Astronomy:VV Ursae Majoris

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Short description: Variable star system in the constellation Ursa Major
VV Ursae Majoris
VVUMaLightCurve.png
A light curve for VV Ursae Majoris, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ursa Major
Right ascension  09h 38m 06.719s[2]
Declination +56° 01′ 07.29″[2]
Apparent magnitude (V) 10.19[3]
Characteristics
Spectral type A1.5–2V[4] + G5IV[5]
Variable type Semidetached Algol[6]
Astrometry
Proper motion (μ) RA: −18.536[2] mas/yr
Dec.: 3.254[2] mas/yr
Parallax (π)2.177 ± 0.0394[2] mas
Distance1,500 ± 30 ly
(459 ± 8 pc)
Absolute magnitude (MV)1.87[4]
Orbit
Period (P)0.68735545 d[5]
Semi-major axis (a)3.54[5]"
(4.87 R☉[4])
Eccentricity (e)0.0[7]
Inclination (i)82.07±0.3[4]°
Periastron epoch (T)2,428,925.637 JD[7]
Semi-amplitude (K1)
(primary)		59.6[7] km/s
Details
Primary
Mass0.97[5] M☉
Radius1.35[5] R☉
Luminosity11.2[5] L☉
Surface gravity (log g)4.37[4] cgs
Temperature9,090[5] K
Secondary
Mass0.29[5] M☉
Radius0.96[5] R☉
Luminosity0.42[5] L☉
Surface gravity (log g)4.00[4] cgs
Temperature4,740[5] K
Other designations
VV UMa, BD+56°1395, HIP 47279[8]
Database references
SIMBADdata

VV Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated VV UMa. It is a variable star system with a brightness that cycles around an apparent visual magnitude of 10.19,[3] making it too faint to be visible to the naked eye. The system is located at a distance of approximately 1,500 light years based on parallax measurements.[2]

This star was found to be variable by H. K. Gitz in 1936 based on photographic plates taken in Moscow, then S. Kaho published an ephemeris in 1939 using observed minima.[9] In 1950, O. Struve computed the orbital elements for a single-lined spectroscopic binary system with a short orbital period of just 17 hours. He found a stellar classification of A0V for the primary component.[10] P. Broglia and P. Conconi analyzed the light curve of the system in 1977, and determined this to be a semidetached binary with the secondary component being significantly less massive than the primary.[11] In 1996, V. Simon found a periodic variation in the system minima with a cycle length of 22 years. He proposed that this variation is being driven by a third component in the system.[9]

This is an eclipsing binary;[4] a semi-detached Algol-type system.[6] The best fit spectral type for the primary component is A1.5–2V, matching an A-type main-sequence star. The secondary is a cooler, overluminous, late G-type star;[4] it is a slightly evolved subgiant star that is filling its Roche lobe.[11] The system displays an intrinsic low amplitude variability, which is probably coming from the primary.[4] Multiple pulsation periods have been detected.[12] There is no evidence of an infrared excess.[4]

The light-travel time effect provides information about the properties of the purported third component in the system. It has 0.787 times the mass of the Sun and is orbiting at a distance of 10.75 astronomical unit|AU from the inner pair with an eccentricity of 0.35 and a period of 23.22±0.17 years.[13]

References

  1. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 17 September 2022. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 4.8 4.9 Lázaro, C. et al. (May 2002), "BVRJK Photometry and a Spectroscopic Study of the Algol Short-Period Binary VV Ursae Majoris", The Astronomical Journal 123 (5): 2733–2743, doi:10.1086/339835, Bibcode: 2002AJ....123.2733L. 
  5. ↑ 5.00 5.01 5.02 5.03 5.04 5.05 5.06 5.07 5.08 5.09 5.10 Malkov, Oleg Yu (February 2020), "Semidetached double-lined eclipsing binaries: Stellar parameters and rare classes", Monthly Notices of the Royal Astronomical Society 491 (4): 5489–5497, doi:10.1093/mnras/stz3363, Bibcode: 2020MNRAS.491.5489M. 
  6. ↑ 6.0 6.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  7. ↑ 7.0 7.1 7.2 Lucy, L. B.; Sweeney, M. A. (August 1971), "Spectroscopic binaries with circular orbits", Astronomical Journal 76: 544–556, doi:10.1086/111159, Bibcode: 1971AJ.....76..544L.  See row 19, table 1, p. 540.
  8. ↑ "VV UMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=VV+UMa. 
  9. ↑ 9.0 9.1 Šimon, V. (July 1996), "The cyclic period changes of the close binary VV Ursae Majoris", Astronomy and Astrophysics 311: 915–918, Bibcode: 1996A&A...311..915S. 
  10. ↑ Struve, Otto (July 1950), "Spectrographic Observations of the Eclipsing Binaries TW Cassiopeiae, TY Puppis, and VV Ursae Majoris", Astrophysical Journal 112: 184, doi:10.1086/145326, Bibcode: 1950ApJ...112..184S. 
  11. ↑ 11.0 11.1 Broglia, P.; Conconi, P. (February 1977), "Two-colour photometry and elements of VV UMa", Astronomy and Astrophysics Supplement Series 27: 285–293, Bibcode: 1977A&AS...27..285B. 
  12. ↑ Gunsriwiwat, K.; Mkrtichian, D. E. (September 2015), "Study of Pulsation Spectrum of Mass-accreting Component of Algol-type system VV UMa", Information Bulletin on Variable Stars 6148: 1, Bibcode: 2015IBVS.6148....1G. 
  13. ↑ Tanrıver, Mehmet (April 2015), "Cyclic period changes and the light-time effect in eclipsing binaries: A low-mass companion around the system VV Ursae Majoris", New Astronomy 36: 56–63, doi:10.1016/j.newast.2014.09.008, Bibcode: 2015NewA...36...56T. 

Further reading

  • Ulas, Burak et al. (August 2007), "The Algol-type Binary VV UMa: New VRI Photometry and Search for Pulsations", JENAM-2007, "Our non-stable Universe", held 20–25 August 2007 in Yerevan, Armenia: pp. 21, 21-21, Bibcode: 2007jena.confE..21U. 
  • Kim, S. -L. et al. (February 2005), "On a short-periodic pulsating component in the Algol-type eclipsing binary system VV UMa", Information Bulletin on Variable Stars 5598: 1, Bibcode: 2005IBVS.5598....1K. 
  • Lázaro, C. et al. (August 2001), "uvbyβ photometry of the short-period binary VV Ursae Majoris", Monthly Notices of the Royal Astronomical Society 325 (2): 617–630, doi:10.1046/j.1365-8711.2001.04437.x, Bibcode: 2001MNRAS.325..617L. 
  • Simon, Vojtech (1997), Leung, Kam-Ching, ed., "Period Changes of the Binary VV UMa: Light-Time Effect or Magnetic Activity", The Third Pacific Rim Conference on Recent Development on Binary Star Research. Proceedings of a conference sponsored by Chiang Mai University, Thai Astronomical Society and the University of Nebraska-Lincoln held in Chiang Mai, Thailand, 26 October -1 November 1995, ASP Conference Series 130: p. 277, Bibcode: 1997ASPC..130..277S. 
  • Simon, V. (July 1996), "The cyclic period changes of the close binary VV Ursae Majoris", Astronomy and Astrophysics 311: 915–918, Bibcode: 1996A&A...311..915S. 
  • Wunder, E. (March 1995), "The First Period Change Discovered in the Bright Algol System UV Leonis", Information Bulletin on Variable Stars 4179: 1, Bibcode: 1995IBVS.4179....1W. 
  • Horák, T. (1966), "New elements of the eclipsing variables TW Draconis, RW Tauri and KR Cygni and the influence of the rectification of the light curve upon the elements VV Ursae Maioris", Bulletin of the Astronomical Institute of Czechoslovakia 17: 272, Bibcode: 1966BAICz..17..272H. 
  • Wilson, Robert E. (June 1965), "A possible extended atmosphere in the eclipsing system W UMa", Astronomical Journal 70: 368, doi:10.1086/109749, Bibcode: 1965AJ.....70..368W. 




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