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Sigma Virginis is a star in the zodiac constellation of Virgo. It can be faintly seen with the naked eye with a baseline apparent visual magnitude of 4.86. Based upon parallax measurements, the distance to this star is roughly 680 light-years.
Mu1 Cancri, Latinised from μ1 Cancri, is a variable star in the zodiac constellation of Cancer. The name Mu1 comes from the Bayer naming system: the "1" in the name is because (from Earth) it appears to be close to 10 Cancri, or Mu2 Cancri. It is also known by the variable star designation BL Cancri. The star is dimly visible to the naked eye with an apparent visual magnitude that ranges from 5.87 down to 6.07. Parallax measurements put it about 630 light-years (192 parsecs) from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.28. The position of the star near the ecliptic means it is subject to lunar occultations.
Iota Draconis, also named Edasich, is a star in the northern circumpolar constellation of Draco. A visually unremarkable star of apparent magnitude 3.3, in 2002 it was discovered to have a planet orbiting it. From parallax measurements, this star is located at a distance of about 101.2 light-years from the Sun.
2 Centauri is a single star in the southern constellation of Centaurus, located approximately 183 light-years from Earth. It has the Bayer designation g Centauri; 2 Centauri is the Flamsteed designation. This object is visible to the naked eye as faint, red-hued star with an apparent visual magnitude of 4.19. It is moving away from the Earth with a heliocentric radial velocity of +41 km/s. The star is a member of the HR 1614 supercluster.
W Cephei is a spectroscopic binary and variable star located in the constellation Cepheus. It is thought to be a member of the Cep OB1 stellar association at about 8,000 light years. The supergiant primary star is one of the largest known stars and as well as one of the most luminous red supergiants.
HD 36678 is single star in the northern constellation of Auriga. This star is dimly visible to the naked eye with an apparent visual magnitude of 5.83. It is located at a distance of approximately 840 light years from the Sun based on parallax.
NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away. It is a 6th magnitude star faintly visible to the naked eye under very good observing conditions.
HD 33463 is a suspected variable star in the northern constellation of Auriga, about 1,050 light years away. It is a red giant star with a stellar classification of M2III, and has expanded away from the main sequence after exhausting its core hydrogen. It has reached 133 times the size of the Sun and, at an effective temperature of 3,753 K it shines at a bolometric luminosity of 2,114 L☉.
HD 118508 is a suspected variable star in the northern constellation of Boötes. Its apparent magnitude may vary with an amplitude of 0.04, discovered during a search for small-amplitude red variables. It is a red giant about 552 light years away.
HD 128333 or CH Boötis is an irregular variable star in the northern constellation of Boötes. With an apparent magnitude of 5.7, it is faintly visibly to the naked eye under good observing conditions.
HD 135530 is a suspected variable star in the northern constellation of Boötes.
Kappa Herculis is an optical double star in the constellation of Hercules. The two components, Kappa Herculis A and B, were 27.3 arc seconds apart in 2000. Based on parallax measurements from the Hipparcos mission, κ Her A is about 113 parsecs from the Sun and κ Her B is 600 parsecs ; more recent parallax measurements suggest that B is around 5% more distant than A.
HD 115337 is a binary star located in the northern circumpolar constellation Camelopardalis. The pair have a combined apparent magnitude of 6.25, placing it near the limit for naked eye visibility. Parallax measurements place the system at a distance of 698 light years. It has a heliocentric radial velocity of −9.4 km/s, indicating that it is drifting towards the Solar System.
PZ Cassiopeiae is a red supergiant star located in the constellation of Cassiopeia, and a semi-regular variable star.
Psi Pegasi, which is Latinized from ψ Pegasi, is a binary star system within the great square in the northern constellation of Pegasus. It has a red hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.66. This object is located at a distance of approximately 476 light-years away from the Sun based on parallax, but is drifting closer with a radial velocity of −6.6 km/s.
φ Pegasi, Latinised as Phi Pegasi, is a solitary, reddish hued star in the northern constellation of Pegasus. With an apparent visual magnitude of around 5.1, it is a faint star that can be seen with the naked eye. Based upon an annual parallax shift of 7.05 mas as seen from Earth, the system is located around 460 light years distant from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.15 due to interstellar dust.
T Persei is a red supergiant located in the constellation Perseus. It varies in brightness between magnitudes 8.3 and 9.7 and is considered to be a member of the Double Cluster.
HD 198404 is a star in the equatorial constellation Delphinus. It has an apparent magnitude of 6.19, allowing it to be faintly seen with the naked eye. Parallax measurements place the object at a distance of 395 light years and it is approaching the Solar System with a heliocentric radial velocity of −21.6 km/s.
HD 58425, also known as HR 2830, is an astrometric binary located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye as an orang point of light at an apparent magnitude of 5.64. Based on parallax measurements from Gaia DR3, the system is estimated to be 470 light years away from Earth. It appears to be rapidly receding from the Sun, having a heliocentric radial velocity of 58.6 km/s. HD 58425 is listed as 54 Ursae Majoris in Johann Hevelius' catalogue, but this was dropped after the official IAU's official constellation borders were drawn.
HD 34255, also known HR 1720, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.60, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of about 1.65 kly but is approaching the Solar System with a heliocentric radial velocity of −7.7 km/s.
References
- ESA (1997). "The Hipparcos and Tycho Catalogues" . Retrieved 2006-12-26.
- Kostjuk, N. D. (2002). "HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index" . Retrieved 2006-12-26.
- Roman, N. G. (1987). "Identification of a Constellation from a Position" . Retrieved 2006-12-26.
- "SIMBAD Astronomical Database". Centre de Données astronomiques de Strasbourg. Retrieved 2007-01-02.
- "Naming Stars" . Retrieved 4 July 2018.
- ↑ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv: astro-ph/0409579 , Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304.
- 1 2 Li, Yaguang; Bedding, Timothy R.; Li, Tanda; Bi, Shaolan; Stello, Dennis; Zhou, Yixiao; White, Timothy R. (2020), "Asteroseismology of 36 Kepler subgiants – I. Oscillation frequencies, linewidths, and amplitudes", Monthly Notices of the Royal Astronomical Society, 495 (2): 2363–2386, arXiv: 2005.06460 , doi: 10.1093/mnras/staa1335
- ↑ Metcalfe, T. S.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Molenda-Żakowicz, J.; Appourchaux, T.; Chaplin, W. J.; Doğan, G.; Eggenberger, P.; Bedding, T. R.; Bruntt, H.; Creevey, O. L.; Quirion, P.-O.; Stello, D.; Bonanno, A.; Silva Aguirre, V.; Basu, S.; Esch, L.; Gai, N.; Di Mauro, M. P.; Kosovichev, A. G.; Kitiashvili, I. N.; Suárez, J. C.; Moya, A.; Piau, L.; García, R. A.; Marques, J. P.; Frasca, A.; Biazzo, K.; Sousa, S. G.; et al. (2010). "A Precise Asteroseismic Age and Radius for the Evolved Sun-Like Star Kic 11026764". The Astrophysical Journal. 723 (2): 1583–1598. arXiv: 1010.4329 . Bibcode:2010ApJ...723.1583M. doi:10.1088/0004-637X/723/2/1583. S2CID 56123879.