Back Juxta Crucem AST Epsilon Crucis BS Epsilon Crucis German Ginan Spanish اپسیلون صلیب Persian Epsilon Crucis French Epsilon Crucis Italian みなみじゅうじ座イプシロン星 Japanese 기난 Korean Epsilon Crucis Dutch

Epsilon Crucis

ε Crucis
Location of ε Crucis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Crux
Right ascension 12h 21m 21.608s[1]
Declination −60° 24′ 04.13″[1]
Apparent magnitude (V) 3.58[2]
Characteristics
Spectral type K3 III[3]
Apparent magnitude (B) 4.98±0.01[4]
Apparent magnitude (G) 3.1[4]
Apparent magnitude (J) 1.226±0.274[4]
U−B color index +1.63[2]
B−V color index +1.42[2]
Variable type suspected[5]
Astrometry
Radial velocity (Rv)−4.60[6] km/s
Proper motion (μ) RA: −171.223 mas/yr[1]
Dec.: 91.795 mas/yr[1]
Parallax (π)14.2 ± 0.1 mas[1]
Distance230 ± 2 ly
(70.4 ± 0.5 pc)[1]
Absolute magnitude (MV)−0.63±0.09[7]
Details
Mass(1.4 – 1.5)±0.2[8] M☉
Radius31±2[8] R☉
Luminosity282[8] L☉
Surface gravity (log g)1.91[6] cgs
Temperature4,210±125[8] K
Metallicity [Fe/H]−0.03[8] dex
Rotational velocity (v sin i)3.14[6] km/s
Age2.17[6] Gyr
Other designations
Ginan, ε Cru, NSV 5568, CD−59° 4221, FK5 2989, HD 107446, HIP 60260, HR 4700, SAO 251862[4]
Database references
SIMBADdata

Epsilon Crucis, Latinised from ε Crucis (abbreviated Epsilon Cru, ε Cru) and also known as Ginan /ˈɡiːnən/,[9] is a single,[10] orange-hued star in the southern constellation of Crux. Measurements made by the Gaia spacecraft showed an annual parallax shift of 14.2 mas,[1] which provides a distance estimate of about 230 light years. The star can be seen with the naked eye, having an apparent visual magnitude of 3.58.[2] It is moving closer to the Sun with a radial velocity of −4.60 km/s.[6]

This is a giant star of type K with a stellar classification of K3III,[3] indicating that it has exhausted the hydrogen at its core and evolved away from the main sequence. It is about two billion years old[6] with 1.4–1.5 times the mass of the Sun and has expanded to 31 times the Sun's radius. The star is shining with around 282 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,210 K.[8]

  1. ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d Cite error: The named reference eggen was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference perkins was invoked but never defined (see the help page).
  4. ^ a b c d "eps Cru". SIMBAD. Centre de données astronomiques de Strasbourg.
  5. ^ Cite error: The named reference gcvs was invoked but never defined (see the help page).
  6. ^ a b c d e f Cite error: The named reference jofre was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference aaa458_2_609 was invoked but never defined (see the help page).
  8. ^ a b c d e f Cite error: The named reference kallinger was invoked but never defined (see the help page).
  9. ^ "Naming Stars". IAU.org. Retrieved 16 December 2017.
  10. ^ 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, S2CID 14878976.
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