RU Camelopardalis
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 07h 21m 44.11647s |
| Declination | +69° 40′ 14.7192″ |
| Apparent magnitude (V) | 8.10 - 9.79 |
| Characteristics | |
| Spectral type | C0,1-C3,2e(K0-R0) |
| U−B color index | +0.97 - +1.17(+0.9 - +1.3) |
| B−V color index | +1.09 - +1.16(+1.0 - +1.4) |
| Variable type | W Vir |
| Astrometry | |
| Radial velocity (Rv) | 21.20 km/s |
| Proper motion (μ) |
RA: 0.24 mas/yr Dec.: −2.10 mas/yr |
| Parallax (π) | 0.71 ± 0.80mas |
| Absolute magnitude (MV) | −2.4 |
| Details | |
| Mass | 0.57 M☉ |
| Luminosity | 417 L☉ |
| Surface gravity (log g) | 1.44 cgs |
| Temperature | 5,250 K |
| Metallicity [Fe/H] | −0.37 dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
RU Camelopardalis, or RU Cam, is a W Virginis variable (type II Cepheid) in the constellation of Camelopardalis. It is also a Carbon star, which is very unusual for a Cepheid variable.
RU Cam was reported as a new variable star in 1907. It was quickly recognised as one of the Cepheid class of variable stars, varying between 8.1 and 9.8 in a period of 22 days.
The first detailed study of the spectrum of RU Cam showed that it changed during the brightness variations. From partway down the descending branch of the light curve to just after minimum brightness, the spectrum is class R with hydrogen absorption lines. The spectrum then develops hydrogen emission lines. For several days either side of maximum brightness, the spectrum becomes a relatively normal class K.
RU Cam remained a somewhat unusual W Virginis variable until 1964, when the relatively regular pulsation of about 1 magnitude almost entirely stopped. Since then the pulsations have varied from cycle to cycle, with amplitudes changing from several tenths of a magnitude to almost zero. The light curve has a more sinusiodal shape than when it was pulsating at full amplitude and the period changes erratically between 17.4 and 26.6 days.
RU Camelopardalis is both a Carbon star and a type II Cepheid variable star. This is unusual but not unique. At least five other relatively bright examples are known, two of which are of the BL Herculis sub-type. The atmosphere contains more carbon than oxygen but is not deficient in hydrogen. This can be explained as the result of triple-alpha helium burning being processed through a CNO cycle and convected to the surface. This process occurs in some of the more massive asymptotic giant branch (AGB) stars at the third dredge-up. W Virginis stars are typically metal-poor and enriched by s-process elements, but this is not the case for RU Cam which has near-solar metallicity and no heavy metal enhancement.
W Virginis variables are thought to be AGB stars executing a blue loop due to a thermal pulse from the helium burning shell. These stars cross the instability strip and undergo very regular pulsations. RU Cam fits this model reasonably well despite its peculiarities. Its temperature of around 5,000 K and luminosity several hundred times the sun's place it on or near the instability strip, and its mass about 0.6 M☉ is typical of AGB stars.
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