S Crucis

S Crucis is a star in the constellation Crux. A Cepheid variable, its apparent magnitude ranges from 6.22 to 6.92 over 4.68997 d.[2] It is a yellow-white supergiant that pulsates between spectral types F6Ib-II and G1Ib-II.[2]

S Crucis
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Crux
Right ascension  12h 54m 21.99728s[1]
Declination −58° 25′ 50.2146″[1]
Apparent magnitude (V) 6.22 - 6.92[2]
Characteristics
Spectral type F6-G1Ib-II[2]
Variable type δ Cep[2]
Astrometry
Radial velocity (Rv)−6.10[3] (−21.1 - 5.9)[4] km/s
Proper motion (μ) RA: −9.480[1] mas/yr
Dec.: 3.987[1] mas/yr
Parallax (π)1.0215 ± 0.0448[1] mas
Distance3,200 ± 100 ly
(980 ± 40 pc)
Absolute magnitude (MV)-3.27[5]
Details
Radius37.9[6] R☉
Surface gravity (log g)1.2 - 1.9[4] cgs
Temperature5,517 - 6,482[4] K
Metallicity [Fe/H]−0.07 - 0.16[4] dex
Age116[7] Myr
Other designations
CD−57°4766, HD 112044, HIP 62986, HR 4895, SAO 240362[8]
Database references
SIMBADdata
Light curve of the classical Cepheid variable S Crucis recorded by NASA's Transiting Exoplanet Survey Satellite (TESS)

S Crucis is a pulsating variable star of the δ Cephei type, a Classical Cepheid variable. Its mean radius is 37.9 R☉ and that radius varies by up to 4.1 R☉ during its 4.7-day pulsation cycle.[6] Over the same cycle, the effective temperature varies between 5,517 K and 6,482 K.[4] The star is thought to be 116 million years old; it has exhausted its core hydrogen and left the main sequence.[7]

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. Watson, Christopher (4 January 2010). "S Crucis". AAVSO Website. American Association of Variable Star Observers. Retrieved 12 March 2014.
  3. Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
  4. Proxauf, B.; Da Silva, R.; Kovtyukh, V. V.; Bono, G.; Inno, L.; Lemasle, B.; Pritchard, J.; Przybilla, N.; Storm, J.; Urbaneja, M. A.; Valenti, E.; Bergemann, M.; Buonanno, R.; d'Orazi, V.; Fabrizio, M.; Ferraro, I.; Fiorentino, G.; François, P.; Iannicola, G.; Laney, C. D.; Kudritzki, R. -P.; Matsunaga, N.; Nonino, M.; Primas, F.; Romaniello, M.; Thévenin, F. (2018). "A new and homogeneous metallicity scale for Galactic classical Cepheids. I. Physical parameters". Astronomy and Astrophysics. 616: A82. arXiv:1805.00727. Bibcode:2018A&A...616A..82P. doi:10.1051/0004-6361/201833087.
  5. Molinaro, R.; Ripepi, V.; Marconi, M.; Bono, G.; Lub, J.; Pedicelli, S.; Pel, J. W. (2011). "CORS Baade-Wesselink method in the Walraven photometric system: The period-radius and the period-luminosity relation of classical Cepheids". Monthly Notices of the Royal Astronomical Society. 413 (2): 942. Bibcode:2011MNRAS.413..942M. doi:10.1111/j.1365-2966.2010.18183.x.
  6. Moskalik, P.; Gorynya, N. A. (2005). "Mean Angular Diameters and Angular Diameter Amplitudes of Bright Cepheids". Acta Astronomica. 55: 247. arXiv:astro-ph/0507076. Bibcode:2005AcA....55..247M.
  7. Marsakov, V. A.; Koval', V. V.; Kovtyukh, V. V.; Mishenina, T. V. (2013). "Properties of the population of classical Cepheids in the Galaxy". Astronomy Letters. 39 (12): 851. Bibcode:2013AstL...39..851M. doi:10.1134/S1063773713120050.
  8. "V* S Cru". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 12 March 2014.
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