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HD 147513 is a star in the southern constellation of Scorpius. It was first catalogued by Italian astronomer Piazzi in his star catalogue as "XVI 55". With an apparent magnitude of 5.38, according to the Bortle scale it is visible to the naked eye from suburban skies. Based upon stellar parallax measurements by the Hipparcos spacecraft, HD 147513 lies some 42 light years from the Sun.
Zeta Tauri is a binary star in the zodiac constellation of Taurus, the Bull. It has an apparent visual magnitude of about 3.0, which is bright enough to be seen with the naked eye. Parallax measurements place it at a distance of roughly 440 light-years from the Sun.
ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.
Sigma Tauri is the Bayer designation for a pair of white-hued stars in the zodiac constellation of Taurus. The system is a visual double star, whose components are designated σ1 Tauri and σ2 Tauri, with the latter being the more northerly star. The two are separated by 7.2 arcminutes on the sky and can be readily split with a pair of binoculars. They have apparent visual magnitudes of +5.07 and +4.70, respectively, which indicates they are both visible to the naked eye. Based upon parallax measurements, σ1 Tauri is about 147 light years from the Sun, while σ2 Tauri is 156 light years distant.
Zeta Tucanae, Latinized from ζ Tucanae, is a star in the constellation Tucana. It is a spectral class F9.5 main sequence star with an apparent magnitude of +4.23. Despite having a slightly lower mass, this star is more luminous than the Sun. Based upon parallax measurements by the Hipparcos spacecraft, it is approximately 28.0 light years from Earth. This is one of the least variable stars observed during the Hipparcos mission.
HD 80230 is a single star in the southern constellation of Carina, near the northern constellation border with Vela. It has the Bayer designation g Carinae, while HD 80230 is the star's identifier in the Henry Draper catalogue. This is a suspected variable star with a brightness that has been measured varying from magnitude 4.31 down to 4.35, both of which is bright enough for the star to be visible to the naked eye. The distance to this object is approximately 490 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −5 km/s.
10 Tauri is a single star in the zodiac constellation of Taurus. It can be seen with the naked eye, having an apparent visual magnitude of 4.29. An annual parallax shift of 71.62 mas provides a distance estimate of 45.5 light years. It is moving further from the Sun with a radial velocity of +28 km/s and has a relatively high proper motion.
Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.
HR 3384 is solitary star in the southern constellation of Pyxis. It has an apparent magnitude of 6.38, indicating it is faintly visible to the naked eye. Based on the Bortle scale, the star can be viewed from dark rural skies. Astrometric measurements of the star by the Hipparcos spacecraft, give an estimated distance of about 40 light-years from Earth. It is moving away from the Sun with a radial velocity of +81.91.
111 Tauri is a wide binary star system in the constellation Taurus. It is located at a distance of 48 light years from the Sun. Primary component A is a main sequence star with a stellar classification of F8V. The secondary component B is a K-type main sequence star. The primary is larger and more luminous than the Sun, with about 130% of the Sun's radius and 185% of the Sun's luminosity. The apparent magnitude of 5.0 indicates it is a faint star that can be viewed by the naked eye under good, dark-sky conditions.
61 Leonis is a possible binary star system in the zodiac constellation of Leo. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.73. The star is moving closer to the Sun with a heliocentric radial velocity of −12.7 km/s. It is located roughly 580 light-years from the Sun, as determined from its annual parallax shift of 5.58 mas.
90 Tauri is a star in the zodiac constellation of Taurus, located 144 light-years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.27. 90 Tauri is a member of the Hyades cluster and is listed as a double star.
37 Tauri is a single, orange-hued star in the zodiac constellation of Taurus. It can be seen with the naked eye, having an apparent visual magnitude of 4.36. A magnitude 10.01 visual companion has an angular separation of 134.30″ on a position angle of 138.6°, as of 2003. Based on an annual parallax shift of 17.43±0.21 mas, 37 Tauri is about 187 light years away. It is moving further from the Sun with a heliocentric radial velocity of 9.5 km/s.
114 Tauri, or o Tauri, is a single, blue-white hued star in the zodiac constellation of Taurus. It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.88. The distance to this star, as determined from its annual parallax shift of 5.22±0.21 mas, is roughly 620 light years. It is moving further from the Sun with a heliocentric radial velocity of 16.5 km/s, having come as close as 240 ly (75 pc) some 9.6 million years ago. It is a member of the Cas-Tau OB association of co-moving stars, and has a peculiar velocity of 8.3 km/s.
75 Tauri is a single, orange-hued star in the zodiac of constellation Taurus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.96. Based upon an annual parallax shift of 17.47 mas as seen from Earth's orbit, it is located around 187 light years away. Due to its position near the ecliptic, it is subject to lunar occultations. The star is moving further from the Sun with a heliocentric radial velocity of +16 km/s.
σ Pegasi, Latinised as Sigma Pegasi, is a binary star system in the northern constellation of Pegasus. With a combined apparent visual magnitude of 5.16, it is faintly visible to the naked eye. Based upon an annual parallax shift of 36.66 mas as seen from Earth, the system is located 89 light years distant from the Sun. It has a relatively high proper motion, advancing across the celestial sphere at the rate of 0.524 arcseconds per year.
ζ Pictoris, Latinised as Zeta Pictoris, is a solitary star in the southern constellation of Pictor. It is visible to the naked eye with an apparent visual magnitude of +5.43. Based upon an annual parallax shift of 28.00 mas as seen from the Earth, the system is located 116.5 light years from the Sun.
Omega2 Tauri is a solitary, white hued star in the zodiac constellation of Taurus. It has an apparent visual magnitude of +4.9, which is bright enough to be seen with the naked eye at night. The distance to this system, as determined using an annual parallax shift of 34.55 mas as seen from the Earth, is about 94 light years.
Omega1 Tauri is a solitary, orange hued star in the zodiac constellation of Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.51. Based upon an annual parallax shift of 11.22 mas as seen from Earth, it is located about 290 light years from the Sun.
CQ Tauri is a young variable star in the equatorial constellation of Taurus. It is too faint to be visible to the naked eye with an apparent visual magnitude that ranges from 8.7 to 12.25. The distance to this star is approximately 487 light years based on parallax measurements, and it is drifting further away with a radial velocity of ~23 km/s. It appears to be part of the T-association Tau 4. CQ Tauri lies close enough to the ecliptic to undergo lunar occultations.
References
- 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
- 1 2 3 4 5 6 7 Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv: 1301.1582 , Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78, S2CID 118751608.
- 1 2 3 4 5 6 7 White, Russel J.; et al. (June 2007), "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun", The Astronomical Journal, 133 (6): 2524–2536, arXiv: 0706.0542 , Bibcode:2007AJ....133.2524W, doi:10.1086/514336, S2CID 122854.
- 1 2 3 4 Bernkopf, Jan; Fuhrmann, Klaus (June 2006), "Local subgiants and time-scales of disc formation", Monthly Notices of the Royal Astronomical Society, 369 (2): 673–676, Bibcode:2006MNRAS.369..673B, doi: 10.1111/j.1365-2966.2006.10326.x .
- 1 2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ↑ "m Tau -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg , retrieved 2013-08-12.
- ↑ Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z.; Lachaume, R. (2017-07-21). "The barium-to-iron enrichment versus age relation of ancient disc stars". Monthly Notices of the Royal Astronomical Society. 471 (3). Oxford University Press (OUP): 3768–3774. Bibcode:2017MNRAS.471.3768F. doi:10.1093/mnras/stx1848. ISSN 0035-8711.
- ↑ Holmes, E. K.; et al. (June 2003), "A Survey of Nearby Main-Sequence Stars for Submillimeter Emission", The Astronomical Journal, 125 (6): 3334–3343, Bibcode:2003AJ....125.3334H, doi: 10.1086/375202 .
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