VZ Camelopardalis

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VZ Camelopardalis
VZCamLightCurve.png
A visual band light curve for VZ Camelopardalis, plotted from data presented by Tabur et al. (2009) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Camelopardalis
Right ascension 07h 31m 04.48017s [2]
Declination +82° 24 41.2905 [2]
Apparent magnitude  (V)4.92 [3]
Characteristics
Evolutionary stage AGB [4]
Spectral type M4IIIa [5]
B−V color index +1.633±0.018 [3]
Variable type Lb? [6]
Astrometry
Radial velocity (Rv)+11.90±0.22 [3]  km/s
Proper motion (μ)RA: −5.249 [2]   mas/yr
Dec.: −42.174 [2]   mas/yr
Parallax (π)6.4908 ± 0.2204  mas [2]
Distance 500 ± 20  ly
(154 ± 5  pc)
Absolute magnitude  (MV)−1.00 [3]
Details
Radius 88.93+7.92
−15.25
[2]   R
Luminosity 1252±48 [2]   L
Temperature 3,641+359
−152
[2]   K
Other designations
VZ Cam, BD+82°201, FK5  3951, GC  9851, HD  55966, HIP  36547, HR  2742, SAO  1179 [7]
Database references
SIMBAD data

VZ Camelopardalis is a single, [8] 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. [3] The star is located at a distance of approximately 500  light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of +12 km/s. [3] It was considered a member of the Hyades Supercluster, [9] but in 1990 this was brought into question. [10]

This object is an aging red giant star on the asymptotic giant branch [4] with a stellar classification of M4IIIa. [5] Its variable nature was discovered by American astronomer J. Ashbrook in 1948. [11] This is a suspected slow irregular variable of sub-type Lb that varies in visual magnitude from 4.80 down to 4.96. [6] Long-term photometry measurements suggest there are at least seven pulsation periods ranging from 27.1 to 249.4 days. [1] 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. [2]

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−1.9
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References

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  2. 1 2 3 4 5 6 7 8 9 10 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  3. 1 2 3 4 5 6 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
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  10. Yamakawa, Fusatoshi; Uji-Iye, Kei-Ichi (August 1990), "A Candidate Star for Irregular Variability", Publications of the Astronomical Society of Japan, 42: L65 –L67, Bibcode:1990PASJ...42L..65Y.
  11. Eggen, Olin J.; Iben, Icko Jr. (April 1991), "First Giant Branch and Asymptotic Giant Branch Stars in Nearby Aggregates", Astronomical Journal, 101: 1377, Bibcode:1991AJ....101.1377E, doi:10.1086/115773.