Astronomy:DV Aquarii

From HandWiki
Short description: Binary star in the constellation Aquarius
DV Aquarii
DVAqrLightCurve.png
The visual band light curve of DV Aquarii, adapted from Okazaki (1985)[1]
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas
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
SIMBADdata

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. doi:10.1086/131497. Bibcode: 1985PASP...97...62O. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. 
  3. ↑ 3.0 3.1 3.2 Avvakumova, E. A. et al. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten 334 (8): 860. doi:10.1002/asna.201311942. Bibcode: 2013AN....334..860A. http://elar.urfu.ru/bitstream/10995/27061/1/scopus-2013-0239.pdf. 
  4. ↑ 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. 
  5. ↑ 5.0 5.1 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. http://www.aavso.org/vsx/index.php?view=detail.top&oid=989. 
  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. doi:10.1002/asna.200410256. Bibcode: 2004AN....325..740K. 
  8. ↑ 8.0 8.1 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. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 Polubek, G. (December 2001). "DV Aquarii Revisited". Odessa Astronomical Publications 14: 65–68. Bibcode: 2001OAP....14...65P. 
  10. ↑ 10.0 10.1 10.2 10.3 Tokovinin, A. et al. (2008). Tertiary companions to close spectroscopic binaries. 450. Berlin Heidelberg. 129. doi:10.1051/0004-6361:20054427. ISBN 978-3-540-74744-4. Bibcode: 2006yCat..34500681T. 
  11. ↑ 11.0 11.1 11.2 Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. Bibcode: 2012A&A...537A.120Z. 
  12. ↑ 12.0 12.1 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. doi:10.1088/0004-637X/804/2/146. Bibcode: 2015ApJ...804..146D. 
  13. ↑ "HD 199603". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+199603. 
  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. doi:10.1051/aas:1999225. Bibcode: 1999A&AS..136..429C. 
  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. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+358087. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:DV_Aquarii&oldid=3426793"