Просмотр кода страницы Английская Википедия:HD 105382

{{Английская Википедия/Панель перехода}}
{{Short description|Star in the constellation Centaurus}}
{{Starbox begin
 | name = HD 105382
}}
{{Starbox image
| image = [[Image:V863CenLightCurve.png|250px]]
| caption = A [[light curve]] for V863 Centauri, plotted from ''[[Hipparcos]]'' data<ref name=HipDataAccess/>
}}
{{starbox observe
| epoch=J2000
| constell=[[Centaurus]]
| ra=   {{RA|12|08|05.22401}}<ref name=vanLeeuwen2007/>
| dec=  {{DEC|-50|39|40.5728}}<ref name=vanLeeuwen2007/>
| appmag_v=4.47<ref name=SIMBAD>{{cite simbad|title=HD 105382|access-date=25 October 2017}}</ref>
|names=
}}
{{starbox character
| class= B6III<ref name=Petit2013/>
| b-v = −0.15<ref name=SIMBAD/>
| u-b = −0.67<ref name=SIMBAD/>
| variable = rotating variable<ref name=Briquet2004/>
}}
{{starbox astrometry
| radial_v=16.5<ref name=SIMBAD/>
| prop_mo_ra=−35.16<ref name=vanLeeuwen2007/>
| prop_mo_dec=−6.47<ref name=vanLeeuwen2007/>
| parallax=7.44
| p_error=0.61
| parallax_footnote = <ref name=vanLeeuwen2007/>
| absmag_v = {{Val|−1.2|0.3}}<ref name=Petit2013/>
 | absmag_bol = −2.9 ± 0.4<ref name=Petit2013/>
}}
{{Starbox detail
 | source = 
 | mass = 5.7 ± 0.4<ref name=Briquet2004/>
 | radius = 3.0 ± 0.6<ref name=Briquet2004/>
 | luminosity = 1000{{±|590|370}}<ref name=Petit2013/>
 | temperature = 17400 ± 400<ref name=Briquet2004/>
 | gravity = 4.18 ± 0.15<ref name=Briquet2004/>
 | metal_fe = 
 | rotational_velocity = 90<ref name=Petit2013/>
 | rotation =   1.295 ± 0.001<ref name=Briquet2004/> days
 | age_myr = 
}}
{{starbox catalog
| names={{odlist|CD=−49°6813|HD=105382|HIP=59173|HR=4618|SAO=239687}}<ref name=SIMBAD/>
}}{{Starbox reference
 | Simbad = HD+105382
}}{{starbox end}}

'''HD 105382''' (also known as '''V863 Centauri''') is a [[star]] in the [[constellation]] [[Centaurus (constellation)|Centaurus]]. Its [[apparent magnitude]] is 4.47. From [[parallax]] measurements, it is located 130 [[parsecs]] (440 [[light year]]s) 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]].<ref name=Briquet2001/> A 2004 study showed that the 1.295 day period is actually the [[stellar rotation|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.<ref name=Briquet2004/> This peculiar abundance pattern is probably related to HD 105382's [[stellar magnetic field|magnetic field]],<ref name=Briquet2004/> which has a polar strength of 2.3&nbsp;[[gauss (unit)|kG]].<ref name=Petit2013/>

From [[Astrometry|astrometric]] measurements by the [[Hipparcos]] spacecraft, HD 105382 is identified as a probable [[astrometric binary]].<ref name=Makarov2005/> 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.<ref name=Eggleton2008/> It is a member of the Lower Centaurus–Crux (LCC) subgroup of the [[Scorpius–Centaurus association]].<ref name=deGeus1989/>

==References==
{{reflist|refs=

<ref name=Eggleton2008>{{citation
 | last1=Eggleton | first1=P. P. | last2=Tokovinin | first2=A. A.
 | title=A catalogue of multiplicity among bright stellar systems
 | journal=[[Monthly Notices of the Royal Astronomical Society]]
 | volume=389 | issue=2 | pages=869–879 | date=September 2008
 | doi=10.1111/j.1365-2966.2008.13596.x | bibcode=2008MNRAS.389..869E
 | arxiv=0806.2878 | s2cid=14878976 | postscript=. }}</ref>

<ref name=Petit2013>{{citation
 | title=A magnetic confinement versus rotation classification of massive-star magnetospheres
 | display-authors=1 | last1=Petit | first1=V.
 | last2=Owocki | first2=S. P. | last3=Wade | first3=G. A.
 | last4=Cohen | first4=D. H. | last5=Sundqvist | first5=J. O.
 | last6=Gagné | first6=M. | last7=Maíz Apellániz | first7=J.
 | last8=Oksala | first8=M. E. | last9=Bohlender | first9=D. A.
 | last10=Rivinius | first10=T. | last11=Henrichs | first11=H. F.
 | last12=Alecian | first12=E. | last13=Townsend | first13=R. H. D.
 | last14=ud-Doula | first14=A. | last15=MiMeS Collaboration
 | journal=Monthly Notices of the Royal Astronomical Society
 | volume=429 | issue=1 | pages=398–422 | date=February 2013
 | doi=10.1093/mnras/sts344 | bibcode=2013MNRAS.429..398P
 | arxiv=1211.0282 | s2cid=14961579 | postscript=. }}</ref>

<ref name=HipDataAccess>{{cite web |title=Hipparcos Tools Interactive Data Access |url=https://www.cosmos.esa.int/web/hipparcos/interactive-data-access |website=Hipparcos |publisher=ESA |access-date=8 December 2021}}</ref>

<ref name=Briquet2001>{{cite journal
 |author1=Briquet, M.|author2=Aerts, C.|author3=De Cat, P.
 |title=Optical variability of the B-type star HD 105382: Pulsation or rotation?
 |journal=Astronomy and Astrophysics|volume=366|pages=121–128
 |date=January 2001|bibcode=2001A&A...366..121B|doi=10.1051/0004-6361:20000193|doi-access=free}}</ref>

<ref name=Briquet2004>{{cite journal
 |author=Briquet, M.|display-authors=etal
 |title=He and Si surface inhomogeneities of four Bp variable stars
 |journal=Astronomy and Astrophysics|volume=413|pages=273–283
 |date=January 2004|bibcode=2004A&A...413..273B|doi=10.1051/0004-6361:20031450|doi-access=free}}</ref>

<ref name=vanLeeuwen2007>{{citation
 | title=Validation of the new Hipparcos reduction
 | last1=van Leeuwen | first1=F.
 | journal=Astronomy and Astrophysics
 | volume=474 | issue=2 | pages=653–664 | date=2007
 | arxiv=0708.1752 | bibcode=2007A&A...474..653V
 | doi=10.1051/0004-6361:20078357 | s2cid=18759600 | postscript=. }}</ref>

<ref name=Makarov2005>{{citation
 | last1=Makarov | first1=V. V. | last2=Kaplan | first2=G. H.
 | title=Statistical Constraints for Astrometric Binaries with Nonlinear Motion
 | journal=The Astronomical Journal | postscript=.
 | volume=129 | issue=5 | pages=2420–2427 | date=May 2005
 | doi=10.1086/429590 | bibcode=2005AJ....129.2420M | doi-access=free }}</ref>

<ref name=deGeus1989>{{citation | last1=de Geus | first1=E. J. | last2=de Zeeuw | first2=P. T. | last3=Lub | first3=J. | title=Physical parameters of stars in the Scorpio-Centaurus OB association | journal=Astronomy and Astrophysics | volume=216 | issue=1–2 | pages=44–61 |date=June 1989 | bibcode=1989A&A...216...44D }}</ref>

}}

{{Stars of Centaurus}}

{{DEFAULTSORT:HD 105382}}
[[Category:Centaurus]]
[[Category:B-type giants]]
[[Category:Variable stars]]
[[Category:Objects with variable star designations|Centauri, V863]]
[[Category:Durchmusterung objects]]
[[Category:Henry Draper Catalogue objects|105382]]
[[Category:Hipparcos objects|059173]]
[[Category:Bright Star Catalogue objects|4618]]
[[Category:Helium-weak stars]]
[[Category:Astrometric binaries]]
[[Category:Lower Centaurus Crux]]
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