Astronomy:AG Virginis

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Short description: Eclipsing binary star in the constellation Virgo
AG Virginis
AGVirLightCurve.png
A visual band light curve for AG Virginis, plotted from ASAS data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Virgo
Right ascension  12h 01m 03.504s[2]
Declination 13° 00′ 30.01″[2]
Apparent magnitude (V) 8.51[3]
Characteristics
Spectral type A7V-A9V[4]
B−V color index 0.289±0.017[3]
Variable type W UMa[5]
Astrometry
Proper motion (μ) RA: −2.740[2] mas/yr
Dec.: −18.255[2] mas/yr
Parallax (π)3.9564 ± 0.0621[2] mas
Distance820 ± 10 ly
(253 ± 4 pc)
Orbit[6]
Period (P)0.6426507 d
Semi-major axis (a)4.477 R☉[7]
Eccentricity (e)0.00 (assumed)
Inclination (i)84.40[7]°
Periastron epoch (T)53,501.5388±0.0013 MJD
Semi-amplitude (K1)
(primary)		93.39±1.06 km/s
Semi-amplitude (K2)
(secondary)		244.24±1.97 km/s
Details
Component 1
Mass2.179[7] M☉
Radius2.185[7] R☉
Luminosity19.0[7] L☉
Temperature8,150[7] K
Metallicity [Fe/H]−0.08±0.09[8] dex
Age2.252[7] Gyr
Component 2
Mass0.739[7] M☉
Radius1.356[7] R☉
Luminosity3.85[7] L☉
Temperature6,915[7] K
Other designations
AG Vir, BD+13°2481, HD 104350, HIP 58605, SAO 99908, PPM 128717[9]
Database references
SIMBADdata

AG Virginis is an eclipsing binary star system in the equatorial constellation of Virgo. With a maximum apparent visual magnitude of 8.51[3] it is too faint to be visible to the naked eye. The system is located at a distance of approximately 820 light years from the Sun based on parallax measurements.[2]

The variability of this system was first reported by P. Guthnick and R. Prager in 1929. R. S. Dugan determined the periodicity in 1933.[10] C. Blanco and F. Catalano in 1970 proposed that this is a semidetached binary where the primary component has filled its Roche lobe, thereby allowing mass transfer. They noted that the orbital period appeared to vary slightly with a ~40 year cycle,[11] which could be explained by a third component.[12] In 1986, J. Kaluzny produced a model for the light curve which suggested this is instead a contact binary. Multiple observers noted a permanent asymmetry to the light curve, with the primary minimum appearing distorted. A localized "hot spot" hypothesis was proposed to explain this feature.[13]

This is a close binary system with an orbital period of 15.4 hours. It is classified as a W Ursae Majoris variable,[6] which means the components are in near contact with each other and their mutual gravitational influence is distorting their shapes. The components are separated by just 4.5 times the radius of the Sun, and the orbital plane is inclined at an angle of 84.4° to the line of sight from the Earth.[7] This causes the two stars to eclipse each other during every orbit. The net visual brightness decreases by 0.58 in magnitude during the primary eclipse and by 0.45 during the secondary eclipse.[14]

The combined spectrum of the system has a varying stellar classification in the range of A7V-A9V,[4] matching an A-type main-sequence star. The primary component has 2.2 times the mass and radius of the Sun, while the secondary has 74% of the Sun's mass and 136% of the radius of the Sun.[7]

References

  1. ↑ "ASAS All Star Catalogue". The All Sky Automated Survey. http://www.astrouw.edu.pl/asas/?page=aasc. 
  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 3.2 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 Hill, G. et al. (1975), "MK Classifications of some Northern Hemisphere Binary Systems", Memoirs of the Royal Astronomical Society 79: 131, Bibcode: 1975MmRAS..79..131H. 
  5. ↑ 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. 
  6. ↑ 6.0 6.1 Pribulla, Theodor et al. (August 2006), "Radial Velocity Studies of Close Binary Stars. XI.", The Astronomical Journal 132 (2): 769–780, doi:10.1086/505536, Bibcode: 2006AJ....132..769P. 
  7. ↑ 7.00 7.01 7.02 7.03 7.04 7.05 7.06 7.07 7.08 7.09 7.10 7.11 7.12 Latković, Olivera et al. (May 2021), "Statistics of 700 Individually Studied W UMa Stars", The Astrophysical Journal Supplement Series 254 (1): 18, doi:10.3847/1538-4365/abeb23, 10, Bibcode: 2021ApJS..254...10L. 
  8. ↑ Rucinski, Slavek M. et al. (September 2013), "Spectroscopic Metallicity Determinations for W UMa-type Binary Stars", The Astronomical Journal 146 (3): 20, doi:10.1088/0004-6256/146/3/70, 70, Bibcode: 2013AJ....146...70R. 
  9. ↑ "AG Vir". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=AG+Vir. 
  10. ↑ Binnendijk, L. (October 1969), "The light variation and orbital elements of AG Virginis", Astronomical Journal 74: 1024–1031, doi:10.1086/110898, Bibcode: 1969AJ.....74.1024B. 
  11. ↑ Blanco, C.; Catalano, F. (1970), "Light curve and elements of AG Vir", Memorie della Società Astronomia Italiana 41: p. 343, Bibcode: 1970MmSAI..41..343B. 
  12. ↑ Avvakumova, E. A. et al. (2014), "Observations of two unusual eclipsing binaries, FN Cam and AG Vir", Baltic Astronomy 23 (3–4): 255–259, doi:10.1515/astro-2017-0188, Bibcode: 2014BaltA..23..255A. 
  13. ↑ Kaluzny, J. (1986), "Contact binaries with components in poor thermal contact. IV. AG Virginis", Acta Astronomica 36: 121–129, Bibcode: 1986AcA....36..121K. 
  14. ↑ 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. 

Further reading

  • Pribulla, T. et al. (July 2011), "O'Connell effect in early-type contact binaries: du Boo and AG Vir", Astronomische Nachrichten 332 (6): 607, doi:10.1002/asna.201111569, Bibcode: 2011AN....332..607P. 
  • Kim, Ho-Il et al. (December 2005), "A Spectroscopic Study of the Close Binary AG Virginis", Journal of Astronomy and Space Sciences 22 (4): 353–362, doi:10.5140/JASS.2005.22.4.353, Bibcode: 2005JASS...22..353K. 
  • Hobart, M. A. et al. (November 1998), "Character of the O-C Variation of Four W UMa Type Stars: AW UMa, AP Leo, AG VIR and AH Vir", Astrophysics and Space Science 260 (3): 375–388, doi:10.1023/A:1001726821949, Bibcode: 1998Ap&SS.260..375H. 
  • Djurašević, Gojko (August 1993), "An Analysis of Close Binaries Based on Photometric Measurements - Part Four - an Interpretation of CB Lightcurve Ag-Virginis by Using the Inverse-Problem Method", Astrophysics and Space Science 206 (1): 119–127, doi:10.1007/BF00658388, Bibcode: 1993Ap&SS.206..119D. 
  • Bell, S. A. et al. (December 1990), "Spots on AG Virginis - paradigm or panacea?", Monthly Notices of the Royal Astronomical Society 247: 632, Bibcode: 1990MNRAS.247..632B. 
  • Michaels, E. J. (June 1988), "AG Virginis: New Times of Minima and Period Study", Information Bulletin on Variable Stars 3202: 1, Bibcode: 1988IBVS.3202....1M. 
  • Niarchos, P. G. (August 1985), "Photoelectric light curves and elements of AG Virginis", Astronomy and Astrophysics Supplement Series 61: 313–318, Bibcode: 1985A&AS...61..313N. 
  • Hill, Graham; Barnes, Jeannette V. (June 1972), "A Spectroscopic Study of AG Virginis", Publications of the Astronomical Society of the Pacific 84 (499): 382, doi:10.1086/129298, Bibcode: 1972PASP...84..382H. 




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