Jump to content

HD 105382: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous edit
Content deleted Content added
VisualWikitext
Monkbot (talk | contribs)
Bots
3,695,952 edits
m Task 18b (cosmetic): eval 1 template: hyphenate params (1×);
Added naked eye visibility
 
(17 intermediate revisions by 11 users not shown)
Line 1: Line 1:
{{Short description|Star in the constellation Centaurus}}
{{Starbox begin
{{Starbox begin
| name = HD 105382
| 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
{{starbox observe
Line 39: Line 44:
}}
}}
{{starbox catalog
{{starbox catalog
| names={{odlist|CD=-49° 6813|HD=105382|HIP=59173|HR=4618|SAO=239687}}<ref name=SIMBAD/>
| names={{odlist|CD=−49°6813|HD=105382|HIP=59173|HR=4618|SAO=239687}}<ref name=SIMBAD/>
}}{{Starbox reference
}}{{Starbox reference
| Simbad = HD+105382
| Simbad = HD+105382
}}{{starbox end}}
}}{{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''' (also known as '''V863 Centauri''') is a [[star]] in the [[constellation]] [[Centaurus (constellation)|Centaurus]]. Its [[apparent magnitude]] is 4.47, making it visible to the [[naked eye]] under good observing conditions. 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/>
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/>
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==
==References==
Line 58: Line 63:
| journal=[[Monthly Notices of the Royal Astronomical Society]]
| journal=[[Monthly Notices of the Royal Astronomical Society]]
| volume=389 | issue=2 | pages=869–879 | date=September 2008
| volume=389 | issue=2 | pages=869–879 | date=September 2008
| doi=10.1111/j.1365-2966.2008.13596.x | bibcode=2008MNRAS.389..869E
| doi=10.1111/j.1365-2966.2008.13596.x | doi-access=free | bibcode=2008MNRAS.389..869E
| arxiv=0806.2878 | s2cid=14878976 | postscript=. }}</ref>
| arxiv=0806.2878 | s2cid=14878976 | postscript=. }}</ref>


Line 73: Line 78:
| journal=Monthly Notices of the Royal Astronomical Society
| journal=Monthly Notices of the Royal Astronomical Society
| volume=429 | issue=1 | pages=398–422 | date=February 2013
| volume=429 | issue=1 | pages=398–422 | date=February 2013
| doi=10.1093/mnras/sts344 | bibcode=2013MNRAS.429..398P
| doi=10.1093/mnras/sts344 | doi-access=free | bibcode=2013MNRAS.429..398P
| arxiv=1211.0282 | s2cid=14961579 | postscript=. }}</ref>
| 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
<ref name=Briquet2001>{{cite journal
Line 109: Line 116:
{{Stars of Centaurus}}
{{Stars of Centaurus}}


{{DEFAULTSORT:HD 105382}}
[[Category:Centaurus (constellation)]]
[[Category:Centaurus]]
[[Category:B-type giants]]
[[Category:B-type giants]]
[[Category:Variable stars]]
[[Category:Variable stars]]
Line 116: Line 124:
[[Category:Henry Draper Catalogue objects|105382]]
[[Category:Henry Draper Catalogue objects|105382]]
[[Category:Hipparcos objects|059173]]
[[Category:Hipparcos objects|059173]]
[[Category:HR objects|4618]]
[[Category:Bright Star Catalogue objects|4618]]
[[Category:Helium-weak stars]]
[[Category:Helium-weak stars]]
[[Category:Astrometric binaries]]
[[Category:Astrometric binaries]]
[[Category:Lower Centaurus Crux]]

Latest revision as of 22:48, 27 December 2024

HD 105382

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]
Distance440 ± 40 ly
(130 ± 10 pc)
Absolute magnitude (MV)−1.2±0.3[4]
Absolute bolometric
magnitude (Mbol)		−2.9 ± 0.4[4]
Details
Mass5.7 ± 0.4[5] M☉
Radius3.0 ± 0.6[5] R☉
Luminosity1000+590
−370[4] L☉
Surface gravity (log g)4.18 ± 0.15[5] cgs
Temperature17400 ± 400[5] K
Rotation1.295 ± 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
SIMBADdata

HD 105382 (also known as V863 Centauri) is a star in the constellation Centaurus. Its apparent magnitude is 4.47, making it visible to the naked eye under good observing conditions. 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]

References

[edit]
  1. ^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. ^ a b c d e 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. ^ a b c d e "HD 105382". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 25 October 2017.
  4. ^ a b c d e f 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. ^ a b c d e f g h 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
Retrieved from "https://en.wikipedia.org/w/index.php?title=HD_105382&oldid=1265637765"