YY Canis Minoris

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YY Canis Minoris
Canis Minor constellation map.svg
Red circle.svg
Location of YY Canis Minoris (circled)
Observation data
Epoch J2000 [1]        Equinox J2000 [1]
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  mas [6]
Distance 772 ± 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
Mass 1.56  M☉
Radius 2.52±0.01  R☉
Luminosity 13.5  L☉
Surface gravity (log g)3.83±0.01  cgs
Temperature 7000±100  K
YY CMi B
Mass 1.39  M☉
Radius 2.38±0.01  R☉
Luminosity7.2  L☉
Surface gravity (log g)3.83±0.01  cgs
Temperature 6161±36  K
Other designations
YY CMi, AG+02°1064, BD+02°1872, Gaia DR3  3090880296971961216, HD  67110, SAO  116352, PPM  153885, TIC  452928315, TYC  198-1383-1, GSC  00198-01383, 2MASS J08063856+0155464 [1]
Database references
SIMBAD data

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.

Contents

Stellar properties

A light curve for YY Canis Minoris, plotted from TESS data YYCMiLightCurve.png
A light curve for YY Canis Minoris, plotted from TESS data

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]

Related Research Articles

<span class="mw-page-title-main">Canis Minor</span> Constellation in the northern celestial hemisphere

Canis Minor is a small constellation in the northern celestial hemisphere. In the second century, it was included as an asterism, or pattern, of two stars in Ptolemy's 48 constellations, and it is counted among the 88 modern constellations. Its name is Latin for "lesser dog", in contrast to Canis Major, the "greater dog"; both figures are commonly represented as following the constellation of Orion the hunter.

<span class="mw-page-title-main">Castor (star)</span> Sextuple star system in Gemini

Castor is the second-brightest object in the zodiac constellation of Gemini. It has the Bayer designation α Geminorum, which is Latinised to Alpha Geminorum and abbreviated Alpha Gem or α Gem. With an apparent visual magnitude of 1.58, it is one of the brightest stars in the night sky. Castor appears singular to the naked eye, but it is actually a sextuple star system organized into three binary pairs. Although it is the 'α' (alpha) member of the constellation, it is half a magnitude fainter than 'β' (beta) Geminorum, Pollux.

<span class="mw-page-title-main">Beta Canis Minoris</span> Star in the constellation Canis Minor

Beta Canis Minoris, also named Gomeisa, is a star in the constellation of Canis Minor. In the night sky it is notable for its proximity to the prominent star Procyon.

<span class="mw-page-title-main">Iota Canis Majoris</span> Variable star in the constellation Canis Major

Iota Canis Majoris, Latinized from ι Canis Majoris, is a solitary variable supergiant star in the southern constellation of Canis Major. It is visible to the naked eye with an apparent visual magnitude that varies between +4.36 and +4.40. The distance to this star is approximately 2,500 light years based on spectroscopic measurements. It is drifting further away with a radial velocity of +42 km/s.

<span class="mw-page-title-main">UW Canis Majoris</span> Beta Lyrae variable star in the constellation Canis Major

UW Canis Majoris is a star in the constellation Canis Major. It is classified as a Beta Lyrae eclipsing contact binary and given the variable star designation UW Canis Majoris. Its brightness varies from magnitude +4.84 to +5.33 with a period of 4.39 days. Bode had initially labelled it as Tau2 Canis Majoris, but this designation had been dropped by Gould and subsequent authors. It is visible to the naked eye of a person under good observing conditions.

Delta<sup>3</sup> Canis Minoris Star in the constellation Canis Minor

Delta3 Canis Minoris, Latinized from δ3 Canis Minoris, is a solitary, white-hued star in the equatorial constellation of Canis Minor. Based upon a parallax of 4.46 mas as seen from Gaia spacecraft in its repeated orbits around the Sun, just beyond the Earth. This star is about 730 light years from the Solar System. At that distance, the visual magnitude of these stars is diminished by an extinction of more than 0.15 due to interstellar dust. With an apparent visual magnitude of +5.81, it is just bright enough to be faintly visible to the naked eye.

<span class="mw-page-title-main">Eta Canis Minoris</span> Binary star system in the constellation Canis Minor

Eta Canis Minoris is a binary star system in the equatorial constellation of Canis Minor. It is approximately 318 light-years from Earth.

1 Canis Minoris is a single star in the equatorial constellation of Canis Minor, located about 287 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.37. The radial velocity of this object is poorly constrained at −1.0±4.2 km/s.

11 Canis Minoris is a single star in the equatorial constellation of Canis Minor, located around 313 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.25. This object is moving away from the Earth with a heliocentric radial velocity of +28 km/s, having come to within 157 light-years some 2.35 million years ago.

HR 178 is a probable binary star in the constellation Andromeda. Located approximately 124 parsecs (400 ly) distant, it is an evolved Am star with a combined apparent magnitude of 6.06, meaning that it can only be seen with the naked eye on dark, clear nights. The star is suspected of variability, possibly varying between magnitudes 6.04 and 6.06. The variable magnitude period of HD 3883 is about 9.17 min.

<span class="mw-page-title-main">LS Canis Majoris</span> Binary star system in the constellation Canis Major

LS Canis Majoris is an eclipsing binary star located around 1,510 light years from Earth in the constellation Canis Major. Its apparent magnitude ranges from 5.63 to 5.79, so it is faintly visible to the naked eye. The orbital period of binary pair and the period of light variation is 70.048 days.

<span class="mw-page-title-main">BU Canis Minoris</span> Star in the constellation Canis Minor

BU Canis Minoris is a quadruple star system in the equatorial constellation of Canis Minor. It has the Henry Draper Catalogue designation of HD 65241, while BU Canis Minoris is its variable star designation. The system is a challenge to view with the naked eye, having a peak apparent visual magnitude of 6.42. It is located at a distance of approximately 700 light years from the Sun based on parallax, and is drifting further away with a radial velocity of about +34 km/s.

<span class="mw-page-title-main">S Canis Minoris</span> Variable star in the constellation Canis Minor

S Canis Minoris is a variable star in the equatorial constellation Canis Minor. It has a peak apparent visual magnitude of 6.5, so not normally visible to the naked eye. The star is located at a distance of approximately 1,340 light-years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of about +68 km/s.

<span class="mw-page-title-main">AZ Canis Minoris</span> A-type subgiant star in the constellation Canis Minor

AZ Canis Minoris is a variable star in the equatorial constellation of Canis Minor. It is just visible to the naked eye in good viewing conditions as a dim, white-hued star with an apparent visual magnitude of around 6.46. The star is located around 500 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +15 km/s. No evidence has been found for a companion to this star, although in the past it has been reported as a binary star system.

<span class="mw-page-title-main">31 Cygni</span> Triple star system in the constellation Cygnus

31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, ο2 Cygni or V695 Cygni, is a ternary star system about 750 light years away in the constellation Cygnus.

<span class="mw-page-title-main">V915 Scorpii</span> Variable star in the constellation Scorpius

V915 Scorpii is a hypergiant and semiregular variable star, located 1,718 parsecs (5,600 ly) away in the constellation Scorpius. Its apparent magnitude varies between 6.22 and 6.64, being heavily diminshed by 2.93 magnitudes due to interstellar extinction. When it is at its brightest, it is very faintly visible to the naked eye under excellent observing conditions.

<span class="mw-page-title-main">BG Canis Minoris</span> Variable star in the constellation of Canis Minor

BG Canis Minoris is a binary star system in the equatorial constellation of Canis Minor, abbreviated BG CMi. With an apparent visual magnitude that fluctuates around 14.5, it is much too faint to be visible to the naked eye. Parallax measurements provide a distance estimate of approximately 2,910 light years from the Sun.

<span class="mw-page-title-main">HD 31134</span> Star in the constellation of Camelopardalis

HD 31134, also designated as HR 1561, is a solitary star located in the northern circumpolar constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued star with an apparent magnitude of 5.74. Gaia DR3 parallax measurements place it 473 light years away. It appears to be approaching the Solar System with a heliocentric radial velocity of −15.1 km/s. At its current distance, HD 31134's brightness is diminished by 0.35 magnitudes due to interstellar dust. It has an absolute magnitude of +0.19.

<span class="mw-page-title-main">HD 194783</span> HgMn star; Microscopium

HD 194783 is a solitary star located in the southern constellation Microscopium near the border with Sagittarius. It is barely visible to the naked eye as a bluish-white-hued point of light with an apparent magnitude of 6.08. The object is located relatively far at a distance of 740 light-years based on Gaia DR3 parallax measurements, but it is drifting closer with a heliocentric radial velocity of −9.7 km/s. At its current distance, HD 194783's brightness is diminished by an interstellar extinction of 0.31 magnitudes and it has an absolute magnitude of either −0.59 or −1.10, depending on the source.

<span class="mw-page-title-main">V1149 Orionis</span> Binary star in the constellation Orion

HD 37824 is a spectroscopic binary star system in the constellation of Orion. It has the variable-star designation V1149 Orionis. With an apparent magnitude of 6.59, it is near the limit for naked eye observation from Earth, faintly visible as an orange-hued dot of light under dark skies. It is located approximately 492 light-years distant according to Gaia DR3 parallax measurements, and is moving further away at a heliocentric radial velocity of 26.90 km/s.

References

  1. 1 2 3 "YY CMi". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 21 January 2025.
  2. 1 2 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. Record for this source at VizieR.
  4. 1 2 3 4 5 6 7 Vivekananda Rao, P.; Sarma, M. B. K.; Abhyankar, K. D. (1999). "A rediscussion on the eclipsing binary YY Canis Minoris" (PDF). Astronomy and Astrophysics Supplement Series. 139 (1): 57–62. doi: 10.1051/aas:1999378 . ISSN   0365-0138 . Retrieved 21 January 2025.
  5. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (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. 1 2 3 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  7. ↑ Zarenski, Ed (2004). "Limiting Magnitude in Binoculars" (PDF). Cloudy Nights. Archived (PDF) from the original on 21 July 2011. Retrieved 6 May 2011.
  8. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 22 January 2025.
  9. ↑ Morgenroth, O. (August 1934). "77 neue Veränderliche". Astronomische Nachrichten. 252 (24): 389–394. Bibcode:1934AN....252..389M. doi:10.1002/asna.19342522402. ISSN   0004-6337.
  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?" (PDF). Astronomy and Astrophysics Supplement Series. 133 (1): 7–12. doi: 10.1051/aas:1998306 . ISSN   0365-0138 . Retrieved 21 January 2025.
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