2 Camelopardalis

2 Camelopardalis is a triple star^[6] system in the northern circumpolar constellation of Camelopardalis, next to the southern constellation border with Perseus. It is dimly visible to the naked eye with a combined apparent visual magnitude of 5.36.^[2] The system is located at a distance of about 213 light-years (65 parsecs) from the Sun, based on its parallax.^[1] It is drifting further away with a radial velocity of +20 km/s.^[4]

2 Camelopardalis

Observation data Epoch J2000      Equinox J2000
Constellation	Camelopardalis
Right ascension	04h 39m 58.06187s[1]
Declination	+53° 28′ 22.4654″[1]
Apparent magnitude (V)	5.36[2]
Characteristics
A
Spectral type	A8V[3]
U−B color index	+0.05[2]
B−V color index	+0.34[2]
Astrometry
Radial velocity (Rv)	+20.1±3.2[4] km/s
Proper motion (μ)	RA: +44.269[1] mas/yr Dec.: −77.004[1] mas/yr
Parallax (π)	15.3220±0.3790 mas[1]
Distance	213 ± 5 ly (65 ± 2 pc)
Orbit[5]
Primary	2 Cam A
Companion	2 Cam B
Period (P)	26.34 ± 0.05 yr
Semi-major axis (a)	0.1727 ± 0.0023″
Eccentricity (e)	0.846 ± 0.005
Inclination (i)	113.3 ± 3.4°
Longitude of the node (Ω)	12.6 ± 2.5°
Periastron epoch (T)	B 1988.98 ± 0.03
Argument of periastron (ω) (secondary)	42.9 ± 2.6°
Orbit[5]
Primary	2 Cam AB
Companion	2 Cam C
Period (P)	660 yr
Semi-major axis (a)	1.666 ± 0.019″
Eccentricity (e)	0.405 ± 0.015
Inclination (i)	132.5 ± 1.9°
Longitude of the node (Ω)	286.2 ± 1.8°
Periastron epoch (T)	B 2011.7 ± 2.7
Argument of periastron (ω) (secondary)	105.1 ± 5.4°
Details[5]
A
Mass	1.94 M☉
B
Mass	1.45 M☉
C
Mass	1.5 M☉
Other designations
2 Cam, BD+53° 794, HD 29316, HIP 21730, HR 1466, SAO 24744, ADS 3358 ABC, CCDM J04400+5328ABC, WDS 04400+5328
Database references
SIMBAD	2 Cam
	2 Cam AB
	2 Cam C

The primary member of 2 Camelopardalis, designated component A, is an A-type main-sequence star with a spectral type of A8V. It has an apparent magnitude of 5.86, and has a secondary with an apparent magnitude of 7.35, designated component B.^[7] The two orbit each other on a very eccentric orbit with a period of 26.34 years.^[5] Further out, there is an eight-magnitude companion (designated component C), orbiting once every few hundred years.^[5] As the third star was previously thought to be relatively massive for its luminosity, it was suspected of being a binary star itself,^[8] but the current estimate of component C's magnitude as a single star matches its absolute magnitude.^[5]