HR 4180

Last updated
HD 92449
Observation data
Epoch J2000       Equinox J2000
Constellation Vela
HD 92449
Right ascension 10h 39m 18.3925s [1]
Declination −55° 36 11.765 [1]
Apparent magnitude  (V)4.29 [2]
HD 92463
Right ascension 10h 39m 24.2778s [3]
Declination −55° 36 25.642 [3]
Characteristics
Spectral type G5 IIa [4] + B8 V [5]
B−V color index 1.025±0.003 [2]
Astrometry
HD 92449
Radial velocity (Rv)+20.1±0.7 [6]  km/s
Proper motion (μ)RA: −19.032(91)  mas/yr [1]
Dec.: 5.032(90)  mas/yr [1]
Parallax (π)4.1595 ± 0.0940  mas [1]
Distance 780 ± 20  ly
(240 ± 5  pc)
Absolute magnitude  (MV)−2.76 [2]
HD 92463
Proper motion (μ)RA: −18.941(40)  mas/yr [3]
Dec.: 5.386(42)  mas/yr [3]
Parallax (π)4.2647 ± 0.0405  mas [3]
Distance 765 ± 7  ly
(234 ± 2  pc)
Details
Luminosity 1370.29 [7]   L
Temperature 5,100 [7]   K
Other designations
x Vel, HR  4180, WDS J10393-5536
A: CD−54 3915, HD  92449, HIP  52154, SAO  238309
B: CD−54 3675, HD  92463, SAO  238313
Database references
SIMBAD HD 92449
HD 92463

HR 4180 is a double star with components HD 92449 and HD 92463 in the southern constellation of Vela. They are probably members of a binary star system. [8] HR 4180 can be viewed with the naked eye, having an apparent visual magnitude of 4.29. [2] Based upon the annual parallax shift of the two stars it is located approximately 780  light years from the Sun. [1] [3] The system is moving further from the Earth with a heliocentric radial velocity of +20 km/s. [6]

The primary component of this system, HD 92449, is a bright giant with a stellar classification of G5 IIa. [4] The star radiates 1,370 times the Sun's luminosity from its photosphere at an effective temperature of 5,100 K. [7] It shares a common proper motion with the magnitude 6.06 [9] star HD 92463, [10] and the pair likely form a binary system. [8] This secondary component is a B-type main-sequence star with a class of B8 V. [5] As of 2000, it had an angular separation of 51.70 along a position angle of 105° from the primary. [9]

Related Research Articles

<span class="mw-page-title-main">9 Aurigae</span> Multiple star system in the constellation Auriga

9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.

Mu Boötis, Latinized from μ Boötis, consists of a pair of double stars in the northern constellation of Boötes, 120 light-years from the Sun.

24 Cancri is a triple star system in the constellation Cancer. The system is located about 226 light-years away, based on its parallax. The system has a combined apparent magnitude of 6.5, and the two components A and B are separated by 5.7″.

<span class="mw-page-title-main">9 Vulpeculae</span> Star in the constellation Vulpecula

9 Vulpeculae is a star in the northern constellation of Vulpecula, located about 560 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.01. The star is moving further from the Earth with a heliocentric radial velocity of +5 km/s.

<span class="mw-page-title-main">IC 2391</span> Open star cluster in the constellation Vela

IC 2391 is an open cluster in the constellation Vela consisting of hot, young, blueish stars, some of which binaries and one of which is a quadruple. Persian astronomer A. a.-R. al-Sufi first described it as "a nebulous star" in c. 964. It was re-found by Abbe Lacaille and cataloged as Lac II 5.

HD 115404 is a binary star system located in the constellation Coma Berenices. Parallax measurements made by Hipparcos put the system at 36 light-years, or 11 parsecs, away. The combined apparent magnitude of the system is 6.52, with the magnitudes of the components being 6.66 and 9.50.

HD 1185 is a double star in the northern constellation of Andromeda. The primary, with an apparent magnitude of 6.15, is a white main-sequence star of spectral type A2VpSi, indicating it has stronger silicon absorption lines than usual, thus making it also an Ap star. The secondary companion, which is 9.08 arcseconds away, is not visible to the naked eye at an apparent magnitude of 9.76. It shares common proper motion and parallax with the primary star but orbital parameters are still unknown.

HD 88836, also known as HR 4019, is a solitary, yellow-hued star located in the southern constellation Antlia. It has an apparent magnitude of 6.32, placing it near the limit for naked eye visibility. Based on an annual parallax shift of 7.019 mas, the object is estimated to be 465 light years away from the Solar System. Its distance from the Sun does not appear to be changing, having a radial velocity of 0 km/s.

HD 156768 is a double star in the southern constellation of Ara, with a combined apparent magnitude of 5.86. The brighter component is a sixth magnitude bright giant or supergiant star with a stellar classification of G8Ib/II. The magnitude 9.6 companion lies at an angular separation of 1.81″ along a position angle of 184°.

<span class="mw-page-title-main">HD 158476</span> Star in the constellation Ara

HD 158476 is a supergiant star in the southern constellation of Ara. There is a faint magnitude 10.5 companion at an angular separation of 20.0″ along a position angle of 209°.

HD 135438 is a K-type giant star in the northern constellation of Boötes. With an apparent magnitude of 6.0, it lies about 650 light years away.

HD 106515 is a binary star in the constellation of Virgo.

<span class="mw-page-title-main">1 Puppis</span> Star in the constellation Puppis

1 Puppis is a single star in the southern constellation of Puppis. It lies in the northern part of the constellation at a distance of about 790 ly, east of Aludra in Canis Major and just north of the white supergiant, 3 Puppis. This object is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.59. It is moving further from the Earth with a heliocentric radial velocity of +32.4 km/s.

<span class="mw-page-title-main">HD 59612</span> Star in the constellation Puppis

HD 59612 is a class A5Ib supergiant star in the constellation Puppis. Its apparent magnitude is 4.86 and it is approximately 4,300 light years away based on parallax.

57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.4 mas provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).

<span class="mw-page-title-main">31 Cygni</span> Triple star system in the constellation Cygnus

31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, ο2 Cygni or V695 Cygni, is a ternary star system about 750 light years away in the constellation Cygnus.

<span class="mw-page-title-main">HD 53367</span> Binary star system in the constellation Monoceros

HD 53367 is a triple star system in the constellation of Monoceros. The primary star was identified as a variable Herbig Ae/Be star in 1989. Its companion, spectroscopically discovered in 2006, is a pre-main-sequence star star with an average separation of 1.7 AU. The star system is embedded in the extended nebula IC 2177.

7 Tauri is a multiple star in the northern constellation of Taurus. It has a combined apparent visual magnitude of 5.95, so, according to the Bortle scale, it is faintly visible from suburban skies at night. Measurements made with the Gaia spacecraft show an annual parallax shift of 5.5 mas, which is equivalent to a distance of around 593 light years from the Sun.

<span class="mw-page-title-main">RS Sagittarii</span> Eclipsing binary star system in the constellation Sagittarius

RS Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated RS Sgr. It is a double-lined spectroscopic binary with an orbital period of 2.416 days, indicating that the components are too close to each other to be individually resolved. The system has a combined apparent visual magnitude of 6.01, which is bright enough to be faintly visible to the naked eye. During the primary eclipse the brightness drops to magnitude 6.97, while the secondary eclipse is of magnitude 6.28. The distance to this system is approximately 1,420 light years based on parallax measurements.

References

  1. 1 2 3 4 5 6 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 4 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 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.
  4. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. S2CID   123149047.
  5. 1 2 Houk, Nancy; Cowley, A. P. (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  6. 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.
  7. 1 2 3 McDonald, I.; et al. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–357, arXiv: 1208.2037 , Bibcode:2012MNRAS.427..343M, doi: 10.1111/j.1365-2966.2012.21873.x , S2CID   118665352.
  8. 1 2 Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . S2CID   14878976.
  9. 1 2 Mason, B. D.; et al. (2008). "Washington Visual Double Star Catalog, 2006.5 (WDS)". U. S. Naval Observatory, Washington D.C. Archived from the original on 2011-02-14. Retrieved 2018-08-13.
  10. Eggen, O. J. (June 15, 1980). "VY Carinae, S Normae, and photometric luminosities for bright giants and supergiants of types G and K". Astrophysical Journal, Part 1. 238: 919–928. Bibcode:1980ApJ...238..919E. doi:10.1086/158055.