HD 105382

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HD 105382
V863CenLightCurve.png
A light curve for V863 Centauri, plotted from Hipparcos data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Centaurus
Right ascension 12h 08m 05.22401s [2]
Declination −50° 39′ 40.5728″ [2]
Apparent magnitude  (V)4.47 [3]
Characteristics
Spectral type B6III [4]
U−B color index −0.67 [3]
B−V color index −0.15 [3]
Variable type rotating variable [5]
Astrometry
Radial velocity (Rv)16.5 [3]  km/s
Proper motion (μ)RA: −35.16 [2]   mas/yr
Dec.: −6.47 [2]   mas/yr
Parallax (π)7.44 ± 0.61  mas [2]
Distance 440 ± 40  ly
(130 ± 10  pc)
Absolute magnitude  (MV)−1.2±0.3 [4]
Absolute bolometric
magnitude  (Mbol)		−2.9 ± 0.4 [4]
Details
Mass 5.7 ± 0.4 [5]   M☉
Radius 3.0 ± 0.6 [5]   R☉
Luminosity 1000+590
−370 [4]   L☉
Surface gravity (log g)4.18 ± 0.15 [5]   cgs
Temperature 17400 ± 400 [5]   K
Rotation 1.295 ± 0.001 [5] days
Rotational velocity (v sin i)90 [4]  km/s
Other designations
CD−49°6813, HD  105382, HIP  59173, HR  4618, SAO  239687 [3]
Database references
SIMBAD data

HD 105382 (also known as V863 Centauri) is a star in the constellation Centaurus. Its apparent magnitude is 4.47. From parallax measurements, it is located 130 parsecs (440 light years) from the Sun.

HD 105382 is a variable star whose apparent magnitude varies with an amplitude of 0.012 over a period of 1.295 days. It has been previously classified as a Be star, which would explain the variability as stellar pulsations, but this classification was probably due to accidental observation of the nearby Be star δ Centauri. [6] A 2004 study showed that the 1.295 day period is actually the rotation period of the star, and that the variability is caused by non-homogeneous distribution of elements in the stellar surface. In particular, HD 105382 is a helium-weak chemically peculiar star with a helium abundance varying between 0.5% and 15% of the solar abundance, and a silicon abundance varying between 0.00044% and 0.0069% the solar value. Regions with more helium appear to coincide with the regions with less silicon, and vice versa. [5] This peculiar abundance pattern is probably related to HD 105382's magnetic field, [5] which has a polar strength of 2.3  kG. [4]

From astrometric measurements by the Hipparcos spacecraft, HD 105382 is identified as a probable astrometric binary. [7] It is only 267" away from δ Centauri, and both stars appear to be at the same distance from Earth and have the same motion through space, so they may be related. In total, this may be a five star system. [8] It is a member of the Lower Centaurus–Crux (LCC) subgroup of the Scorpius–Centaurus association. [9]

Related Research Articles

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

Beta Centauri is a triple star system in the southern constellation of Centaurus. It is officially called Hadar. The Bayer designation of Beta Centauri is Latinised from β Centauri, and abbreviated Beta Cen or β Cen. The system's combined apparent visual magnitude of 0.61 makes it the second-brightest object in Centaurus and the eleventh brightest star in the night sky. According to parallax measurements from the astrometric Hipparcos satellite, the distance to this system is about 390 light-years.

Omicron Aurigae, Latinized from ο Aurigae, is the Bayer designation for an astrometric binary star system in the northern constellation of Auriga. With an apparent visual magnitude of 5.47, it is faintly visible to the naked eye. Based upon an annual parallax shift of 7.89 ± 0.84 mas, it is approximately 413 light-years distant from Earth. The star is a member of the Ursa Major stream of co-moving stars.

<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.

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

Mu Centauri, Latinized from μ Centauri, is a third-magnitude star in the southern constellation of Centaurus. With the stars ν and φ Centauri, it marks what has been traditionally portrayed as "dextro Latere" of the Centaur. The apparent visual magnitude of this star is 3.42, making it one of the brighter members of the constellation. The distance to this star can be estimated directly using parallax measurements, which yield a value of roughly 510 light years (155 parsecs) from Earth.

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

Phi Centauri, Latinized from φ Centauri, is a blue-white hued star in the southern constellation Centaurus. It is visible to the naked eye with an apparent visual magnitude of +3.7. The annual parallax shift is 6.21 mas as measured from Earth, which yields a distance estimate of around 530 light years. It is moving further from the Sun with a radial velocity of +5 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">Psi Centauri</span> Binary star system in the constellation Centaurus

Psi Centauri, which is Latinized from ψ Centauri, is a binary star system in the southern constellation of Centaurus. It is visible to the naked eye with a baseline apparent visual magnitude of +4.05. The distance to this system is approximately 259 light years based on parallax. The radial velocity is poorly constrained, but it appears to be slowly drifting away from the Sun at the rate of +2 km/s.

C3 Centauri is a suspected astrometric binary star system in the southern constellation of Centaurus. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.46. The distance to this object is approximately 342 light years based on parallax. It is a member of the Hyades Stream of co-moving stars.

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.

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.

<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 116243 is a single star in the southern constellation of Centaurus. It has the Bayer designation m Centauri, while HD 116243 is the identifier from the Henry Draper catalogue. This star has a yellow hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.52. It is located at a distance of approximately 244 light years from the Sun based on parallax, and it has an absolute magnitude of 0.01. It is drifting further away with a radial velocity of +13.3 km/s.

HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, 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.

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.

<span class="mw-page-title-main">KT Lupi</span> Visual binary star system in the constellation of Lupus

KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of 2.19″±0.03″. Based upon an annual parallax shift of 7.6 mas as seen from Earth's orbit, it is located 430 light-years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +6.5 km/s. It is a member of the Lower Centaurus–Crux sub-group of the Scorpius–Centaurus association.

<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">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.

Phi Phoenicis, Latinized from φ Phoenicis, is a binary star system in the southern constellation of Phoenix. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1. Based upon an annual parallax shift of 10.185 mas as seen from Earth, it is located approximately 320 light years from the Sun. It is moving away with a heliocentric radial velocity of 10.4 km/s.

<span class="mw-page-title-main">Xi Phoenicis</span> Binary star in the constellation Phoenix

Xi Phoenicis, Latinized from ξ Phoenicis, is a visual binary star system in the southern constellation of Phoenix. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.70. Based upon an annual parallax shift of 14.61 mas as measured from Earth, it is located around 223 light years from the Sun. The system is moving away from the Sun with a radial velocity of about +10 km/s.

References

  1. ↑ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. 1 2 3 4 5 van Leeuwen, F. (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.
  3. 1 2 3 4 5 "HD 105382". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 25 October 2017.
  4. 1 2 3 4 5 6 Petit, V.; et al. (February 2013), "A magnetic confinement versus rotation classification of massive-star magnetospheres", Monthly Notices of the Royal Astronomical Society, 429 (1): 398–422, arXiv: 1211.0282 , Bibcode:2013MNRAS.429..398P, doi:10.1093/mnras/sts344, S2CID   14961579.
  5. 1 2 3 4 5 6 7 8 Briquet, M.; et al. (January 2004). "He and Si surface inhomogeneities of four Bp variable stars". Astronomy and Astrophysics. 413: 273–283. Bibcode:2004A&A...413..273B. doi: 10.1051/0004-6361:20031450 .
  6. ↑ Briquet, M.; Aerts, C.; De Cat, P. (January 2001). "Optical variability of the B-type star HD 105382: Pulsation or rotation?". Astronomy and Astrophysics. 366: 121–128. Bibcode:2001A&A...366..121B. doi: 10.1051/0004-6361:20000193 .
  7. ↑ Makarov, V. V.; Kaplan, G. H. (May 2005), "Statistical Constraints for Astrometric Binaries with Nonlinear Motion", The Astronomical Journal, 129 (5): 2420–2427, Bibcode:2005AJ....129.2420M, doi: 10.1086/429590 .
  8. ↑ 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.
  9. ↑ de Geus, E. J.; de Zeeuw, P. T.; Lub, J. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1–2): 44–61, Bibcode:1989A&A...216...44D
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