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HD 129116








HD 129116


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This article is about b Centauri. For B Centauri, see B Centauri. For β Centauri, see Beta Centauri.

Not to be confused with Alpha Centauri B.




















































































b Centauri
Observation data
Epoch J2000.0      Equinox J2000.0

Constellation
Centaurus

Right ascension
 14h 41m 57.59s[1]

Declination
 −37° 47′ 37.6″[1]

Apparent magnitude (V)
 +4.01
Characteristics

Spectral type
 B3V
U−B color index
 −0.70
B−V color index
 −0.17

Variable type
 none
Astrometry
Radial velocity (Rv) +1 km/s
Proper motion (μ) RA: -29.92 ± 0.14[1] mas/yr
Dec.: -30.68 ± 0.13[1] mas/yr
Parallax (π) 9.62 ± 0.18[1] mas
Distance 339 ± 6 ly
(104 ± 2 pc)
Absolute magnitude (MV) −0.84
Details
Radius 2.93 ± 0.12[2] R☉
Surface gravity (log g) 4.23 ± 0.03[2] cgs
Temperature 18,445 ± 344[2] K
Other designations
HR 5471, HD 129116, CD−37°9618, HIP 71865, SAO 205839, GC 19779
Database references
SIMBAD data

HD 129116, also known by its Bayer designation b Centauri (b Cen), is a star in the constellation Centaurus.


b Centauri is a blue-white B-type main sequence dwarf with an apparent magnitude of +4.01. It is approximately 339 light years from Earth.



References[edit]





  1. ^ 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}
    Vizier catalog entry


  2. ^ abc Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855














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