HD 113703

Last updated
f Centauri
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Centaurus
Right ascension 13h 06m 16.70s [1]
Declination −48° 27′ 47.8″ [1]
Apparent magnitude  (V)+4.71 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type B4V [3] + K0Ve [4]
U−B color index −0.562 [2]
B−V color index −0.148±0.006 [2]
Astrometry
Radial velocity (Rv)+6.0±4.2 [5]  km/s
Proper motion (μ)RA: −29.558 [1]   mas/yr
Dec.: −15.692 [1]   mas/yr
Parallax (π)8.1592 ± 0.1559  mas [1]
Distance 400 ± 8  ly
(123 ± 2  pc)
Absolute magnitude  (MV)−0.68 [2]
Details
f Cen Aa
Mass 4.39 [6]   M☉
Surface gravity (log g)3.99 [6]   cgs
Temperature 14,769 [6]   K
Rotational velocity (v sin i)140±7 [7]  km/s
Age 92 [6]   Myr
f Cen C
Mass 0.9 [8]   M☉
Luminosity0.49 [8]   L☉
Temperature 5,020 [8]   K
Age 50 [8]   Myr
Other designations
f Cen, CD−47°8088, GC  17750, HD  113703, HIP  63945, HR  4940, SAO  223900, CCDM J13063-4828
Database references
SIMBAD data

HD 113703, also known by the Bayer designation f Centauri , is a multiple star [9] system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, [2] which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association. [6]

The primary of f Centauri is a blue-white hued B-type main-sequence star with a stellar classification of B4V. [3] It is a young star with an age estimated at around 92 million years, [6] and is spinning rapidly with a projected rotational velocity of 140 km/s. [7] A close companion with a K magnitude of 9.16, designated component C, was detected in 2002 at an angular separation of 1.55″ . [10] In 2013, a spectroscopic companion to the primary was observed using long baseline interferometry, with the two being designated components Aa and Ab. [11]

A faint, magnitude 10.8 companion, component B, was first reported by J. F. W. Herschel in 1836. As of 2015, it was located at a separation of 11.6″ along a position angle of 78°. [12] This is a K-type star with a class of K0Ve, showing emission in the Calcium H and K lines. It is a known BY Draconis variable star with the designation V1155 Centauri. [13] It shares a common space motion with the primary, indicating a probable physical relationship, and its Gaia Data Release 3 parallax of 7.965″ ±0.018″ suggests a distance of 409 light years. [14] The star shows a strong overabundance in lithium, which demonstrates its young age. [4] It is about 0.8 magnitudes above zero age main sequence and thus is still contracting as a post-T Tauri star. [15] X-ray emission has been detected from this star. [8]

Related Research Articles

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

Lambda Centauri, Latinized from λ Centauri, is a star in the southern circumpolar constellation of Centaurus. It has an apparent visual magnitude of +3.13, which is bright enough to be seen with the naked eye from the Southern Hemisphere and places it among the brighter members of this constellation. The star is close enough that its distance can be determined directly using the parallax technique, which gives a value of approximately 470 light-years from the Sun. Although a putative solitary star, it has a candidate proper motion companion at an angular separation of 0.73 arcseconds along a position angle of 135°. The nebula IC 2944 lies nearby.

D Centauri is a double star in the southern constellation of Centaurus. The system is faintly visible to the naked eye as a point of light with a combined apparent magnitude of +5.31; the two components are of magnitude 5.78 and 6.98, respectively. It is located at a distance of approximately 610 light years from the Sun based on parallax, and is drifting further away with a radial velocity of ~10 km/s.

Sigma Centauri, Latinized from σ Centauri, is the Bayer designation for a solitary star in the southern constellation of Centaurus. It is visible to the naked eye with an apparent visual magnitude of 3.91. A visual companion at an angular separation of 88.11±0.37 mas along a position angle of 14.33°±2.59° was detected in 2010 using interferometry, but its association with Sigma Centauri remains undetermined as of 2013. The distance to Sigma Centauri, based upon an annual parallax shift of 7.92 mas, is around 412 light years.

<span class="mw-page-title-main">Rho Centauri</span> Binary star system in the constellation Centaurus

Rho Centauri, Latinized from ρ Centauri, is a binary star system in the southern constellation of Centaurus. It is visible to the naked eye as a blue-white hued point of light with a combined apparent visual magnitude of +3.97. The system is located approximately 276 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +15 km/s. It is a proper motion member of the Lower Centaurus–Crux sub-group in the Scorpius–Centaurus OB association, the nearest such association of co-moving massive stars to the Sun.

<span class="mw-page-title-main">HD 129116</span> Binary star in the constellation Centaurus

HD 129116 is a binary star in the northeastern part of Centaurus, east of Menkent. It is also known by its Bayer designation of b Centauri, while HD 129116 is the star's identifier in the Henry Draper catalogue. This object has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.01. It is located at a distance of approximately 325 light years from the Sun based on parallax, and has an absolute magnitude of −1.07.

N Centauri is a binary star in the southern constellation of Centaurus. The brighter star is dimly visible to the naked eye with an apparent visual magnitude of 5.26, and it is approximately 304 light years away based on parallax. It has an absolute magnitude of +0.76 and is drifting further away from the Sun with a radial velocity of +27 km/s. It is a candidate member of the Sco OB2 moving group.

HD 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary star system in the southern constellation of Centaurus. It has a blue-white hue and is faintly visible to the naked eye with a typical apparent visual magnitude of 4.30. The distance to this star is approximately 600 light years based on parallax, and it is drifting further away with a radial velocity of ~29 km/s. It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association. HD 102776 has a relatively large peculiar velocity of 31.1 km/s and is a candidate runaway star that was ejected from its association, most likely by a supernova explosion.

J Centauri is a star in the constellation Centaurus. It is approximately 350 light years from Earth.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

E Centauri is a single star in the southern constellation of Centaurus. It is a white-hued star that is dimly visible to the naked eye with an apparent visual magnitude of +5.34. The distance to this object is approximately 560 light years based on parallax, and it has an absolute magnitude of −0.97. It is drifting closer to the Sun with a radial velocity of +7 km/s, and it is a candidate member of the Lower Centaurus Crux subgroup of the Sco OB2 association.

<span class="mw-page-title-main">HD 125823</span> Star in the constellation Centaurus

HD 125823, also known as V761 Centauri or a Centauri, is a variable star in the constellation Centaurus. It is a blue-white star that is visible to the naked eye with a mean apparent visual magnitude of +4.41. The distance to this star is approximately 460 light years based on parallax measurements. It is a member of the Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association.

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.

K Centauri is a possible binary star in the southern constellation of Centaurus. It has a white hue and is bright enough to be visible to the naked eye, having an apparent visual magnitude of +5.04.

Omicron<sup>1</sup> Centauri Star in the constellation Centaurus

Omicron1 Centauri is a star in the constellation Centaurus. It is approximately 10,000 light years from Earth.

<span class="mw-page-title-main">R Centauri</span> Variable star in the constellation Centaurus

R Centauri is a Mira variable star in the constellation Centaurus.

HD 143699 is a single star in the southern constellation of Lupus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.90. Based upon an annual parallax shift of 9.2 mas, it is located around 350 light years away. It is most likely a member of the Upper Centaurus–Lupus subgroup of the Sco OB2 moving group.

<span class="mw-page-title-main">N Scorpii</span> Star in the constellation of Scorpius

N Scorpii, also known as HD 148703, is a solitary, bluish-white hued star located in the southern constellation Scorpius. It has an apparent magnitude of 4.23, making it readily visible to the naked eye. N Scorpii was initially given the Bayer designation Alpha Normae by Lacaille but it was later moved from Norma to Scorpius. N Scorpii is currently located 550 light years away based on parallax measurements from the Hipparcos satellite and is part of the Upper Scorpius–Centaurus region of the Scorpius–Centaurus association.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

<span class="mw-page-title-main">Y Centauri</span> Variable star in the constellation Centaurus

Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.

HD 98176, also designated as HIP 55133 and rarely 22 G. Centauri, is a solitary, white hued star located in the southern constellation Centaurus. It has an apparent magnitude of 6.44, placing it near the limit for naked eye visibility. Based on parallax measurements from Gaia DR3, the object is estimated to be 348 light years distant. At its current distance, its brightness is diminished by 0.32 magnitudes due to interstellar dust. Pauzen et al. (2001) lists it as a potential λ Boötis star.

References

  1. 1 2 3 4 5 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 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. 2. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  4. 1 2 Catchpole, R. M. (1971). "A lithium rich star in Sco-Cen". Monthly Notices of the Royal Astronomical Society. 154: 15. Bibcode:1971MNRAS.154P..15C. doi: 10.1093/mnras/154.1.15P .
  5. ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  6. 1 2 3 4 5 6 Goldman, Bertrand; et al. (November 2018). "A Large Moving Group within the Lower Centaurus Crux Association". The Astrophysical Journal. 868 (1): 15. arXiv: 1807.02076 . Bibcode:2018ApJ...868...32G. doi: 10.3847/1538-4357/aae64c . S2CID   119343278. 32.
  7. 1 2 Brown, A. G. A.; Verschueren, W. (March 1997). "High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2". Astronomy and Astrophysics. 319: 811–838. arXiv: astro-ph/9608089 . Bibcode:1997A&A...319..811B.
  8. 1 2 3 4 5 Stelzer, B.; et al. (September 2003). "Late B-type stars and their candidate companions resolved with Chandra". Astronomy and Astrophysics. 407 (3): 1067–1078. arXiv: astro-ph/0306401 . Bibcode:2003A&A...407.1067S. doi:10.1051/0004-6361:20030934. S2CID   16766165.
  9. ↑ 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.
  10. ↑ Shatsky, N.; Tokovinin, A. (January 2002). "The mass ratio distribution of B-type visual binaries in the Sco OB2 association". Astronomy and Astrophysics. 382: 92–103. arXiv: astro-ph/0109456 . Bibcode:2002A&A...382...92S. doi:10.1051/0004-6361:20011542. S2CID   16697655.
  11. ↑ Rizzuto, A. C.; et al. (December 2013). "Long-baseline interferometric multiplicity survey of the Sco-Cen OB association". Monthly Notices of the Royal Astronomical Society. 436 (2): 1694–1707. arXiv: 1309.3811 . Bibcode:2013MNRAS.436.1694R. doi:10.1093/mnras/stt1690.
  12. ↑ Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
  13. ↑ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  14. ↑ 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.
  15. ↑ Andrews, P. J.; Thackeray, A. D. (1973). "Absolute magnitudes of B-type primaries in visual binaries". Monthly Notices of the Royal Astronomical Society. 165: 1–9. Bibcode:1973MNRAS.165....1A. doi: 10.1093/mnras/165.1.1 .
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