N Centauri

N Centauri is a binary star[3] in the southern constellation of Centaurus. It is dimly visible to the naked eye with an apparent visual magnitude of 5.26.[2] The distance to this system is approximately 311 light years based on parallax, and it has an absolute magnitude of +0.76.[2] The system is drifting further away from the Sun with a radial velocity of +27 km/s.[2] It is a candidate member of the Sco OB2 moving group.[11]

For n Centauri, see HD 111968.
N Centauri
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension 13h 52m 04.86241s[1]
Declination −52° 48′ 41.4976″[1]
Apparent magnitude (V) 5.26[2] (5.24 + 7.89)[3]
Characteristics
Spectral type B9V + F0Vn[4][5]
B−V color index −0.084±0.003[2]
Astrometry
A
Radial velocity (Rv)+27.0±4.2[2] km/s
Proper motion (μ) RA: −39.039[1] mas/yr
Dec.: −27.426[1] mas/yr
Parallax (π)10.4791 ± 0.1632[1] mas
Distance311 ± 5 ly
(95 ± 1 pc)
Absolute magnitude (MV)+0.76[2]
Details
A
Mass3.32[6] M☉
Luminosity70.18[2] L☉
Surface gravity (log g)4.32±0.14[6] cgs
Temperature13,032±443[6] K
Rotational velocity (v sin i)205[6] km/s
Age66[6] Myr
B
Mass1.48±0.01[7] M☉
Radius1.61+0.08
−0.09[7] R☉
Luminosity6.43[8] L☉
Temperature7,354[8] K
Metallicity [Fe/H]−0.01+0.17
−0.15[7] dex
Age1.07+1.56
−0.42[7] Gyr
Other designations
N Cen, CPD−52°6787, FK5 2985, HR 5207, CCDM J13521-5249, WDS J13521-5249[9]
A: GC 18720, HD 120642, HIP 67703, SAO 241239[9]
B: GC 18718, HD 120641, HIP 67702, SAO 241238[10]
Database references
SIMBADA
B

The double nature of this system was discovered by German astronomer Carl Rümker in 1835. As of 2016, the companion lay at an angular separation of 18.5″ along a position angle of 289° from the primary.[12] They form a co-moving pair with a projected separation of 1,566 AU.[13] The more luminous member is a B-type main-sequence star with a stellar classification of B9V.[3] Its fainter companion is an F-type main-sequence star with a class of F0Vn, where the 'n' suffix indicates that the metal absorption lines in its spectrum are unusual broad ("nebulous") and indicative of rapid rotation.[4][5] Based upon discrepancies in the proper motion measurements, there are hints of a third member of this system.[3]

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  3. 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.
  4. Skiff, B. A. (2014), "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009- )", VizieR On-line Data Catalog, Bibcode:2014yCat....1.2023S.
  5. Gahm, G. F.; Ahlin, P.; Lindroos, K. P. (1983), "A study of visual double stars with early type primaries. I. Spectroscopic results", Astronomy and Astrophysics Supplement Series, 51: 143, Bibcode:1983A&AS...51..143G.
  6. David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146.
  7. Bochanski, John J.; et al. (April 2018), "Fundamental Properties of Co-moving Stars Observed by Gaia", The Astronomical Journal, 155 (4): 17, arXiv:1801.00537, Bibcode:2018AJ....155..149B, doi:10.3847/1538-3881/aaaebe, 149.
  8. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  9. "N Cen". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-03-03.
  10. "HD 120641". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-03-03.
  11. Rizzuto, Aaron; et al. (October 2011), "Multidimensional Bayesian membership analysis of the Sco OB2 moving group", Monthly Notices of the Royal Astronomical Society, 416 (4): 3108–3117, arXiv:1106.2857, Bibcode:2011MNRAS.416.3108R, doi:10.1111/j.1365-2966.2011.19256.x.
  12. Mason, B. D.; et al. (2014), The Washington Visual Double Star Catalog, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, retrieved 2015-07-22
  13. Lindroos, K. P. (1985), "A study of visual double stars with early type primaries. IV Astrophysical data", Astronomy and Astrophysics Supplement Series, 60: 183, Bibcode:1985A&AS...60..183L.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.