S Vulpeculae
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Vulpecula |
| Right ascension | 19h 48m 23.8067s[1] |
| Declination | 27° 17′ 11.388″[1] |
| Apparent magnitude (V) | 8.974[2] (8.69 - 9.42[3]) |
| Characteristics | |
| Spectral type | G0-K2(M1)[4] |
| U−B color index | ++1.3 - +2.0[5] |
| B−V color index | +1.7 - +2.1[5] |
| Variable type | δ Cep[3] |
| Astrometry | |
| Radial velocity (Rv) | 0.0 ± 2[6] km/s |
| Proper motion (μ) | RA: −4.4 ± 1.2[7] mas/yr Dec.: −5.1 ± 1.1[7] mas/yr |
| Distance | 3,480[2] pc |
| Absolute magnitude (MV) | −6.08[2] |
| Details[2] | |
| Mass | 14.2 M☉ |
| Radius | 382[8] R☉ |
| Luminosity | 28,840 L☉ |
| Temperature | 4,477 K |
| Metallicity [Fe/H] | −0.01[9] dex |
| Age | 12.6 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
S Vulpeculae is a supergiant[10] star in the constellation Vulpecula.
S Vulpeculae was first suspected of varying in brightness in 1836 and this was confirmed by 1862. It has been variously classified as an RV Tauri variable, a semiregular variable star, or a Cepheid variable.[11][4]
S Vulpeculae is now confirmed as a classical Cepheid variable with one of the longest known periods at 68 days,[2] although the period has changed several times.[12] As such, it is also one of the cooler and more luminous of the Cepheids, and it lies close to the zone where semiregular variable stars are found. The shape and amplitude of the light curve varies significantly from cycle to cycle and secularly. The apparent magnitude ranges from 8.69 to 9.42.[3] The spectrum varies from early G to late K as it pulsates, with TiO bands typical of an M1 star when the star is coolest.[4]
References
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