21 Comae Berenices

21 Comae Berenices

A visual band light curve for UU Comae Berenices from MOST data. Adapted from Paunzen et al. (2019)[1]
Observation data Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation	Coma Berenices
Right ascension	12h 31m 00.561s[2]
Declination	+24° 34′ 01.80″[2]
Apparent magnitude (V)	5.47[3] or 5.41 – 5.46[4]
Characteristics
Evolutionary stage	main sequence[1]
Spectral type	A3p SrCr[5]
B−V color index	0.056±0.008[3]
Variable type	α2 CVn[1] + δ Sct[4]
Astrometry
Radial velocity (Rv)	+1.0±1.8[3] km/s
Proper motion (μ)	RA: −12.474 mas/yr[2] Dec.: −9.085 mas/yr[2]
Parallax (π)	12.0785 ± 0.1214 mas[2]
Distance	270 ± 3 ly (82.8 ± 0.8 pc)
Absolute magnitude (MV)	0.66[3]
Details[1]
Mass	2.29±0.10 M☉
Radius	2.6±0.2 R☉
Luminosity	38.2±1.3 L☉
Surface gravity (log g)	3.9±0.2 cgs
Temperature	8,900±200 K
Rotation	2.05219 d
Rotational velocity (v sin i)	63±2 km/s
Age	400–800 Myr
Other designations
Kissīn[6], 21 Com, UU Com, BD+25°2517, HD 108945, HIP 61071, HR 4766, SAO 82346[7]
Database references
SIMBAD	data

21 Comae Berenices is a variable star in the northern constellation of Coma Berenices.^[8] It has the variable star designation UU Comae Berenices, while 21 Comae Berenices is the Flamsteed designation.^[7][8][9]

According to R. H. Allen, English orientalist Thomas Hyde attributed the ancient title Kissīn to this star, a name that comes from a climbing plant – either bindweed or dog rose.^[6] This star has a white hue and is just visible to the naked eye with an apparent visual magnitude that fluctuates around 5.47.^[3] Based upon parallax measurements, it is located at a distance of approximately 270 light years away from the Sun.^[2] It is a single star but is a confirmed physical member of the Melotte 111 open cluster.^[10]

This object has been studied extensively since 1953, producing some occasionally contradictory results such as hints of pulsational behavior or a binary companion. It is a weakly magnetic chemically peculiar star of type CP2, or Ap star, that is most likely on the main sequence.^[1] The stellar classification is A3p SrCr,^[5] where the suffix notation indicates abundance anomalies of the iron-peak element chromium, as well as strontium.

This is an Alpha² Canum Venaticorum (ACV) variable, which indicates it varies in luminosity as it rotates due to spots on its surface created by a magnetic field. The range of variation has an amplitude of 0.02 magnitude and a period of just over two days.^[1] Samus et al. (2017) have it classified as a low-amplitude Delta Scuti variable,^[4] although this is disputed.^[1]

The age of the Melotte 111 cluster, and therefore this star, lies in the range of 400–800 million years. The star has a projected rotational velocity of 63 km/s, with a polar inclination of 64° or greater, resulting in a rotation period of 2.05 days. Stellar evolutionary models yield a mass of around 2.3 times that of the Sun and 2.6 times the Sun's radius for this object. It is radiating 38 times the luminosity of the Sun from its photosphere at an effective temperature of 8,900 K.^[1]