Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Virgo |
Right ascension | 12h 14m 20.996s [2] |
Declination | +11° 49′ 09.39″ [2] |
Apparent magnitude (V) | 9.18 [3] |
Characteristics | |
Spectral type | G8V [4] |
B−V color index | 0.81±0.25 [3] |
Variable type | Eclipsing W UMa [5] |
Astrometry | |
Radial velocity (Rv) | 6.6±0.9 [6] km/s |
Proper motion (μ) |
RA: 47.828
mas/
yr
[2] Dec.: −107.737 mas/ yr [2] |
Parallax (π) | 9.6552 ± 0.0203 mas [2] |
Distance | 337.8 ± 0.7
ly (103.6 ± 0.2 pc) |
Absolute magnitude (MV) | 4.25±0.16 [4] |
Absolute bolometric magnitude (Mbol) | 4.07±0.16 [4] |
Orbit [4] | |
Period (P) | 0.4075 d |
Semi-major axis (a) | 2.796±0.017 R☉ |
Eccentricity (e) | 0.0 (assumed) |
Inclination (i) | 85.2±1.2° |
Periastron epoch (T) | 2,448,765 JD |
Argument of periastron (ω) (secondary) | 0.0° |
Semi-amplitude (K1) (primary) | 79.6±1.6 km/s |
Semi-amplitude (K2) (secondary) | 263.5±1.9 km/s |
Details [7] | |
Primary | |
Mass | 1.360 M☉ |
Radius | 1.397 R☉ |
Luminosity | 1.860 L☉ |
Temperature | 5,300 K |
Age | 4.622 Gyr |
Secondary | |
Mass | 0.412 M☉ |
Radius | 0.826 R☉ |
Luminosity | 0.634 L☉ |
Temperature | 5,671 K |
Other designations | |
Database references | |
SIMBAD | data |
AH Virginis is a contact binary [7] star system in the equatorial constellation of Virgo, abbreviated AH Vir. It is a variable star with a brightness that peaks at an apparent visual magnitude of 9.18, making it too faint to be viewed with the naked eye. [3] The distance to this system is approximately 338 light years based on parallax measurements, and it is drifting further away with a mean radial velocity of 7 km/s. [6] O. J. Eggen in 1969 included this system as a probable member of the Wolf 630 group of co-moving stars. [9]
In 1905, this source was identified as an optical double star by W. J. Hussey, with the pair showing an angular separation of 1.27 ″ along a position angle of 15.2°. [10] Gaia Data Release 3 astrometry for the companion is flagged as potentially unreliable but shows a similar parallax and proper motion to AH Virginis. [11]
The brighter visual component was found to be variable by P. Guthnick and R. Prager in 1929, and designated AH Vir. [12] [4] This component was determined to be a W Ursae Majoris variable, and an orbital period of 9.78 hours was found by F. Lause in 1934–1935. [13] Y. C. Chang computed orbital elements of this close binary in 1948 and found the system is eclipsing. [14]
In 1960, L. Binnendijk interpreted the particular shape of the light curve for AH Vir as being due to a sub-luminous region on the primary. [15] Multiple observers noted frequent changes to the light curve and period over time, and in 1977 G. A. Bakos found emission in the calcium K line that suggested mass transfer is taking place. [16] The amplitude of these changes compared to the overall brightness variation is among the largest known among W UMa-type variables. The primary eclipse is total with a duration of around 43 minutes. [17] It was proposed in 1991 that the observed variations in the light curve may be caused by magnetic activity and magnetic interactions between the components. [18]
There has been uncertainty as to whether the two stars are in direct contact with each other, or if the system is semi-detached with only the primary being close to its Roche lobe. The evidence now suggests that they are an overcontact system. The orbital period is showing a increase over time of (2.1869±0.0161)×10−7 d·yr−1, combined with a cyclical variation with a period of 37.19 years. The system shows a strong level of magnetic activity, [19] with the primary being the more active component. [4] The mean magnetic field strength of the primary is estimated as 1.487 kG. The cyclical variation in orbital period may be related to the activity on the primary. [19]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Virgo |
Right ascension | 12h 14m 20.996s [2] |
Declination | +11° 49′ 09.39″ [2] |
Apparent magnitude (V) | 9.18 [3] |
Characteristics | |
Spectral type | G8V [4] |
B−V color index | 0.81±0.25 [3] |
Variable type | Eclipsing W UMa [5] |
Astrometry | |
Radial velocity (Rv) | 6.6±0.9 [6] km/s |
Proper motion (μ) |
RA: 47.828
mas/
yr
[2] Dec.: −107.737 mas/ yr [2] |
Parallax (π) | 9.6552 ± 0.0203 mas [2] |
Distance | 337.8 ± 0.7
ly (103.6 ± 0.2 pc) |
Absolute magnitude (MV) | 4.25±0.16 [4] |
Absolute bolometric magnitude (Mbol) | 4.07±0.16 [4] |
Orbit [4] | |
Period (P) | 0.4075 d |
Semi-major axis (a) | 2.796±0.017 R☉ |
Eccentricity (e) | 0.0 (assumed) |
Inclination (i) | 85.2±1.2° |
Periastron epoch (T) | 2,448,765 JD |
Argument of periastron (ω) (secondary) | 0.0° |
Semi-amplitude (K1) (primary) | 79.6±1.6 km/s |
Semi-amplitude (K2) (secondary) | 263.5±1.9 km/s |
Details [7] | |
Primary | |
Mass | 1.360 M☉ |
Radius | 1.397 R☉ |
Luminosity | 1.860 L☉ |
Temperature | 5,300 K |
Age | 4.622 Gyr |
Secondary | |
Mass | 0.412 M☉ |
Radius | 0.826 R☉ |
Luminosity | 0.634 L☉ |
Temperature | 5,671 K |
Other designations | |
Database references | |
SIMBAD | data |
AH Virginis is a contact binary [7] star system in the equatorial constellation of Virgo, abbreviated AH Vir. It is a variable star with a brightness that peaks at an apparent visual magnitude of 9.18, making it too faint to be viewed with the naked eye. [3] The distance to this system is approximately 338 light years based on parallax measurements, and it is drifting further away with a mean radial velocity of 7 km/s. [6] O. J. Eggen in 1969 included this system as a probable member of the Wolf 630 group of co-moving stars. [9]
In 1905, this source was identified as an optical double star by W. J. Hussey, with the pair showing an angular separation of 1.27 ″ along a position angle of 15.2°. [10] Gaia Data Release 3 astrometry for the companion is flagged as potentially unreliable but shows a similar parallax and proper motion to AH Virginis. [11]
The brighter visual component was found to be variable by P. Guthnick and R. Prager in 1929, and designated AH Vir. [12] [4] This component was determined to be a W Ursae Majoris variable, and an orbital period of 9.78 hours was found by F. Lause in 1934–1935. [13] Y. C. Chang computed orbital elements of this close binary in 1948 and found the system is eclipsing. [14]
In 1960, L. Binnendijk interpreted the particular shape of the light curve for AH Vir as being due to a sub-luminous region on the primary. [15] Multiple observers noted frequent changes to the light curve and period over time, and in 1977 G. A. Bakos found emission in the calcium K line that suggested mass transfer is taking place. [16] The amplitude of these changes compared to the overall brightness variation is among the largest known among W UMa-type variables. The primary eclipse is total with a duration of around 43 minutes. [17] It was proposed in 1991 that the observed variations in the light curve may be caused by magnetic activity and magnetic interactions between the components. [18]
There has been uncertainty as to whether the two stars are in direct contact with each other, or if the system is semi-detached with only the primary being close to its Roche lobe. The evidence now suggests that they are an overcontact system. The orbital period is showing a increase over time of (2.1869±0.0161)×10−7 d·yr−1, combined with a cyclical variation with a period of 37.19 years. The system shows a strong level of magnetic activity, [19] with the primary being the more active component. [4] The mean magnetic field strength of the primary is estimated as 1.487 kG. The cyclical variation in orbital period may be related to the activity on the primary. [19]