Astronomy:Epsilon Capricorni

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Short description: Star in the constellation Capricornus
"Kastra" redirects here. For the DJ and musical artist, see Kastra (musical artist). For the Late Roman fortified camp, see Castra ad Fluvio Frigido.
Epsilon Capricorni
Location of ε Capricorni (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Capricornus[1]
Right ascension  21h 37m 04.83068s[2]
Declination −19° 27′ 57.6464″[2]
Apparent magnitude (V) +4.62[3]
Characteristics
Spectral type B2.5 Vpe[4]
U−B color index −0.64[3]
B−V color index −0.19[3]
Variable type γ Cas[5]
Astrometry
Proper motion (μ) RA: +12.79[2] mas/yr
Dec.: +0.28[2] mas/yr
Parallax (π)3.09 ± 0.18[2] mas
Distance1,060 ± 60 ly
(320 ± 20 pc)
Absolute magnitude (MV)−3.03[1]
Details
ε Cap A
Mass7.6[6] M☉
Radius4.80[6] R☉
Luminosity4,649[1] L☉
Surface gravity (log g)4.0[6] cgs
Temperature18,800[6] K
Metallicity [Fe/H]−0.08[1] dex
Rotational velocity (v sin i)225[7] km/s
Age27.5±4.2[8] Myr
Other designations
Kastra[9], ε Cap, 39 Cap, BD−20°6251, FK5 3724, HD 205637, HIP 106723, HR 8260, SAO 164520, WDS J21371-1928A[10]
Database references
SIMBADdata

Epsilon Capricorni is a binary star system[11] in the constellation Capricornus. It has the traditional star name Kastra, meaning "fort" or "military camp" in Latin; Epsilon Capricorni is the Bayer designation, which is Latinized from ε Capricorni and abbreviated Epsilon Cap or ε Cap. Based upon an annual parallax shift of 3.09 mas as seen from the Earth,[2] the star is located about 1,060 light years from the Sun. It can be seen with the naked eye, having a combined apparent visual magnitude of 4.62.[3]

In Chinese, 壘壁陣 (Lěi Bì Zhèn), meaning Line of Ramparts, refers to an asterism consisting of ε Capricorni, κ Capricorni, γ Capricorni, δ Capricorni, ι Aquarii, σ Aquarii, λ Aquarii, φ Aquarii, 27 Piscium, 29 Piscium, 33 Piscium and 30 Piscium.[12] Consequently, the Chinese name for ε Capricorni itself is 壘壁陣二 (Lěi Bì Zhèn èr, English: the Second Star of Line of Ramparts.)[13]

Observations

A light curve for Epsilon Capricorni, adapted from Lefèvre et al. (2009)[14]

In 2006, this was reported as a single-lined spectroscopic binary with an orbital period of 128.5 days. It was confirmed in 2023.[11] The primary, component Aa, is a Be star that is surrounded by ionized gas that is producing the emission lines in the spectrum. This circumstellar shell is inclined by 80° to the line of sight from the Earth.[6] The system is undergoing both short term and long term variations in luminosity, with the short period variations showing a phase cycle of 1.03 days.[5] It is classified as a Gamma Cassiopeiae variable with an amplitude of 0.16 in magnitude.[5]

Epsilon Capricorni Aa is a blue-white hued B-type main sequence star with a stellar classification of B2.5 Vpe[4] and a visual magnitude of +4.62.[3] It has 7.6 times the mass of the Sun and 4.8 times the Sun's radius.[6] The star is spinning rapidly, with a projected rotational velocity of 225 km/s. This is giving it an oblate shape with an equatorial bulge that is 7% larger than the polar radius.[7]

The system has two visual companions. Component B is a visual magnitude 10.11 star at an angular separation of 65.8 arc seconds along a position angle of 46°, as of 2013. Component C with visual magnitude of 14.1 lies at an angular separation of 62.7 arc seconds along a position angle of 164°, as of 1999.[15] Both stars are likely to be unrelated and at different distances to Epsilon Capricorni.[16]

References

  1. ↑ 1.0 1.1 1.2 1.3 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 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Feinstein, A.; Marraco, H. G. (November 1979), "The photometric behavior of Be Stars", Astronomical Journal 84: 1713–1725, doi:10.1086/112600, Bibcode: 1979AJ.....84.1713F. 
  4. ↑ 4.0 4.1 Adelman, S. J. et al. (December 2000), "On the Variability of O4-B5 Luminosity Class III-V Stars", Information Bulletin on Variable Stars 5008 (5008): 1, Bibcode: 2000IBVS.5008....1A. 
  5. ↑ 5.0 5.1 5.2 Balona, L. A. (December 2002), "Short period spectral variability in the Be stars I: eta Centauri and epsilon Capricorni", The Journal of Astronomical Data 8: 1, Bibcode: 2002JAD.....8....1B. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Silaj, J. et al. (November 2014), "The Hα Profiles of Be Shell Stars", The Astrophysical Journal 795 (1): 12, doi:10.1088/0004-637X/795/1/82, 82, Bibcode: 2014ApJ...795...82S. 
  7. ↑ 7.0 7.1 Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review 20 (1), doi:10.1007/s00159-012-0051-2, Bibcode: 2012A&ARv..20...51V. 
  8. ↑ 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. 
  9. ↑ Kostjuk, N. D. (2004), "VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)", VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002) 4027, Bibcode: 2004yCat.4027....0K. 
  10. ↑ "del Cap". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=del+Cap. 
  11. ↑ 11.0 11.1 Klement, Robert et al. (February 2024), "The CHARA Array Interferometric Program on the Multiplicity of Classical Be Stars: New Detections and Orbits of Stripped Subdwarf Companions" (in en), The Astrophysical Journal 962 (1): 70, doi:10.3847/1538-4357/ad13ec, ISSN 0004-637X, Bibcode: 2024ApJ...962...70K. 
  12. ↑ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  13. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 7 日
  14. ↑ Lefèvre, L. et al. (November 2009), "A systematic study of variability among OB-stars based on HIPPARCOS photometry", Astronomy and Astrophysics 507 (2): 1141–1201, doi:10.1051/0004-6361/200912304, Bibcode: 2009A&A...507.1141L, https://www.aanda.org/articles/aa/pdf/2009/44/aa12304-09.pdf, retrieved 29 July 2022. 
  15. ↑ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M, http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/wds, retrieved 2015-07-22 
  16. ↑ 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.

de:Castra



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