HD 105382
HD 105382
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
Constellation | Centaurus |
Right ascension | 12h 08m 05.22401s[1] |
Declination | −50° 39′ 40.5728″[1] |
Apparent magnitude (V) | 4.47[2] |
| Characteristics | |
Spectral type | B6III[3] |
| U−B color index | −0.67[2] |
| B−V color index | −0.15[2] |
Variable type | rotating variable[4] |
| Astrometry | |
| Radial velocity (Rv) | 16.5[2] km/s |
| Proper motion (μ) | RA: −35.16[1] mas/yr Dec.: −6.47[1] mas/yr |
| Parallax (π) | 7.44 ± 0.61[1] mas |
| Distance | 440 ± 40 ly (130 ± 10 pc) |
| Absolute magnitude (MV) | 2999880000000000000♠−1.2±0.3[3] |
| Absolute bolometric magnitude (Mbol) | −2.9 ± 0.4[3] |
| Details | |
| Mass | 5.7 ± 0.4[4] M☉ |
| Radius | 3.0 ± 0.6[4] R☉ |
| Luminosity | 1000+590 −370[3] L☉ |
| Surface gravity (log g) | 4.18 ± 0.15[4] cgs |
| Temperature | 17400 ± 400[4] K |
| Rotation | 1.295 ± 0.001[4] days |
| Rotational velocity (v sin i) | 90[3] km/s |
| Other designations | |
CD−49° 6813, HD 105382, HIP 59173, HR 4618, SAO 239687[2] | |
| 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.[5] 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.[4] This peculiar abundance pattern is probably related to HD 105382's magnetic field,[4] which has a polar strength of 2.3 kG.[3]
From astrometric measurements by the Hipparcos spacecraft, HD 105382 is identified as a probable astrometric binary.[6] 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.[7] It is a member of the Lower Centaurus-Crux (LCC) subgroup of the Scorpius–Centaurus Association.[8]
References[edit]
^ abcde 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..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output q{quotes:"""""""'""'"}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-limited a,.mw-parser-output .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}
^ abcde "HD 105382". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 25 October 2017.
^ abcdef 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.
^ abcdefgh 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.
^ 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.
^ 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.
^ 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.
^ 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
Categories:
- Centaurus (constellation)
- B-type giants
- Variable stars
- Objects with variable star designations
- Durchmusterung objects
- Henry Draper Catalogue objects
- Hipparcos objects
- HR objects
- Peculiar stars
- Astrometric binaries
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