it near the limit for naked eye visibility. Based on parallax measurements from the Gaia spacecraft, the star is estimated to be 428 light years distant. [1] It appears to be receding from the Solar System, having a heliocentric radial velocity of 23.8  km/s . [5] Pauzen et al. (2001) listed it as a λ Boötis star, [3] but is now considered a non member. [14]

HD 66920 has a classification of A3 V, [3] indicating that it is an ordinary A-type main-sequence star. Although it has been classified as a giant star (III), [15] HR 3171 is still on the main sequence [1] (according to Gaia DR3 models). It has 2.33 times the mass of the Sun and an enlarged radius of 3.53  R☉. [8] It radiates 42 times the luminosity of the Sun [9] from its enlarged photosphere at an effective temperature of 8,247  K . [10] HD 66920 has a solar metallicity, [11] and is estimated to be 711 million years old. [1]

Related Research Articles

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<span class="mw-page-title-main">Beta Coronae Australis</span> Star in the constellation Corona Australis

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<span class="mw-page-title-main">Q Scorpii</span> High proper motion binary star system in the constellation of Scorpius

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<span class="mw-page-title-main">HD 154972</span> Star in the constellation of Apus

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HD 30080, also known as HR 1509, is a solitary, orange hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 5.66, allowing it to be faintly visible to the naked eye. Parallax measurements from Gaia DR3 place the object at a distance of 612 light years. It appears to be approaching the Solar System with a heliocentric radial velocity of −3.8 km/s. Eggen (1989) lists it as a member of the thick disk population.

<span class="mw-page-title-main">10 Trianguli</span> Star in the constellation Triangulum

10 Trianguli, or simply 10 Tri is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.29. Gaia DR3 parallax measurements imply a distance of 363 light-years and it is slowly receding with a heliocentric radial velocity of 0.4 km/s. At its current distance, 10 Tri's brightness is diminished by an interstellar extinction of 0.11 magnitudes and it has an absolute magnitude of −0.02.

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HD 30669 is a yellowish-orange hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 9.11, making it readily visible in small telescopes but not to the naked eye. The object is relatively close at a distance of 188 light years, based on parallax measurements from Gaia DR3. Its distance from the Solar System is rapidly increasing, having a heliocentric radial velocity of 66 km/s.

HD 218108, also known as HR 8786, is a solitary, white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.11, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from Gaia DR3, the object is estimated to be 247 light years away. It appears to be approaching the Solar System with a fairly constrained radial velocity of −7 km/s. Paunzen et al. (2001) lists it as a λ Boötis star with a weak magnesium line.

<span class="mw-page-title-main">HD 168592</span> Star in the constellation of Corona Australis

HD 168592, also designated as HR 6862 or rarely 7 G. Coronae Australis, is a solitary star located in the southern constellation Corona Australis. It is faintly visible to the naked eye as an orange-hued star with an apparent magnitude of 5.07. Gaia DR3 parallax measurements place it at a distance of 490 light years and is currently receding with a heliocentric radial velocity of 18 km/s. At its current distance, HD 168592's brightness is diminished by 0.38 magnitudes due to interstellar dust. It has an absolute magnitude of −0.76.

<span class="mw-page-title-main">HD 31134</span> Star in the constellation of Camelopardalis

HD 31134, also designated as HR 1561, is a solitary star located in the northern circumpolar constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued star with an apparent magnitude of 5.74. Gaia DR3 parallax measurements place it 473 light years away. It appears to be approaching the Solar System with a heliocentric radial velocity of −15.1 km/s. At its current distance, HD 31134's brightness is diminished by 0.35 magnitudes due to interstellar dust. It has an absolute magnitude of +0.19.

<span class="mw-page-title-main">HD 182893</span> Star in the constellation Telescopium

HD 182893, also known as HR 7388 or rarely 60 G. Telescopii, is a solitary, yellowish-orange hued star located in the southern constellation Telescopium. It has an apparent magnitude of 6.13, making it barely visible to the naked eye even under ideal conditions. Based on Gaia DR3 parallax measurements, the object is estimated to be 328 light years away. However, it is approaching the Solar System with a heliocentric radial velocity of −27 km/s. At its current distance, HD 182893's brightness is diminished by 0.19 magnitudes due to interstellar dust. It has an absolute magnitude of +1.23.

<span class="mw-page-title-main">HD 189080</span> Star in the constellation of Telescopium

HD 189080, also known as HR 7621 or rarely 74 G. Telescopii, is a solitary orange-hued star located in the southern constellation Telescopium. It has an apparent magnitude of 6.18, placing it near the limit for naked eye visibility. Gaia DR3 parallax measurements place it at a distance of 357 light years and it is currently receding rapidly with a heliocentric radial velocity of 66.9 km/s. At its current distance, HD 189080's brightness is diminished by 0.17 magnitudes due to extinction from interstellar dust. It has an absolute magnitude of +1.1.

<span class="mw-page-title-main">QQ Telescopii</span> Delta Scuti variable; Telescopium

QQ Telescopii, also known as HD 185139 or simply QQ Tel, is a solitary variable star located in the southern constellation Telescopium. It has an apparent magnitude of 6.25, placing it near the limit for naked eye visibility, even under ideal conditions. Gaia DR3 parallax measurements imply a distance of 333 light years and it is currently receding with a heliocentric radial velocity of 7.8 km/s. At its current distance, QQ Telescopii's brightness is diminished by two tenths of a magnitude due to interstellar dust and it has an absolute magnitude of +1.01.

HD 181295 is a star located in the southern constellation Telescopium. It has an apparent magnitude of 6.42, placing it near the limit of naked eye visibility, even under ideal conditions. The object is located relatively close at a distance of approximately 252 light-years based on Gaia DR3 parallax measurements, and it is currently drifting closer with a heliocentric radial velocity of −35.7 km/s. At its current distance, HD 181295's brightness is diminished by 0.22 magnitudes due to interstellar extinction and it has an absolute magnitude +2.14.

References

  1. 1 2 3 4 5 6 7 8 9 10 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 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (1 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 3 Paunzen, E.; Duffee, B.; Heiter, U.; Kuschnig, R.; Weiss, W. W. (July 2001). "A spectroscopic survey for λ Bootis stars". Astronomy & Astrophysics. 373 (2): 625–632. Bibcode:2001A&A...373..625P. doi: 10.1051/0004-6361:20010630 . eISSN   1432-0746. ISSN   0004-6361.
  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 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN   1562-6873. ISSN   1063-7737. S2CID   119231169.
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  7. ↑ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv: 2109.10912 . Bibcode:2022A&A...657A...7K. doi: 10.1051/0004-6361/202142146 . eISSN   1432-0746. ISSN   0004-6361.
  8. 1 2 3 Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . eISSN   1538-3881.
  9. 1 2 Murphy, Simon J.; Paunzen, Ernst (5 December 2016). "Gaia's view of the λ Boo star puzzle". Monthly Notices of the Royal Astronomical Society. 466 (1): 546–555. arXiv: 1612.01528 . Bibcode:2017MNRAS.466..546M. doi: 10.1093/mnras/stw3141 . eISSN   1365-2966. ISSN   0035-8711.
  10. 1 2 Paunzen, E.; Schnell, A.; Maitzen, H. M. (October 2006). "An empirical temperature calibration for the Δa photometric system II: The A-type and mid F-type stars". Astronomy & Astrophysics. 458 (1): 293–296. arXiv: astro-ph/0607567 . Bibcode:2006A&A...458..293P. doi: 10.1051/0004-6361:20064889 . eISSN   1432-0746. ISSN   0004-6361.
  11. 1 2 Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv: 1606.08814 . Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. ISSN   0320-0108. S2CID   255201789.
  12. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  13. ↑ "HD 66920". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved September 7, 2022.
  14. ↑ Murphy, Simon J.; Corbally, Christopher J.; Gray, Richard O.; Cheng, Kwang-Ping; Neff, James E.; Koen, Chris; Kuehn, Charles A.; Newsome, Ian; Riggs, Quinlin (2015). "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue". Publications of the Astronomical Society of Australia. 32. arXiv: 1508.03633 . Bibcode:2015PASA...32...36M. doi: 10.1017/pasa.2015.34 . eISSN   1448-6083. ISSN   1323-3580.
  15. ↑ 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°. Bibcode:1975mcts.book.....H.
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