Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Circinus |
Right ascension | 14h 56m 43.987s [2] |
Declination | −62° 46′ 51.66″ [2] |
Apparent magnitude (V) | 5.110 [3] (5.90 + 5.90) [4] |
Characteristics | |
Spectral type | B3 Ve [5] (B2 + B2) [4] |
B−V color index | +0.00 [3] |
Variable type | GCAS [6] |
Astrometry | |
Proper motion (μ) |
RA: +102.65
[2]
mas/
yr Dec.: +9.35 [2] mas/ yr |
Parallax (π) | 11.82 ± 0.30 mas [2] |
Distance | 276 ± 7
ly (85 ± 2 pc) |
Absolute magnitude (MV) | −2.43/−2.43 [4] |
Orbit [5] | |
Period (P) | 39.62±0.78 yr |
Semi-major axis (a) | 0.08564±0.00056″ |
Eccentricity (e) | 0.3014±0.0081 |
Inclination (i) | 153.3±2.0° |
Longitude of the node (Ω) | 228.0±5.2° |
Periastron epoch (T) | 1993.81±0.12 |
Argument of periastron (ω) (secondary) | 68.6±6.5° |
Details | |
θ Cir A | |
Mass | 9.3±0.6 [7] M☉ |
Surface gravity (log g) | 3.38 [3] cgs |
Temperature | 19,099 [3] K |
Rotational velocity (v sin i) | 195±13 [8] km/s |
Age | 27.1±6.1 [7] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Theta Circini (θ Cir), is a binary star located in the southern constellation of Circinus, to the northwest of Alpha Circini. [6] It is faintly visible to the naked eye with an apparent visual magnitude of 5.110. [3] Based upon an annual parallax shift of 11.82 mas, [2] it is located at a distance of about 276 light years from the Sun.
This is an astrometric binary [10] star system with an orbital period of about 39.6 years, an eccentricity of 0.3, and a semimajor axis of 85.64 mas. [5] The pair show a combined stellar classification of B3 Ve, [5] which matches a B-type main sequence star. [5] The 'e' suffix on the class indicates this is a Be star. Alternate classifications include B4 Vnp [7] and B4npe, [5] with the 'n' indicating broad ("nebulous") absorption lines due to rotation and the 'p' meaning a chemically peculiar star. The two components appear to have similar visual magnitude, mass, and classification. [5] The system behaves as a Gamma Cassiopeiae variable [6] showing occasional outbursts of up to 0.27 in magnitude. [11]
Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Circinus |
Right ascension | 14h 56m 43.987s [2] |
Declination | −62° 46′ 51.66″ [2] |
Apparent magnitude (V) | 5.110 [3] (5.90 + 5.90) [4] |
Characteristics | |
Spectral type | B3 Ve [5] (B2 + B2) [4] |
B−V color index | +0.00 [3] |
Variable type | GCAS [6] |
Astrometry | |
Proper motion (μ) |
RA: +102.65
[2]
mas/
yr Dec.: +9.35 [2] mas/ yr |
Parallax (π) | 11.82 ± 0.30 mas [2] |
Distance | 276 ± 7
ly (85 ± 2 pc) |
Absolute magnitude (MV) | −2.43/−2.43 [4] |
Orbit [5] | |
Period (P) | 39.62±0.78 yr |
Semi-major axis (a) | 0.08564±0.00056″ |
Eccentricity (e) | 0.3014±0.0081 |
Inclination (i) | 153.3±2.0° |
Longitude of the node (Ω) | 228.0±5.2° |
Periastron epoch (T) | 1993.81±0.12 |
Argument of periastron (ω) (secondary) | 68.6±6.5° |
Details | |
θ Cir A | |
Mass | 9.3±0.6 [7] M☉ |
Surface gravity (log g) | 3.38 [3] cgs |
Temperature | 19,099 [3] K |
Rotational velocity (v sin i) | 195±13 [8] km/s |
Age | 27.1±6.1 [7] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Theta Circini (θ Cir), is a binary star located in the southern constellation of Circinus, to the northwest of Alpha Circini. [6] It is faintly visible to the naked eye with an apparent visual magnitude of 5.110. [3] Based upon an annual parallax shift of 11.82 mas, [2] it is located at a distance of about 276 light years from the Sun.
This is an astrometric binary [10] star system with an orbital period of about 39.6 years, an eccentricity of 0.3, and a semimajor axis of 85.64 mas. [5] The pair show a combined stellar classification of B3 Ve, [5] which matches a B-type main sequence star. [5] The 'e' suffix on the class indicates this is a Be star. Alternate classifications include B4 Vnp [7] and B4npe, [5] with the 'n' indicating broad ("nebulous") absorption lines due to rotation and the 'p' meaning a chemically peculiar star. The two components appear to have similar visual magnitude, mass, and classification. [5] The system behaves as a Gamma Cassiopeiae variable [6] showing occasional outbursts of up to 0.27 in magnitude. [11]