Y Carinae

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Y Carinae
File:YCarLightCurve.png
A light curve for Y Carinae, plotted from Hipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Carina
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 8.16[3] (7.53Template:Snd8.48[4])
Characteristics
Spectral type F0/3[5] + B9V[6]
B−V Template:Engvar +0.59[3]
Variable type Classical Cepheid[4]
Astrometry
Radial velocity (Rv)−12.90[7] km/s
Proper motion (μ) RA: −5.83[2] mas/yr
Dec.: 3.21[2] mas/yr
Parallax (π)0.3011±0.0358 mas[8]
Distanceapprox. Template:Rnd ly
(approx. Template:Rnd pc)
Absolute magnitude (MV)−3.0[9]
Orbit[9]
PrimaryA
CompanionB
Period (P)1006.9 days
Eccentricity (e)0.437
Semi-amplitude (K1)
(primary)		10.0 km/s
Details
A
Mass4.9[10] Template:Solar mass
Luminosity1,250[9] Template:Solar luminosity
Surface gravity (log g)1.800[3] cgs
Temperature5,800[9] K
Metallicity−0.230[3]
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Y Carinae, Y Car, CD−57°3305, GSC 08613-01464, HD 91595, HIP 51653, 2MASS J10331084-5829550, SAO 238178, Gaia DR2 5351428787262634624
Database references
SIMBADdata

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Y Carinae (Y Car) is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude varies from 7.53 to 8.48.

Alexander W. Roberts discovered that the brightness of the star varies, in 1893.[11][12] The primary Cepheid pulsation period is 3.6 days, but it also pulsates with a secondary period of 2.56 days. It is known as a double-mode Cepheid, or a beat Cepheid since the two periods interfere to produce slow variations at a beat frequency.[9]

The variable primary star is in a triple system with a very close pair of hot main sequence stars. The period of the outer pair is 2.76 years. The inner pair are constrained to orbit in less than 31 days, but the exact nature of the orbit is unknown. The existence of the close binary pair throws into doubt previous calculations of the mass of the pulsating star. The existence of high numbers of triple systems and short period Cepheids suggests that some at least of the short period Cepheids may have formed by mergers.[13]

References

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Template:Stars of Carina

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