DV Aquarii
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.
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 |
Distance | 291 ± 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 | |
Mass | 1.70[9] M☉ |
Radius | 2.756[8] R☉ |
Luminosity | 28.8+2.6 −2.4[10] L☉ |
Surface gravity (log g) | 3.97[10] cgs |
Temperature | 7,843±267[11] K |
Rotational velocity (v sin i) | 103[10] km/s |
Age | 679[11] Myr |
DV Aqr Ab | |
Mass | 1.01[9] M☉ |
Radius | 1.149[8] R☉ |
Surface gravity (log g) | 4.334[8] cgs |
Temperature | 6,056±240[8] K |
Other designations | |
Database references | |
SIMBAD | data |
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
- 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.
- 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.
- 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.
- Adelman, Saul J. (2002). "On the Periods of the Magnetic CP Stars". Baltic Astronomy. 11: 475–485. Bibcode:2002BaltA..11..475A.
- Watson, Christopher (April 19, 2012). "DV Aquarii". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 2015-06-04.
- 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.
- 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.
- Polubek, G. (December 2001). "DV Aquarii Revisited". Odessa Astronomical Publications. 14: 65–68. Bibcode:2001OAP....14...65P.
- Tokovinin, A.; et al. (2008). Tertiary companions to close spectroscopic binaries. VizieR On-line Data Catalog. Berlin Heidelberg. p. 129. arXiv:astro-ph/0601518. Bibcode:2006yCat..34500681T. doi:10.1051/0004-6361:20054427. ISBN 978-3-540-74744-4.
- 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.
- 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.
- "HD 199603". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2018.
- 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.
- Hauck, B.; Jaschek, C. (February 2000). "A-shell stars in the Geneva system". Astronomy and Astrophysics. 354: 157–162. Bibcode:2000A&A...354..157H.
- "HD 358087". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2018.