31 Camelopardalis

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Template:Short description

31 Camelopardalis
File:TUCamLightCurve.png
A visual band light curve for TU Camelopardalis, adapted from West (1968)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Camelopardalis
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 5.20[3]
Characteristics
Spectral type A2V[4] (A0IV + F0)[5]
U−B Template:Engvar +0.03[6]
B−V Template:Engvar +0.010[3]
Variable type β Lyr[7]
Astrometry
Radial velocity (Rv)Script error: No such module "val".[8] km/s
Proper motion (μ) RA: +1.488[2] mas/yr
Dec.: −17.928[2] mas/yr
Parallax (π)7.1562±0.2336 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Orbit[9]
Period (P)2.9333 d
Eccentricity (e)0.00
Longitude of the node (Ω)0.00°
Periastron epoch (T)Script error: No such module "val".
Semi-amplitude (K1)
(primary)		78.0 km/s
Details
31 Cam A
MassScript error: No such module "val".[10] Template:Solar mass
LuminosityScript error: No such module "val". Template:Solar luminosity
TemperatureScript error: No such module "val". K
Rotational velocity (v sin i)75[10] km/s
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist[4]
Database references
SIMBADdata

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31 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye as a dim point of light with a peak apparent visual magnitude of +5.12.[7] Parallax measurements provide a distance estimate of approximately 460 light years away from the Sun,[2] and the system is drifting closer to the Earth with a radial velocity of −3 km/s.[8]

This is a single-lined spectroscopic binary in a circular orbit with an orbital period of 2.93 days.[9] It is a detached binary with two main sequence components that do not fill their Roche lobes.

Joel Stebbins observed the star for more than thirty nights from 1924 through 1927, and discovered that it is a variable star.[11] It was given its variable star designation, TU Cameleopardis, in 1936.[12] The orbital plane is oriented near the line of sight from the Earth, making this a Beta Lyrae–type eclipsing binary variable star. The primary eclipse lowers the visual magnitude to 5.29, while the secondary eclipse lowers it to 5.22.[7]

References

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  8. ↑ a b Script error: No such module "Citation/CS1".
  9. ↑ a b Script error: No such module "Citation/CS1".
  10. ↑ a b Script error: No such module "Citation/CS1".
  11. ↑ Script error: No such module "Citation/CS1".
  12. ↑ Script error: No such module "Citation/CS1".

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Template:Stars of Camelopardalis

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