HR 3159

Last updated
HR 3159
Observation data
Epoch J2000.00       Equinox J2000.00
Constellation Carina
Right ascension 08h 00m 19.96678s [1]
Declination −63° 34′ 02.8420″ [1]
Apparent magnitude  (V)4.81 [2]
Characteristics
Spectral type B4V [3]
B−V color index −0.173±0.007 [2]
Astrometry
Radial velocity (Rv)+22.1±2.8 [2]  km/s
Proper motion (μ)RA: −1.89 [1]   mas/yr
Dec.: 19.21 [1]   mas/yr
Parallax (π)6.53 ± 0.13  mas [1]
Distance 499 ± 10  ly
(153 ± 3  pc)
Absolute magnitude  (MV)−1.11 [2]
Details
Mass 6.3±0.1 [4]   M☉
Radius 3.77±0.27 [5]   R☉
Luminosity 912 [6]   L☉
Surface gravity (log g)4.03±0.05 [5]   cgs
Temperature 16,983 [6]   K
Metallicity [Fe/H]−0.09±0.06 [7]   dex
Rotational velocity (v sin i)43 [6]  km/s
Age 17.2±1.3 [4] or 176 [8]   Myr
Other designations
D Car, CD−63°866, FK5  2624, GC  10893, HD  66591, HIP  39138, HR  3159, SAO  250069 [9]
Database references
SIMBAD data

HR 3159 is a single [10] star in the southern constellation of Carina, positioned near the southern constellation border with Volans. It has the Bayer designation D Carinae; HR 3159 is the Bright Star Catalogue designation. This object has a blue-white hue and is visible to the naked eye with an apparent visual magnitude of +4.81. [2] It is located at a distance of approximately 499  light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of 22 km/s.

This object is a B-type main-sequence star with a stellar classification of B4V, [3] which indicates it is undergoing core hydrogen fusion. The star has a radius of nearly four times the radius of the Sun, [5] and over six [4] times the Sun's mass. Age estimates range from 17 [4] up to 176 [8]  million years old, and it is spinning with a projected rotational velocity of 43 km/s. [6] It is radiating 912 [6] times the luminosity of the Sun from its photosphere at an effective temperature of 16,983 K. [6]

Related Research Articles

Theta<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Theta1 Sagittarii (θ1 Sagittarii) is a close binary star system in the zodiac constellation of Sagittarius. It is visible to the naked eye with an apparent visual magnitude of 4.37. Based upon an annual parallax shift of 6.29 mas as seen from Earth, this star is located around 520 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.24 due to interstellar dust.

<span class="mw-page-title-main">Theta Volantis</span> A-type main sequence star in the constellation Volans

Theta Volantis, Latinized from θ Volantis, is a solitary star in the southern constellation of Volans. Based upon parallax measurements, is approximately 240 light years from the Sun. It has an apparent visual magnitude of 5.19, which is bright enough to be faintly visible to the naked eye.

15 Aquarii, abbreviated 15 Aqr, is a single, blue-white star in the zodiac constellation of Aquarius. 15 Aquarii is the Flamsteed designation. It is a dim star that is just visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.83. Based upon an annual parallax shift of 4.6 mas, it is located around 710 light years away. At that distance, the visual magnitude is diminished by an extinction of 0.18 due to interstellar dust. It is moving closer to the Earth with a heliocentric radial velocity of −9 km/s. Relative to its neighbors, 15 Aqr has a peculiar velocity of 28.7+2.9
−3.1 km/s and may be a runaway star.

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.

Lambda Canis Majoris is a solitary, blue-white hued star in the constellation Canis Major. Lambda CMa is visible to the naked eye with an apparent visual magnitude of +4.48. Based upon an annual parallax shift of 7.70 mas as seen from Earth, this star is located about 424 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.14 due to interstellar dust.

<span class="mw-page-title-main">Lambda Capricorni</span> A-type main sequenece star in the constellation Capricornus

Lambda Capricorni, Latinized from λ Capricorni, is a solitary star in the southern constellation of Capricornus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.56. Based upon an annual parallax shift of 11.58 mas as seen from the Earth, the star is located about 282 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.11 due to interstellar dust.

42 Camelopardalis is a single star in the constellation Camelopardalis, located roughly 770 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.14. The visual magnitude of the star is diminished by an extinction of 0.22 due to interstellar dust. It is moving further from the Earth with a heliocentric radial velocity of 3 km/s. 42 Camelopardalis has a peculiar velocity of 24.4+1.9
−2.1 km/s and may be a runaway star.

Xi<sup>2</sup> Centauri Triple star system in the constellation Centaurus

Xi2 Centauri, Latinized from ξ2 Centauri, is a triple star system in the southern constellation of Centaurus. It is visible to the naked eye with an apparent visual magnitude of 4.30, and forms a wide optical double with the slightly dimmer ξ1 Centauri. Based upon an annual parallax shift of 6.98 mas, Xi2 Centauri lies roughly 470 light years from the Sun. At that distance, the visual magnitude is diminished by an interstellar extinction factor of 0.32 due to intervening dust.

G Centauri is a single star in the southern constellation of Centaurus. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of +4.82. This object is located approximately 450 light years from the Sun, based on parallax. It is a member of the Lower Centaurus–Crux group of the Scorpius–Centaurus association, with the former having an age of about 17 million years.

HD 111597 is a suspected astrometric binary star system in the southern constellation of Centaurus. It has the Bayer designation p Centauri, while HD 111597 is the star's identifier 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 4.90. It is located at a distance of approximately 380 light years from the Sun based on parallax, and has an absolute magnitude of −0.53. The system is a probable member of the Sco OB2 association of co-moving stars. The visible component is a B-type main-sequence star with a stellar classification of B9V.

2 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 1,800 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.43.

2 Cygni is a blue-white hued star in the northern constellation of Cygnus, located a few degrees from Albireo. It is a probable astrometric binary; the visible component can be viewed with the naked eye, having an apparent visual magnitude of 4.976. Based upon an annual parallax shift of 3.6 mas, it is located roughly 910 light years from Earth. It has a peculiar velocity of 23 km/s and may be a runaway star system.

17 Crateris is a wide binary star system in the equatorial constellation of Hydra, located 90.5 light years away from the Sun. It is visible to the naked eye as a faint, yellow-white hued star with a combined apparent visual magnitude of 4.93. The system is traversing the celestial sphere with a relative proper motion of 24.9 mas/y, and is moving away from the Earth with a heliocentric radial velocity of +5.8 km/s.

4 Lacertae is a single star in the northern constellation Lacerta, located about 1,900 light years away. This object visible to the naked eye as a white-hued star with an apparent visual magnitude of 4.55. It is moving closer to the Earth with a heliocentric radial velocity of −26 km/s. This star is a suspected member of the Lac OB1 association.

Epsilon Normae, Latinised from ε Normae, is a blue-white hued triple star system in the southern constellation of Norma. It has an apparent visual magnitude of 4.47, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 6.15 mas as seen from Earth, the system is located around 530 light years distant from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.21 due to interstellar dust.

<span class="mw-page-title-main">Iota Ophiuchi</span> Star in the constellation Ophiuchus

ι Ophiuchi, Latinized as Iota Ophiuchi, is a single star in the equatorial constellation of Ophiuchus, positioned near the constellation border with Hercules. It makes a naked-eye double with nearby Kappa Ophiuchi, appearing as a faint, blue-white hued star with an apparent visual magnitude of 4.39. The star is approximately 245 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −19 km/s.

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

ET Virginis is a single, red-hued star in the equatorial constellation of Virgo. It can be viewed with the naked eye, having an apparent visual magnitude of 4.91. Based upon an annual parallax shift of 5.9 mas, it is located 560 light years away. It is moving further from the Earth with a heliocentric radial velocity of +18.6 km/s, having come within 177 ly of the Sun around 6.3 million years ago.

<span class="mw-page-title-main">31 Persei</span> Star in the constellation Perseus

31 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a dim, blue-white hued point of light with an apparent visual magnitude of 5.05. This star is located around 172 parsecs (560 ly) away from the Sun, and it is drifting closer with a radial velocity of −1.6 km/s. It is a likely member of the Alpha Persei Cluster.

HR 6875, previously known as Sigma Telescopii, is a single star in the constellation Corona Australis. It has a blue-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.24. This object is located at a distance of approximately 550 light years from the Sun based on parallax. It is listed as a member of the Sco OB2 association.

<span class="mw-page-title-main">HD 28375</span> Star in the constellation Taurus

HD 28375 is a single star in the equatorial constellation of Taurus, near the southern constellation border with Eridanus. It was previously known by the Flamsteed designation 44 Eridani, although the name has fallen out of use because constellations were redrawn, placing the star out of Eridanus and into Taurus. The star is blue-white in hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.53. The distance to this star is approximately 480 light-years based on parallax. It is drifting further away with a radial velocity of 18 km/s, after having come to within an estimated 249 light-years some 3.7 million years ago.

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 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.
  2. 1 2 3 4 5 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 Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1975mcts.book.....H.
  4. 1 2 3 4 Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society , 410 (1): 190–200, arXiv: 1007.4883 , Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID   118629873.
  5. 1 2 3 Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv: astro-ph/0412542 , Bibcode:2005AJ....129.1642F, doi:10.1086/427855, S2CID   119512018.
  6. 1 2 3 4 5 6 Balona, L. A.; et al. (May 2019), "Rotational modulation in TESS B stars", Monthly Notices of the Royal Astronomical Society, 485 (3): 3457–3469, arXiv: 1902.09470 , Bibcode:2019MNRAS.485.3457B, doi:10.1093/mnras/stz586.
  7. ↑ Gáspár, András; et al. (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 171, arXiv: 1604.07403 , Bibcode:2016ApJ...826..171G, doi:10.3847/0004-637X/826/2/171, S2CID   119241004.
  8. 1 2 Gontcharov, G. A. (November 2012), "Spatial distribution and kinematics of OB stars", Astronomy Letters, 38 (11): 694–706, arXiv: 1606.09028 , Bibcode:2012AstL...38..694G, doi:10.1134/S1063773712110035, S2CID   119108982.
  9. ↑ "HD 66591". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-12-04.
  10. ↑ 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.
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.