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4 Centauri








4 Centauri


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This article is about h Centauri. It is not to be confused with H Centauri.





































































































































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

Constellation
Centaurus

Right ascension
 13h 53m 12.53953s[1]

Declination
 −31° 55′ 39.3947″[1]

Apparent magnitude (V)
 +4.73[2](+4.72[3] / +8.47[4])
Characteristics

Spectral type
 B6IV[5] / Am[5]
U−B color index
 −0.56[2]
B−V color index
 −0.14[2]
Astrometry
Radial velocity (Rv) +5.2 ± 2[6] km/s
Proper motion (μ) RA: -12.72[1] mas/yr
Dec.: -9.48[1] mas/yr
Parallax (π) 5.12 ± 0.70[1] mas
Distance approx. 640 ly
(approx. 200 pc)
Absolute magnitude (MV) −1.80[citation needed]

Orbit[5]
Primary 4 Cen Aa
Companion 4 Cen Ab
Period (P) 6.930137 ± 0.000015
Eccentricity (e) 0.25 ± 0.10
Periastron epoch (T) 2418823.406 ± 0.10

Argument of periastron (ω)
(secondary)
 152 ± 17°

Semi-amplitude (K1)
(primary)
 21.0 ± 1.5 km/s

Orbit[5]
Primary 4 Cen Ba
Companion 4 Cen Bb
Period (P) 4.8390 ± 0.0001
Eccentricity (e) 0.05 ± 0.02
Periastron epoch (T) 2442916.55 ± 0.09

Argument of periastron (ω)
(secondary)
 51 ± 20°

Semi-amplitude (K1)
(primary)
 16.9 ± 3.5 km/s
Other designations
h Cen, HD 120955, HR 5221, HIP 67786, CCDM J13532-3156

4 Cen A[7]: SAO 204944, GC 18755, CD–31° 10729[8]

4 Cen B: SAO 204943, GC 18754, CD–31° 10727[9]
Database references
SIMBAD 4 Cen
4 Cen A
4 Cen B

4 Centauri is a star in the constellation Centaurus. It is a blue-white B-type subgiant with an apparent magnitude of +4.75 and is approximately 640 light years from Earth.


4 Centauri is a hierarchical quadruple star system. The primary component of the system, 4 Centauri A, is a spectroscopic binary, meaning that its components cannot be resolved but periodic Doppler shifts in its spectrum show that it must be orbiting. 4 Centauri A has an orbital period of 6.927 days and an eccentricity of 0.23. Because light from only one of the stars can be detected (i.e. it is a single-lined spectroscopic binary), some parameters such as its inclination are unknown.[10] The secondary component, is also a single-lined spectroscopic binary. It has an orbital period of 4.839 days and an eccentricity of 0.05. The secondary component is a metallic-lined A-type star. The two pairs themselves are separated by 14 arcseconds; one orbit would take at least 55,000 years.[5]



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 Mendoza, E. E. (1974). "Multicolor photometry of metallic-line stars. III. A photometric catalogue". Revista Mexicana de Astronomia y Astrofisica. 1: 175. Bibcode:1974RMxAA...1..175M. Color indices accessed using SIMBAD.


  3. ^ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.


  4. ^ Nicolet, B. (1978). "Catalogue of homogeneous data in the UBV photoelectric photometric system". Astronomy and Astrophysics. 34: 1. Bibcode:1978A&AS...34....1N.


  5. ^ abcde Levato, H.; Malaroda, S.; Morrell, N.; Solivella, G. (1987). "Stellar multiplicity in the Scorpius-Centaurus association". Astrophysical Journal Supplement Series. 64: 487–503. Bibcode:1987ApJS...64..487L. doi:10.1086/191204.


  6. ^ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.


  7. ^ "* 4 Cen". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 February 2018.


  8. ^ "* 4 Cen A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 February 2018.


  9. ^ "* 4 Cen B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 February 2018.


  10. ^ Paddock, G. F. (1917). "The Spectroscopic Binary H 4 Centauri". Publications of the Astronomical Society of the Pacific. 29 (167): 56. Bibcode:1917PASP...29...56P. doi:10.1086/122588.












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