![]() A light curve for LU Comae Berenices, adapted from Henry et al. (2000). [1] The plotted brightness is the average of the Strömgren b and y magnitudes. | |
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Coma Berenices |
Right ascension | 13h 00m 16.46725s [2] |
Declination | +30° 47′ 06.0644″ [2] |
Apparent magnitude (V) | 4.88 [3] |
Characteristics | |
Evolutionary stage | Hertzsprung gap [4] |
Spectral type | G9 III CH-2 CN-1 [5] |
B−V color index | 1.165±0.014 [6] |
Variable type | RS CVn [7] |
Astrometry | |
Radial velocity (Rv) | −14.34 [8] km/s |
Proper motion (μ) |
RA: −18.662
[2]
mas/
yr Dec.: −5.802 [2] mas/ yr |
Parallax (π) | 4.6981 ± 0.2586 mas [2] |
Distance | 690 ± 40
ly (210 ± 10 pc) |
Absolute magnitude (MV) | −1.62 [6] |
Details [3] | |
Mass | 5.25 M☉ |
Radius | 38.2 R☉ |
Luminosity (bolometric) | 590 L☉ |
Surface gravity (log g) | 2.3 cgs |
Temperature | 4,625 [4] K |
Metallicity [Fe/H] | −0.05 [4] dex |
Rotation | 111 days [4] |
Rotational velocity (v sin i) | 11±1 [4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
37 Comae Berenices is a variable star system located around 690 [2] light years away from the Sun in the northern constellation of Coma Berenices. [9] It has the variable star designation LU Comae Berenices. 37 Comae Berenices was a later Flamsteed designation of 13 Canum Venaticorum. [10] This object is visible to the naked eye as a faint, yellow-hued star with a baseline apparent visual magnitude of 4.88. [3] It is drifting closer to the Earth with a heliocentric radial velocity of −14 km/s. [8]
Tokovinin (2008) catalogued this as a wide triple star system. [4] The primary component is an aging giant star, currently in the Hertzsprung gap, [4] with a stellar classification of G9 III CH-2 CN-1. [5] It is a weak G-band star, [4] a luminous giant star with a carbon abundance about a factor of 5 lower than is typical for such stars. [11] This is a variable star most likely of the RS CVn type with an amplitude of 0.15 in magnitude, [7] and it displays magnetic activity. [4] It has 5.25 times the mass of the Sun and, having exhausted the supply of hydrogen at its core, has expanded to 38 times the Sun's radius. [3]
![]() A light curve for LU Comae Berenices, adapted from Henry et al. (2000). [1] The plotted brightness is the average of the Strömgren b and y magnitudes. | |
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Coma Berenices |
Right ascension | 13h 00m 16.46725s [2] |
Declination | +30° 47′ 06.0644″ [2] |
Apparent magnitude (V) | 4.88 [3] |
Characteristics | |
Evolutionary stage | Hertzsprung gap [4] |
Spectral type | G9 III CH-2 CN-1 [5] |
B−V color index | 1.165±0.014 [6] |
Variable type | RS CVn [7] |
Astrometry | |
Radial velocity (Rv) | −14.34 [8] km/s |
Proper motion (μ) |
RA: −18.662
[2]
mas/
yr Dec.: −5.802 [2] mas/ yr |
Parallax (π) | 4.6981 ± 0.2586 mas [2] |
Distance | 690 ± 40
ly (210 ± 10 pc) |
Absolute magnitude (MV) | −1.62 [6] |
Details [3] | |
Mass | 5.25 M☉ |
Radius | 38.2 R☉ |
Luminosity (bolometric) | 590 L☉ |
Surface gravity (log g) | 2.3 cgs |
Temperature | 4,625 [4] K |
Metallicity [Fe/H] | −0.05 [4] dex |
Rotation | 111 days [4] |
Rotational velocity (v sin i) | 11±1 [4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
37 Comae Berenices is a variable star system located around 690 [2] light years away from the Sun in the northern constellation of Coma Berenices. [9] It has the variable star designation LU Comae Berenices. 37 Comae Berenices was a later Flamsteed designation of 13 Canum Venaticorum. [10] This object is visible to the naked eye as a faint, yellow-hued star with a baseline apparent visual magnitude of 4.88. [3] It is drifting closer to the Earth with a heliocentric radial velocity of −14 km/s. [8]
Tokovinin (2008) catalogued this as a wide triple star system. [4] The primary component is an aging giant star, currently in the Hertzsprung gap, [4] with a stellar classification of G9 III CH-2 CN-1. [5] It is a weak G-band star, [4] a luminous giant star with a carbon abundance about a factor of 5 lower than is typical for such stars. [11] This is a variable star most likely of the RS CVn type with an amplitude of 0.15 in magnitude, [7] and it displays magnetic activity. [4] It has 5.25 times the mass of the Sun and, having exhausted the supply of hydrogen at its core, has expanded to 38 times the Sun's radius. [3]