Theta Hydrae

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Theta Hydrae
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Hydra
Right ascension 08h 43m 13.47499s[1]
Declination +03° 23′ 55.1867″[1]
Apparent magnitude (V) 3.888[2]
Spectral type B9.5 V + DA 1.6[3]
U−B color index −0.118[2]
B−V color index −0.065[2]
Radial velocity (Rv) −10.7±0.3[4] km/s
Proper motion (μ) RA: +114.64[1] mas/yr
Dec.: −313.94[1] mas/yr
Parallax (π) 28.74 ± 1.55[1] mas
Distance 113 ± 6 ly
(35 ± 2 pc)
θ Hya A
Mass 2.52[3] M
Surface gravity (log g) 3.80±0.08[5] cgs
Temperature 10,099±145[5] K
Metallicity [Fe/H] −0.42±0.09[5] dex
Rotational velocity (v sin i) 95[6] km/s
θ Hya B
Mass 0.68[7] or 1.21[3] M
Temperature 30,700[3] K
Other designations
θ Hya, 22 Hydrae, BD+02° 2167, FK5 347, HD 79469, HIP 45336, HR 3665, SAO 117527.[8]
Database references

Theta Hydrae (θ Hya) is a binary star[7] system in the constellation Hydra. It is visible to the naked eye with an apparent visual magnitude of 3.9.[2] The star system has a high proper motion[7] with an annual parallax shift of 28.74 mas,[1] indicating a distance of about 113 light years. Theta Hydrae forms a double with a magnitude 9.9 star located at an angular separation of 29 arcseconds.[9]

The primary component of this system is a B-type main sequence star with a stellar classification of B9.5 V.[3] It is a candidate Lambda Boötis star, indicating it displays an underabundance of iron peak elements.[10] However, it is also underabundant in oxygen, a characteristic not shared by other Lambda Boötis stars. Instead, it may be a peculiar B star.[11]

An orbiting white dwarf companion was discovered in 1998 from its X-ray emission. This degenerate star must have evolved from a progenitor that was once more massive than the current primary.[7] Burleigh and Barstow (1999) gave a mass estimate of 0.68[7] times the mass of the Sun, whereas Holberg et al. (2013) put it as high as 1.21[3] times the Sun's mass. The latter would put it beyond the theoretical upper limit for white dwarf remnants of typical single stars that did not undergo a merger or mass loss.[12]


  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752Freely accessible, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Cousins, A. W. J. (1984), "Standardization of Broadband Photometry of Equatorial Standards", South African Astronomical Observatory Circulars, 8: 59, Bibcode:1984SAAOC...8...59C. 
  3. ^ a b c d e f Holberg, J. B.; et al. (November 2013), "Where are all the Sirius-like binary systems?", Monthly Notices of the Royal Astronomical Society, 435 (3): 2077–2091, Bibcode:2013MNRAS.435.2077H, arXiv:1307.8047Freely accessible, doi:10.1093/mnras/stt1433. 
  4. ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065. 
  5. ^ a b c Wu, Yue; et al. (January 2011), "Coudé-feed stellar spectral library – atmospheric parameters", Astronomy and Astrophysics, 525: A71, Bibcode:2011A&A...525A..71W, arXiv:1009.1491Freely accessible, doi:10.1051/0004-6361/201015014. 
  6. ^ Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, Bibcode:2012A&A...537A.120Z, arXiv:1201.2052Freely accessible, doi:10.1051/0004-6361/201117691. 
  7. ^ a b c d e Burleigh, M. R.; Barstow, M. A. (January 1999), "Theta Hya: spectroscopic identification of a second B star+white dwarf binary", Astronomy and Astrophysics, 341: 795–798, Bibcode:1999A&A...341..795B, arXiv:astro-ph/9810113Freely accessible. 
  8. ^ "tet Hya – Spectroscopic binary", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-01-04. 
  9. ^ Privett, Grant; Jones, Kevin (2013), The Constellation Observing Atlas, The Patrick Moore Practical Astronomy Series, Springer Science & Business Media, p. 104, ISBN 1461476488. 
  10. ^ King, J. R. (July 1994), "Accretion from Circumstellar Discs and the Lambda-Bootis Phenomenon", Monthly Notices of the Royal Astronomical Society, 269 (1): 209–217, Bibcode:1994MNRAS.269..209K, doi:10.1093/mnras/269.1.209. 
  11. ^ Baschek, Bodo; Searle, Leonard (February 1969), "The Chemical Composition of the Lambda Bootis Stars", Astrophysical Journal, 155: 537, Bibcode:1969ApJ...155..537B, doi:10.1086/149890. 
  12. ^ Vennes, S.; Kawka, A. (September 2008), "On the empirical evidence for the existence of ultramassive white dwarfs", Monthly Notices of the Royal Astronomical Society, 389 (3): 1367–1374, Bibcode:2008MNRAS.389.1367V, arXiv:0806.4742Freely accessible, doi:10.1111/j.1365-2966.2008.13652.x. 

External links[edit]

  • Kaler, James B. (May 8, 2015), "Theta Hydrae", Stars, University of Illinois, retrieved 2016-01-04.