Epsilon Coronae Australis

Epsilon Coronae Australis (ε CrA), is a star system located in the constellation Corona Australis. Varying in brightness between apparent magnitudes of 4.74 to 5 over 14 hours, it is the brightest W Ursae Majoris variable (low mass contact binary) in the night sky.

Epsilon Coronae Australis
Observation data
Epoch J2000      Equinox J2000
Constellation Corona Australis
Right ascension 18h 58m 43.37714s[1]
Declination −37° 06′ 26.4865″[1]
Apparent magnitude (V) +4.75[2]
Characteristics
Spectral type F4V Fe-0.8[3]
U−B color index +0.01[2]
B−V color index +0.39[2]
Variable type W UMa[4]
Astrometry
Radial velocity (Rv)57.90 ± 1.2[5] km/s
Proper motion (μ) RA: −132.40[1] mas/yr
Dec.: −110.62[1] mas/yr
Parallax (π)33.13 ± 0.33[1] mas
Distance98.4 ± 1.0 ly
(30.2 ± 0.3 pc)
Absolute magnitude (MV)2.21[6]
Orbit[7]
Period (P)0.59143357 ± 0.00000016 d
Semi-major axis (a)3.795 ± 0.052 R
Eccentricity (e)0
Inclination (i)73.05 ± 0.16°
Longitude of the node (Ω)2.0113 ± 0.0033°
Periastron epoch (T)JD 2442296.95907 ± 0.0070
Details
ε CrA A
Mass1.9[7] M
Radius2.167[7][note 1] R
Temperature6481 ± 20[7] K
Rotational velocity (v sin i)148.5[8] km/s
ε CrA B
Mass0.24[7] M
Radius0.869[7][note 1] R
Temperature5939 ± 19[7] K
Other designations
BD−37° 13001, HD 175813, HIP 93174, HR 7152, SAO 210781[4]
Database references
SIMBADdata

NamingEdit

Nicolas Louis de Lacaille gave Epsilon Coronae Australis its Bayer designation. It is also known as HR 7152, and HD 175813.

PropertiesEdit

Epsilon Coronae Australis is an F4V dwarf star with an effective temperature of 6000 Kelvin. It ranges between apparent magnitudes of 4.74 to 5 over 14 hours,[9] an absolute magnitude of +2.45, and a mass of 1.1 solar masses. Epsilon Coronae Australis is a W Ursae Majoris variable, indicating that it has a contact companion within the Roche Limit of the primary. The star is located at a distance of 30 pc (97 light years) from the Sun.[6] Yildiz and colleagues estimated the age of the system at 2.83 ± 0.28 billion years based on study of the properties of the system and estimated rate of mass transfer. They found the current masses of the primary and secondary to be 1.72 ± 0.04 and 0.22 ± 0.02 solar masses respectively, from their original masses of 1.06 ± 0.03 and 2.18 ± 0.06 solar masses.[10]

NotesEdit

  1. ^ a b Radii were given as a ratio of the radius to the semi-major axis; the semi-major axis is 3.795 R.

ReferencesEdit

  1. ^ a b c d e van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ^ a b c Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  3. ^ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample". The Astronomical Journal. 132: 161. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637.
  4. ^ a b "* eps CrA". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 13 March 2017.
  5. ^ Bilir, S.; Karataş, Y.; Demircan, O.; Eker, Z. (2005). "Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation". Monthly Notices of the Royal Astronomical Society. 357 (2): 497. arXiv:astro-ph/0411291. Bibcode:2005MNRAS.357..497B. doi:10.1111/j.1365-2966.2005.08609.x.
  6. ^ a b Eker, Z.; Bilir, S.; Yaz, E.; Demircan, O.; Helvaci, M. (2009). "New absolute magnitude calibrations for W Ursa Majoris type binaries". Astronomische Nachrichten. 330 (1): 68–77. arXiv:0807.4989. Bibcode:2009AN....330...68E. doi:10.1002/asna.200811041.
  7. ^ a b c d e f g Wilson, R. E.; Raichur, H. (2011). "Distance and temperature from absolute light curves of three eclipsing binaries". Monthly Notices of the Royal Astronomical Society. 415: 596. Bibcode:2011MNRAS.415..596W. doi:10.1111/j.1365-2966.2011.18741.x.
  8. ^ Schröder, C.; Reiners, A.; Schmitt, J. H. M. M. (2009). "Ca II HK emission in rapidly rotating stars" (PDF). Astronomy and Astrophysics. 493 (3): 1099. Bibcode:2009A&A...493.1099S. doi:10.1051/0004-6361:200810377.[permanent dead link]
  9. ^ BSJ (4 January 2010). "Epsilon Coronae Australis". AAVSO Website. American Association of Variable Star Observers. Retrieved 22 January 2014.
  10. ^ Yildiz (2014). "Origin of W UMa-type contact binaries - age and orbital evolution". Monthly Notices of the Royal Astronomical Society. 437 (1): 185–94. arXiv:1310.5526. Bibcode:2014MNRAS.437..185Y. doi:10.1093/mnras/stt1874.