SV Vulpeculae

SV Vulpeculae is a classical Cepheid (δ Cepheid) variable star in the constellation Vulpecula. It is a supergiant at a distance of 8,700 light years. It is not visible to the naked eye, but can be seen with binoculars.

SV Vulpeculae

A visual band light curve for SV Vulpeculae, plotted from ASAS-SN data[1]
Observation data Epoch J2000      Equinox J2000
Constellation	Vulpecula
Right ascension	19h 51m 30.9060s[2]
Declination	27° 27′ 36.8356″[2]
Apparent magnitude (V)	6.72 - 7.79[3]
Characteristics
Spectral type	F7Iab-K0Iab[3]
U−B color index	+0.868 - +1.659[4]
B−V color index	+1.149 - +1.786[4]
Variable type	δ Cep[3]
Astrometry
Radial velocity (Rv)	−2.00[5] km/s
Proper motion (μ)	RA: −2.139±0.045[2] mas/yr Dec.: −5.820±0.050[2] mas/yr
Parallax (π)	0.3729±0.0303 mas[2]
Distance	8,700 ± 700 ly (2,700 ± 200 pc)
Absolute magnitude (MV)	−5.8[6]
Details
Mass	10[6] M☉
Radius	187.9 - 238.4[7] R☉
Luminosity	15,800[6] L☉
Surface gravity (log g)	0.50 - 1.60[8] cgs
Temperature	4,861 - 6,110[8] K
Metallicity	+0.05[8]
Age	30[6] Myr
Other designations
SV Vul, HD 187921, HIP 97717, BD+27°3536
Database references
SIMBAD	data

In 1921, it was announced that Johanna C. Mackie had discovered the star's brightness varies.^[9] It was given its variable star designation in 1922.^[10] SV Vulpeculae is a δ Cepheid variable whose visual apparent magnitude ranges from 6.72 to 7.79 over 45.0121 days. The light curve is highly asymmetric, with the rise from minimum to maximum taking more less than a third of the time for the fall from maximum to minimum.^[11] The period has been decreasing on average by 214 seconds/year.^[12]

SV Vulpeculae is a yellow bright supergiant around twenty thousand times as luminous as the sun, with a spectral type that varies from late F to early K. It pulsates and varies in temperature from below 5,000 K to above 6,000 K.^[8] The radius is 216.5 R_☉ at maximum, and varies from 188 R_☉ to 238 R_☉ as the star pulsates.^[7]

The mass of SV Vulpeculae is now near 10 M_☉.^[6] The rate of change of the period and the atmospheric abundances show that the star is crossing the instability strip for the second time. The first instability strip crossing occurs rapidly during the transition from the main sequence to becoming a red supergiant. The second crossing occurs during core helium burning when the star executes a blue loop, becoming hotter for a time before returning to the red supergiant stage.^[12]