DV Aquarii

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
DV Aquarii
Observation data
Epoch J2000      Equinox J2000
Constellation Aquarius
Right ascension 20h 58m 41.84009s[1]
Declination −14° 28′ 59.2527″[1]
Apparent magnitude (V) 5.89[2]
Characteristics
Spectral type A9 V[3]
B−V color index 0.244±0.009[4]
Variable type β Lyr[5]
Astrometry
Radial velocity (Rv)+10.3±7.4[6] km/s
Proper motion (μ) RA: −54.986[1] mas/yr
Dec.: −18.428[1] mas/yr
Parallax (π)11.2032 ± 0.1015[1] mas
Distance291 ± 3 ly
(89.3 ± 0.8 pc)
Absolute magnitude (MV)1.25[4]
Orbit[7]
Period (P)1.5755 d
Eccentricity (e)0 (adopted)
Inclination (i)83.18±0.11[8]°
Periastron epoch (T)2426160.50 JD
Semi-amplitude (K1)
(primary)
95.5 km/s
Details
DV Aqr Aa
Mass1.70[9] M
Radius2.756[8] R
Luminosity28.8+2.6
−2.4
[10] L
Surface gravity (log g)3.97[10] cgs
Temperature7,843±267[11] K
Rotational velocity (v sin i)103[10] km/s
Age679[11] Myr
DV Aqr Ab
Mass1.01[9] M
Radius1.149[8] R
Surface gravity (log g)4.334[8] cgs
Temperature6,056±240[8] K
Other designations
BD−15° 5848, HD 199603, HIP 103545, HR 8024, SAO 164027[12]
Database references
SIMBADdata

DV Aquarii is a binary star[9] system in the zodiac constellation of Aquarius. It has a peak apparent visual magnitude of 5.89,[2] which is bright enough to be visible to the naked eye. The distance can be estimated from its annual parallax shift of 11.2 mas,[1] yielding a separation of 291 light years.

This is a detached eclipsing binary system of the Beta Lyrae type. The orbital period for the system is 1.5755 days and the eccentricity is unknown and probably non-zero;[7] the orbital inclination is estimated to be 83.18°±0.11°.[8] During the primary eclipse the magnitude drops to 6.25. It descends to 6.10 with the secondary eclipse (with 6.10 being brighter than 6.25).[2] The pair have been identified as candidate Herbig Ae/Be stars,[13] and catalogued as A-type shell stars.[14]

A magnitude 10.8 star with the designation HD 358087[15] is a common proper motion companion. It is located at an angular separation of 129 and has 78% of the Sun's mass. If it is gravitationally bound to the main system, the orbital period is estimated to be around 611,855 years[9]

References[edit]

  1. ^ a b c d e f 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.
  2. ^ a b c Avvakumova, E. A.; et al. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten. 334 (8): 860. Bibcode:2013AN....334..860A. doi:10.1002/asna.201311942.
  3. ^ Houk, Nancy; Smith-Moore, M. (1978). "Michigan catalogue of two-dimensional spectral types for the HD stars". 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1988mcts.book.....H.
  4. ^ a b Adelman, Saul J. (2002). "On the Periods of the Magnetic CP Stars". Baltic Astronomy. 11: 475–485. Bibcode:2002BaltA..11..475A.
  5. ^ Watson, Christopher (April 19, 2012). "DV Aquarii". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 2015-06-04.
  6. ^ Kharchenko, N. V.; et al. (2004). "Astrophysical supplements to the ASCC-2.5. II. Membership probabilities in 520 Galactic open cluster sky areas". Astronomische Nachrichten. 325 (9): 740–748. Bibcode:2004AN....325..740K. doi:10.1002/asna.200410256.
  7. ^ a b Paffhausen, W.; Seggewiss, W. (April 1976). "Spectroscopic orbits of the eclipsing binaries DV and DX Aqr". Astronomy and Astrophysics Supplement Series. 24: 29–34. Bibcode:1976A&AS...24...29P.
  8. ^ a b c d e f Polubek, G. (December 2001). "DV Aquarii Revisited". Odessa Astronomical Publications. 14: 65–68. Bibcode:2001OAP....14...65P.
  9. ^ a b c d Tokovinin, A.; et al. (2008). "Tertiary companions to close spectroscopic binaries". Berlin Heidelberg: 129. arXiv:astro-ph/0601518. Bibcode:2006yCat..34500681T. doi:10.1051/0004-6361:20054427. ISBN 978-3-540-74744-4.
  10. ^ a b c Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691.
  11. ^ a b David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146.
  12. ^ "HD 199603". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2018.
  13. ^ Corporon, P.; Lagrange, A.-M. (May 1999). "A search for spectroscopic binaries among Herbig Ae/Be stars". Astronomy and Astrophysics Supplement. 136: 429–444. Bibcode:1999A&AS..136..429C. doi:10.1051/aas:1999225.
  14. ^ Hauck, B.; Jaschek, C. (February 2000). "A-shell stars in the Geneva system". Astronomy and Astrophysics. 354: 157–162. Bibcode:2000A&A...354..157H.
  15. ^ "HD 358087". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2018.