Astronomy:Zeta Crucis

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Short description: Star in the constellation Crux
Zeta Crucis
Location of ζ Crucis (circled in red)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Crux[1]
Right ascension  12h 18m 26.24075s[2]
Declination −64° 00′ 11.1073″[2]
Apparent magnitude (V) 4.04[3]
Characteristics
Evolutionary stage main sequence[2]
Spectral type B2.5V[4]
U−B color index −0.68[3]
B−V color index −0.17[3]
Astrometry
Radial velocity (Rv)+15.8[5] km/s
Proper motion (μ) RA: −37.431[2] mas/yr
Dec.: −6.576[2] mas/yr
Parallax (π)9.2402 ± 0.1928[2] mas
Distance353 ± 7 ly
(108 ± 2 pc)
Absolute magnitude (MV)−1.13[1]
Details
Mass6.4±0.1[6] M☉
Radius3.7[2] R☉
Luminosity737[1] L☉
Surface gravity (log g)3.99[2] cgs
Temperature18,155[7] K
Rotational velocity (v sin i)115[8] km/s
Age19.8[9] Myr
Other designations
ζ Cru, CPD−63°2235, HD 106983, HIP 60009, HR 4679, SAO 251841[10]
Database references
SIMBADdata

Zeta Crucis is a binary star system in the southern constellation of Crux. Its name is a Bayer designation that is Latinized from ζ Crucis and abbreviated ζ Cru or ζ Cru. This system is visible to the naked eye as a point of light with an apparent visual magnitude of 4.06m. Based on parallax measurements, ζ Crucis is located at a distance of about 353 light-years (108 pc) from the Sun. It is a member of the Lower Centaurus–Crux subgroup of the Scorpius–Centaurus association.[11]

This is a double-lined spectroscopic binary star system.[12] The spectrum matches a B-type main-sequence star with a stellar classification of B2.5 V. It displays pulsational behavior matching a slowly pulsating B-type star and Beta Cephei variable.[13] There is a faint visual companion with an apparent magnitude of 12.49.[14]

A K-type companion star has an angular separation of 0.15″. This corresponds to a projected separation of about 20 au that would yield an orbital period of around 20 years. A common proper motion companion of type M2 is at a separation of around 11′. This would correspond to a projected separation of 60,000 au. It is about 1.5 magnitudes brighter than expected for its temperature, so it is most likely a pre-main-sequence star.[15]

References

  1. ↑ 1.0 1.1 1.2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Johnson, H. L. et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99): 99. Bibcode: 1966CoLPL...4...99J. 
  4. ↑ Hiltner, W. A. et al. (July 1969). "MK Spectral Types for Bright Southern OB Stars". Astrophysical Journal 157: 313–326. doi:10.1086/150069. Bibcode: 1969ApJ...157..313H. 
  5. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". in Batten, Alan Henry; Heard, John Frederick. University of Toronto: International Astronomical Union. Bibcode: 1967IAUS...30...57E. 
  6. ↑ Tetzlaff, N. et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society 410 (1): 190–200, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T. 
  7. ↑ Gerbaldi, M. et al. (November 2001). "Binary systems with post-T Tauri secondaries". Astronomy and Astrophysics 379: 162–184. doi:10.1051/0004-6361:20011298. Bibcode: 2001A&A...379..162G. 
  8. ↑ Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago 239 (1): 1. Bibcode: 1970CoAsi.239....1B. 
  9. ↑ Gratton, R. et al. (2023). "Multiples among B stars in the Scorpius-Centaurus association". Astronomy and Astrophysics 678: A93. doi:10.1051/0004-6361/202346806. Bibcode: 2023A&A...678A..93G. 
  10. ↑ "zet Cru". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=zet+Cru. 
  11. ↑ Chen, Christine H. et al. (September 2012), "A Spitzer MIPS Study of 2.5–2.0 M☉ Stars in Scorpius–Centaurus", The Astrophysical Journal 756 (2): 24, doi:10.1088/0004-637X/756/2/133, 133, Bibcode: 2012ApJ...756..133C. 
  12. ↑ Chini, R. et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society 424 (3): 1925, doi:10.1111/j.1365-2966.2012.21317.x, Bibcode: 2012MNRAS.424.1925C. 
  13. ↑ Balona, L. A.; Ozuyar, D. (2020). "Pulsation among TESS A and B stars and the Maia variables". Monthly Notices of the Royal Astronomical Society 493 (4): 5871. doi:10.1093/mnras/staa670. Bibcode: 2020MNRAS.493.5871B. 
  14. ↑ Gahm, G. F. et al. (January 1983). "A study of visual double stars with early type primaries. I - Spectroscopic results". Astronomy and Astrophysics Supplement Series 51: 143–159. Bibcode: 1983A&AS...51..143G. 
  15. ↑ Gratton, R. (October 2023). "Multiples among B stars in the Scorpius-Centaurus association". Astronomy & Astrophysics 678: id. A93. doi:10.1051/0004-6361/202346806. Bibcode: 2023A&A...678A..93G. 



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