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g Herculis is a binary star system in the northern constellation of Hercules. It has the Flamsteed designation 30 Herculis,while g Herculis is the Bayer designation. This system is visible to the naked eye as a faint,red-hued point of light. Based upon a measured parallax of 9.2 mas,it is located around 354 light years away from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of 1.5 km/s.
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GW Orionis is a T Tauri type pre-main sequence hierarchical triple star system. It is associated with the Lambda Orionis star-forming region and has an extended circumtrinary protoplanetary disk.
KH 15D,described as a winking star because of its unusual dips in brightness,is a binary T Tauri star system embedded in a circumbinary disk. It is a member of the young open cluster NGC 2264,located about 2,500 light-years (770 pc) from the Sun in the constellation of Monoceros.
RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away,belonging to the Taurus-Auriga association of the Taurus Molecular Cloud. RW Aurigae B was discovered in 1944.
TX Ursae Majoris is an eclipsing binary star system in the northern circumpolar constellation of Ursa Major. With a combined apparent visual magnitude of 6.97,the system is too faint to be readily viewed with the naked eye. The pair orbit each other with a period of 3.063 days in a circular orbit,with their orbital plane aligned close to the line of sight from the Earth. During the primary eclipse,the net brightness decreases by 1.74 magnitudes,while the secondary eclipse results in a drop of just 0.07 magnitude. TX UMa is located at a distance of approximately 780 light years from the Sun based on parallax measurements,but is drifting closer with a mean radial velocity of −13 km/s.
UX Ursae Majoris is an Algol type binary star system in the northern circumpolar constellation of Ursa Major. It is classified as a nova-like variable star similar to DQ Herculis,although no eruptions have been reported. Since its discovery in 1933,this system has been the subject of numerous studies attempting to determine its properties. The combined apparent visual magnitude of UX UMa ranges from 12.57 down to 14.15. The system is located at a distance of approximately 952 light years from the Sun based on parallax,and is drifting further away with a radial velocity of 112 km/s.
CV Serpentis is a binary star system in the equatorial constellation of Serpens. It is a detached eclipsing binary with an orbital period of 29.7 days. The system includes a Wolf–Rayet (WR) star with the identifier WR 113. The system is located at a distance of approximately 6,700 light years from the Sun based on parallax measurements. It is a member of the Serpens OB2 association of co-moving stars.
AW Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major,abbreviated AW UMa. It is an A-type W Ursae Majoris variable with an apparent visual magnitude of 6.83,which is near the lower limit of visibility to the naked eye. This is an eclipsing binary with the brightness dropping to magnitude 7.13 during the primary eclipse and to 7.08 with the secondary eclipse. Parallax measurements give a distance estimate of 221 light years from the Sun. It is drifting closer to the Sun with a radial velocity of approximately −17 km/s. The system has a high proper motion,traversing the celestial sphere at the rate of 0.216 arc second per annum.
V356 Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius,abbreviated V356 Sgr. It has a peak apparent visual magnitude of 6.84,which decreases to 7.66 during the primary eclipse and 7.24 with the secondary eclipse. Based on parallax measurements,this system is located at a distance of approximately 2,210 light years from the Sun.
References
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- ↑ "College hosts astronomer". The York Dispatch. March 25, 1986. p. 24.
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- 1 2 "USF adds 52 to Faculty". Lancaster New Era. March 27, 1986. p. 3.
- ↑ "A big eye for USF". The Tampa Times. July 25, 1968. p. 12.
- ↑ "Wilson to lecture at planetarium". Florence Morning News. July 25, 1968. p. 7.
- ↑ "G". goddardretirees.org.
- ↑ Oswalt, T. D. (1992). "1992IAPPP..49...39O Page 39". International Amateur-Professional Photoelectric Photometry Communications. 49: 39. Bibcode:1992IAPPP..49...39O.
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- 1 2 Wilson, R. E. (1994). "Binary-Star Light-Curve Models". Publications of the Astronomical Society of the Pacific. 106 (703): 921–941. Bibcode:1994PASP..106..921W. doi:10.1086/133464. JSTOR 40680452 – via JSTOR.
- ↑ Kopal, Zdenek (1955). "1955AnAp...18..379K Page 379". Annales d'Astrophysique. 18: 379. Bibcode:1955AnAp...18..379K.
- ↑ Kopal, Zdenek (1959). "1959ASPL....8...81K Page 81". Leaflet of the Astronomical Society of the Pacific. 8 (361): 81. Bibcode:1959ASPL....8...81K.
- ↑ "Close binary systems | WorldCat.org". search.worldcat.org.