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DV Aquarii

The visual band light curve of DV Aquarii, adapted from Okazaki (1985) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Aquarius
Right ascension 20h 58m 41.84009s [2]
Declination −14° 28′ 59.2527″ [2]
Apparent magnitude (V) 5.89 [3]
Characteristics
Spectral type A9 V [4]
B−V color index 0.244±0.009 [5]
Variable type β Lyr [6]
Astrometry
Radial velocity (Rv)+10.3±7.4 [7] km/s
Proper motion (μ) RA: −54.986 [2]  mas/ yr
Dec.: −18.428 [2]  mas/ yr
Parallax (π)11.2032 ± 0.1015  mas [2]
Distance291 ± 3  ly
(89.3 ± 0.8  pc)
Absolute magnitude (MV)1.25 [5]
Orbit [8]
Period (P)1.5755 d
Eccentricity (e)0 (adopted)
Inclination (i)83.18±0.11 [9]°
Periastron epoch (T)2426160.50 JD
Semi-amplitude (K1)
(primary)		95.5 km/s
Details
DV Aqr Aa
Mass1.70 [10]  M☉
Radius2.756 [9]  R☉
Luminosity28.8+2.6
−2.4 [11]  L☉
Surface gravity (log g)3.97 [11]  cgs
Temperature7,843±267 [12]  K
Rotational velocity (v sin i)103 [11] km/s
Age679 [12]  Myr
DV Aqr Ab
Mass1.01 [10]  M☉
Radius1.149 [9]  R☉
Surface gravity (log g)4.334 [9]  cgs
Temperature6,056±240 [9]  K
Other designations
BD−15° 5848, HD 199603, HIP 103545, HR 8024, SAO 164027 [13]
Database references
SIMBAD data

DV Aquarii is a binary star [10] system in the zodiac constellation of Aquarius. It has a peak apparent visual magnitude of 5.89, [3] 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, [2] 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; [8] the orbital inclination is estimated to be 83.18°±0.11°. [9] 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). [3] The pair have been identified as candidate Herbig Ae/Be stars, [14] and catalogued as A-type shell stars. [15]

A magnitude 10.8 star with the designation HD 358087 [16] 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 [10]

This star was a part of the obsolete constellation Norma Nilotica.

References

  1. ^ Okazaki, A.; Yamasaki, A.; Nurwendaya, C.; Malasan, H. L. (January 1985). "Photometric observations and analysis of the close binary system DV Aquarii". Publications of the Astronomical Society of the Pacific. 97: 62–66. Bibcode: 1985PASP...97...62O. doi: 10.1086/131497. S2CID  121673757.
  2. ^ 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.
  3. ^ a b c Avvakumova, E. A.; et al. (October 2013). "Eclipsing variables: Catalogue and classification" (PDF). Astronomische Nachrichten. 334 (8): 860. Bibcode: 2013AN....334..860A. doi: 10.1002/asna.201311942. hdl: 10995/27061.
  4. ^ Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode: 1988mcts.book.....H.
  5. ^ a b Adelman, Saul J. (2002). "On the Periods of the Magnetic CP Stars". Baltic Astronomy. 11: 475–485. Bibcode: 2002BaltA..11..475A.
  6. ^ Watson, Christopher (April 19, 2012). "DV Aquarii". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 2015-06-04.
  7. ^ 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.
  8. ^ 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.
  9. ^ a b c d e f Polubek, G. (December 2001). "DV Aquarii Revisited". Odessa Astronomical Publications. 14: 65–68. Bibcode: 2001OAP....14...65P.
  10. ^ a b c d Tokovinin, A.; et al. (2008). Tertiary companions to close spectroscopic binaries. Vol. 450. Berlin Heidelberg. p. 129. arXiv: astro-ph/0601518. Bibcode: 2006yCat..34500681T. doi: 10.1051/0004-6361:20054427. ISBN  978-3-540-74744-4. S2CID  8899546. {{ cite book}}: |journal= ignored ( help)
  11. ^ 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. S2CID  55586789.
  12. ^ 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. S2CID  33401607.
  13. ^ "HD 199603". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2018.
  14. ^ Corporon, P.; Lagrange, A.-M. (May 1999). "A search for spectroscopic binaries among Herbig Ae/Be stars". Astronomy and Astrophysics Supplement. 136 (3): 429–444. Bibcode: 1999A&AS..136..429C. doi: 10.1051/aas:1999225.
  15. ^ Hauck, B.; Jaschek, C. (February 2000). "A-shell stars in the Geneva system". Astronomy and Astrophysics. 354: 157–162. Bibcode: 2000A&A...354..157H.
  16. ^ "HD 358087". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2018.
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