Information about V533 Cassiopeiae
Summary
Maximum magnitude: 12.1 
Minimum magnitude: 14.3 
Type of variability: SRA 

Position information for 31 Okt 2008 17:29:12
JD: 2454771.18694 
Apparent RA: 00h 00m 23.25s 
Apparent Dec: +57° 2' 02.7" 
Constellation: Cassiopeia 
Altitude: +53° 14' 7" 
Azimuth: 54° 35' 56" 
Hour angle: 19h 45m 0s 
Transit: 21h 43m 29s 
Comments: The star is circumpolar and never rises or sets 

Names and Catalog Numbers
GCVS designation: V533 Cassiopeiae 

Star atlas chart numbers
Herald-Bobroff Astroatlas: Chart C-3 
Millennium Star Atlas: Charts 1083-1084 (Vol III) 
Sky Atlas 2000.0: Chart 3 
Uranometria 2000: Chart 35, Vol 1 

Display GCVS Catalog record


General Catalog of Variable Stars Data
General Catalogue of Variable Stars, 4th edition. (Kholopov et al. 1985-88) 
Identification
Name: V533 Cassiopeiae 

Position for epoch J2000.0
RA: 23h 59m 54.4s 
Dec: +56° 58' 47" 

General information
Type of variability: SRA 
Maximum magnitude: 12.1 
Minimum magnitude: 14.3 
Photometric system: V 
Epoch: JD 41250. 
Period: 305. days 
Rise time: Duration of light increase from minimum to maximum (M-m) for physical variables, or the duration of eclipse (D) for Algol-type stars: 50% of period 
Spectrum: C(N) 

Bibliographical references
Study for the star: Z.Alksne, I.Daube, Issledovan. Solntsa i Krasnykh Zvezd N14, 5, 1981. 
Chart or photograph of the field: Z.Alksne, I.Daube, Issledovan. Solntsa i Krasnykh Zvezd N14, 5, 1981. 

Notes
In the region of the cluster NGC 7789.

Variable star classification: SRA
Pulsating variables are stars showing periodic expansion and contraction of their surface layers. The pulsations may be radial or nonradial. A radially pulsating star remains spherical in shape, while in the case of nonradial pulsations the star's shape periodically deviates from a sphere, and even neighboring zones of its surface may have opposite pulsation phases.


SR variables are semiregular variables, which are giants or supergiants of intermediate and late spectral types showing noticeable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to >2000 days, while the shapes of the light curves are rather different and variable, and the amplitudes may be from several hundredths to several magnitudes (usually 1-2 mag in V).


SRA variables are semiregular late-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small (<2.5 mag in V) light amplitudes (Z Aqr). Amplitudes and light-curve shapes generally vary and periods are in the range of 35-1200 days. Many of these stars differ from Miras only by showing smaller light amplitudes.


SRB variables are semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly defined periodicity (mean cycles in the range of 20 to 2300 days) or with alternating intervals of periodic and slow irregular changes, and even with light constancy intervals (RR CrB, AF Cyg). Every star of this type may usually be assigned a certain mean period (cycle), which is the value given in the Catalogue. In a number of cases, the simultaneous presence of two or more periods of light variation is observed.


SRC variables are semiregular late-type (M, C, S or Me, Ce, Se) supergiants (Mu Cep) with amplitudes of about 1 mag and periods of light variation from 30 days to several thousand days.


SRD variables are semiregular variable giants and supergiants of F, G, or K spectral types, sometimes with emission lines in their spectra. Amplitudes of light variation are in the range from 0.1 to 4 mag, and the range of periods is from 30 to 1100 days (SX Her, SV UMa).


SRS variables are semiregular pulsating red giants with short period (several days to month), probably high-overtone pulsators. Prototype: AU Ari.