Astronomy:YY Canis Minoris

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Short description: Binary star in the constellation Canis Minor
YY Canis Minoris
Location of YY Canis Minoris (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Canis Minor
Right ascension  08h 06m 38.55827s
Declination +01° 55′ 46.4758″
Apparent magnitude (V) 8.70[2] (8.460-9.230[3])
Characteristics
Spectral type F1V-IV + F5V-IV[4]
B−V color index +0.45[2]
J−H color index +0.204[5]
J−K color index +0.309[5]
Variable type W UMa[4]
Astrometry
Proper motion (μ) RA: −11.051[6] mas/yr
Dec.: 8.090[6] mas/yr
Parallax (π)4.2234 ± 0.0283[6] mas
Distance772 ± 5 ly
(237 ± 2 pc)
Orbit[4]
PrimaryYY CMi A
CompanionYY CMi B
Period (P)1.0940197 d
Semi-major axis (a)6.41 R☉
Inclination (i)78.76±0.04°
Details[4]
YY CMi A
Mass1.56 M☉
Radius2.52±0.01 R☉
Luminosity13.5 L☉
Surface gravity (log g)3.83±0.01 cgs
Temperature7000±100 K
YY CMi B
Mass1.39 M☉
Radius2.38±0.01 R☉
Luminosity7.2 L☉
Surface gravity (log g)3.83±0.01 cgs
Temperature6161±36 K
Other designations
YY CMi, BD+02°1872, HD 67110, SAO 116352, PPM 153885, TYC 198-1383-1, GSC 00198-01383, 2MASS J08063856+0155464[1]
Database references
SIMBADdata

YY Canis Minoris, abbreviated YY CMi and otherwise referred to as HD 67110, is an eclipsing contact binary in the constellation of Canis Minor, close to the border with Hydra. Its apparent magnitude ranges between 8.46 and 9.23, making it too faint to be seen by the naked eye but visible using binoculars.[7] It is located at a distance of approximately 772 light-years (237 pc) according to Gaia DR3 parallax measurements.

Stellar properties

A light curve for YY Canis Minoris, plotted from TESS data[8]

The system consists of two F-type stars more massive and hotter than the Sun. Both objects are larger than typical F-type main-sequence stars, which may be because they are evolving away from the main sequence. As such, they both received the luminosity class V-IV, with their spectra indicating an intermediate luminosity between main-sequence stars and subgiants.[4]

The two stars orbit each other every 1.094 days, separated by a mere 6.41 solar radii. As a result, both of them are gravitationally distorted and overfilling their Roche lobes, becoming a W Ursae Majoris variable (also known as a low mass contact binary).[4]

Observational history

YY CMi was first reported to be variable in August 1934 by Otto Morgenroth of the Sonneberg Observatory, who described it as an Algol variable with a magnitude range of 8.4 to 8.8.[9] The 1958 edition of the General Catalogue of Variable Stars listed it as a Beta Lyrae variable with a combined spectral type of F5. Krishna Damodar Abhyankar (1962) gave the spectral types F6III and A5V to the two components,[10] though this was noted to be incorrect in 1970 and, in 1981, the two were reclassified as evolved stars of roughly the types F6 and early G comprising a contact binary.[11] This evolved and contact nature of the system has been supported by subsequent studies,[12] but a re-examination of Abhyankar's light curves in 1999 yielded slightly earlier evolutionary stages and spectral types for the stars.[4]

References

  1. ↑ 1.0 1.1 "YY CMi". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=YY+CMi. 
  2. ↑ 2.0 2.1 Høg, E. et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars". Astronomy and Astrophysics 355 (1): L27–L30. Bibcode: 2000A&A...355L..27H. 
  3. ↑ Samus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80–88. doi:10.1134/S1063772917010085. ISSN 1063-7729. Bibcode: 2017ARep...61...80S.  Record for this source at VizieR.
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Vivekananda Rao, P.; Sarma, M. B. K.; Abhyankar, K. D. (1999). "A rediscussion on the eclipsing binary YY Canis Minoris". Astronomy and Astrophysics Supplement Series 139 (1): 57–62. doi:10.1051/aas:1999378. ISSN 0365-0138. Bibcode: 1999A&AS..139...57V. https://aas.aanda.org/articles/aas/pdf/1999/16/ds8332.pdf. Retrieved 2025-01-21. 
  5. ↑ 5.0 5.1 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. 
  6. ↑ 6.0 6.1 6.2 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  7. ↑ Zarenski, Ed (2004). "Limiting Magnitude in Binoculars". Cloudy Nights. http://www.cloudynights.com/documents/limiting.pdf. 
  8. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  9. ↑ Morgenroth, O. (August 1934). "77 neue Veränderliche". Astronomische Nachrichten 252 (24): 389–394. doi:10.1002/asna.19342522402. ISSN 0004-6337. Bibcode: 1934AN....252..389M. 
  10. ↑ Abhyankar, K. D. (1962). "Photometric Elements of YY CMi". Zeitschrift für Astrophysik 54: 25. Bibcode: 1962ZA.....54...25A. 
  11. ↑ Giuricin, G.; Mardirossian, F. (February 1981). "YY CMi : an evolved contact binary system ?". Astronomy and Astrophysics 94: 391-393. Bibcode: 1981A&A....94..391G. 
  12. ↑ Niarchos, P. G.; Mantegazza, L.; Poretti, E.; Manimanis, V. (1998). "YY Canis Minoris: Contact or near contact system?". Astronomy and Astrophysics Supplement Series 133 (1): 7–12. doi:10.1051/aas:1998306. ISSN 0365-0138. Bibcode: 1998A&AS..133....7N. https://aas.aanda.org/articles/aas/pdf/1998/19/ds1534.pdf. Retrieved 2025-01-21. 



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