Global InformationSV Vulpeculae information
 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) | −6.21[6] |
| Details | |
| Mass | 14.6 - 15.8[7] M☉ |
| Radius | 187.9 - 238.4[8] R☉ |
| Luminosity | 19,800[9] L☉ |
| Surface gravity (log g) | 0.50 - 1.60[10] cgs |
| Temperature | 4,861 - 6,110[10] K |
| Metallicity | +0.05[10] |
| Other designations | |
SV Vul, HD 187921, HIP 97717, BD+27°3536 | |
| Database references | |
| SIMBAD | data |
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.
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.[9]
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.[10] The radius is 216.5 R☉ at maximum, and varies from 188 R☉ to 238 R☉ as the star pulsates.[8]
The mass of SV Vulpeculae is now near 15 M☉, and is estimated to have been about 17 M☉ when it was on the main sequence. 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.[9]
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