VZ Camelopardalis

VZ Camelopardalis

File:VZCamLightCurve.png A visual band light curve for VZ Camelopardalis, plotted from data presented by Tabur et al. (2009)
Observation data Epoch J2000      Equinox J2000
Constellation	Camelopardalis
Right ascension	Template:RA
Declination	Template:DEC
Apparent magnitude (V)	4.92
Characteristics
Evolutionary stage	AGB
Spectral type	M4IIIa
B−V Template:Engvar
Variable type	Lb?
Astrometry
Radial velocity (Rv)	km/s
Proper motion (μ)	RA: −5.249 mas/yr Dec.: −42.174 mas/yr
Parallax (π)	6.4908±0.2204 mas
Distance	Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)	−1.00
Details
Radius	Template:Solar radius
Luminosity	Template:Solar luminosity
Temperature	K
Metallicity [Fe/H]	{{{metal_fe2}}} dex
Other designations
Template:Odlist
Database references
SIMBAD	data

VZ Camelopardalis is a single, variable star in the northern circumpolar constellation of Camelopardalis. It has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.92. The star is located at a distance of approximately 500 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +12 km/s. It was considered a member of the Hyades Supercluster, but in 1990 this was brought into question.

This object is an aging red giant star on the asymptotic giant branch with a stellar classification of M4IIIa. Its variable nature was discovered by American astronomer J. Ashbrook in 1948. This is a suspected slow irregular variable of sub-type Lb that varies in visual magnitude from 4.80 down to 4.96. Long-term photometry measurements suggest there are at least seven pulsation periods ranging from 27.1 to 249.4 days. With the supply of hydrogen at its core exhausted the star has cooled and expanded until it has now reached 89 times the radius of the Sun. It is radiating 1,252 times the luminosity of the Sun from its photosphere at an effective temperature of 3,641 K.