Back Z Camelopardalis AST Z de la Girafa Catalan Z Camelopardalis German Z Camelopardalis Spanish زد زرافه Persian Z Camelopardalis French Z Жирафа Russian Z Camelopardalis Swedish Z Camelopardalis Turkish Z Жирафи Ukrainian
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 08h 25m 13.199s[2] |
| Declination | +73° 06′ 39.28″[2] |
| Apparent magnitude (V) | 9.8 to 14.5[3] |
| Characteristics | |
| Spectral type | pec(UG)+G1[3] |
| Variable type | UGZ[3] |
| Astrometry | |
| Radial velocity (Rv) | −38.0[4] km/s |
| Proper motion (μ) | RA: −9.003[2] mas/yr Dec.: −19.078[2] mas/yr |
| Parallax (π) | 4.4369 ± 0.0403 mas[2] |
| Distance | 735 ± 7 ly (225 ± 2 pc) |
| Other designations | |
| Database references | |
| SIMBAD | data |
Z Camelopardalis (Z Cam) is a cataclysmic variable star system in the northern constellation of Camelopardalis. It has an apparent visual magnitude which varies between 9.8 and 14.5. This system is the prototype star for the family of Z Camelopardalis variable stars: dwarf novae with standstills at a brightness intermediate between their maxima and minima.[3] It may be the same bright nova that was recorded by Chinese astrologers in the autumn of 77 BCE.[6]
Z Camelopardalis was discovered photographically in 1904 by Henry Park Hollis during work for the Astrographic Catalogue.[7] It is surrounded by an extensive shell thought to have been ejected in a nova explosion,[8] the largest known of its type. The size and expansion of this shell sets a firm lower limit since the last eruption of at least 220 years.[6]
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