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Phi Serpentis is a solitary star in the Serpens Caput portion of the equatorial constellation Serpens. Based upon an annual parallax shift of 13.52 mas as seen from Earth, it is located about 241 light years distant. The star is faintly visible to the naked eye with an apparent visual magnitude of +5.55.
110 Virginis is a star in the zodiac constellation Virgo, located 195 light-years away from the Sun. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.40. The star is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.
Kappa Aurigae, Latinised from κ Aurigae, is the Bayer designation for a star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 4.3. Based upon an annual parallax shift of 18.43 mas, it is approximately 177 light-years distant from Earth.
30 Aquarii is a single star located about 301 light years away from the Sun in the zodiac constellation of Aquarius. 30 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.56. The star is moving further from the Earth with a heliocentric radial velocity of 40 km/s.
Phi Boötis is a single, yellow-hued star in the northern constellation of Boötes. It is dimly visible to the naked eye with an apparent visual magnitude of +5.24. Based upon an annual parallax shift of 19.22 mas as seen from the Earth, it is located 170 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.09 due to interstellar dust. It is moving closer to the Sun with a radial velocity of −10.6 km/s.
15 Boötis is a binary star system in the northern constellation of Boötes, located approximately 260 light years away from the Sun. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.45. The system has a relatively high proper motion, traversing the celestial sphere at the rate of 0.166 arc seconds per annum. It is moving away from the Earth with a heliocentric radial velocity of +16.8 km/s.
Kappa Capricorni is a solitary star in the constellation Capricornus. It is visible to the naked eye with an apparent visual magnitude of +4.73. Based upon an annual parallax shift of 11.09 mas as seen from the Earth, the star is located about 294 light years from the Sun.
Omega Persei (ω Persei) is a solitary, orange-hued star in the northern constellation of Perseus. The star is faintly visible to the naked eye with an apparent visual magnitude of +4.6. Based upon an annual parallax shift of 11.32 mas as seen from the Earth, the star is about 288 light years from the Sun.
41 Capricorni is a binary star system in the southern constellation of Capricornus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.24. The distance to this star, based upon an annual parallax shift of 19.06±0.29 mas, is around 171 light years. It is moving closer with a heliocentric radial velocity of −45 km/s.
27 Hydrae is a triple star system system in the equatorial constellation of Hydra, located 222 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with a combined apparent visual magnitude of 4.82. The system is moving further from the Earth with a heliocentric radial velocity of +25.6 km/s.
15 Eridani is a binary star system in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.875. Based upon parallax measurements, the system is located around 260 light years away from the Sun. It is moving further from the Earth with a heliocentric radial velocity of 24 km/s.
30 Geminorum is a suspected astrometric binary star system in the northern zodiac constellation of Gemini. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.49. The distance to this star, as estimated through the use of parallax, is about 299 light years. It is drifting further away from the Sun with a heliocentric radial velocity of +9.5 km/s.
Phi Ophiuchi, a name Latinized from φ Ophiuchi, is a single star in the equatorial constellation of Ophiuchus. It has a yellow hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.27. The star is located at a distance of approximately 244 light-years from the Sun based on parallax, but it is drifting closer with a radial velocity of −33.5 km/s.
74 Ophiuchi is a suspected binary star in the equatorial constellation of Ophiuchus, near the border with Serpens Cauda. It is visible to the naked eye as a faint, yellow-hued point of light with a combined apparent visual magnitude of 4.85. The system is located at a distance of 238 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.4 km/s.
19 Puppis is a binary star system in the southern constellation of Puppis, near the northern border with Hydra and Monoceros. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.72. The system is located approximately 177 light years away from the system based on parallax. It is receding from the Earth with a heliocentric radial velocity of +36 km/s, having come to within 31 light-years some 1.4 million years ago.
56 Sagittarii is a single star in the southern constellation of Sagittarius. It has the Bayer designation f Sagittarii, while 56 Sagittarii is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.87. It is located approximately 208 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s.
69 Virginis is a single star in the zodiac constellation of Virgo, located about 259 light years away. It is visible to the naked eye as a faint orange-hued star with an apparent visual magnitude of 4.76, although it is a suspected variable that may range in magnitude from 4.75 down to 4.79. This object is moving closer to the Earth with a heliocentric radial velocity of −13 km/s. The light from this star is polarized due to intervening interstellar dust.
10 Serpentis is a single, white-hued star in Serpens Caput, the western section of the equatorial constellation of Serpens. It is faintly visible to the naked eye with an apparent visual magnitude of 5.15. Located around 129 ly (39.7 pc) distant, it is moving closer to the Sun with a heliocentric radial velocity of −10 km/s and will make its closest approach in around 983,000 years at a separation of about 112 ly (34.2 pc).
6 Serpentis is a binary star system in the constellation Serpens. It has a combined apparent visual magnitude of 5.382, which is bright enough to be faintly visible to the naked eye. The distance to this system, based upon an annual parallax shift of 13.63±0.73 mas, is about 240 light years. It is moving further from the Sun with a heliocentric radial velocity of +10 km/s.
11 Serpentis is a single star in the constellation of Serpens, located 271 light years away from the Sun. It has the Bayer designation A1 Serpentis, 11 Serpentis is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.497. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.
References
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- 1 2 Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
- 1 2 3 4 5 6 7 8 Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi: 10.1088/0004-6256/135/1/209 , S2CID 121883397.
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- ↑ "60 Ser". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-03-19.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society , 389 (2): 869–879, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ↑ Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv: astro-ph/0003329 , Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121.