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Ara is a southern constellation between Scorpius, Telescopium, Triangulum Australe, and Norma. It was one of the Greek bulk described by the 2nd-century astronomer Ptolemy, and it remains one of the 88 modern constellations designated by the International Astronomical Union.
Deneb is a first-magnitude star in the constellation of Cygnus. Deneb is one of the vertices of the asterism known as the Summer Triangle and the "head" of the Northern Cross. It is the brightest star in Cygnus and the 19th brightest star in the night sky, with an average apparent magnitude of +1.25. A blue-white supergiant, Deneb rivals Rigel as the most luminous first-magnitude star. However, its distance, and hence luminosity, is poorly known; its luminosity is somewhere between 55,000 and 196,000 times that of the Sun. Its Bayer designation is α Cygni, which is Latinised to Alpha Cygni, abbreviated to Alpha Cyg or α Cyg.
V539 Arae (Bayer designation Nu1 Arae (ν1 Arae / ν1 Ara)) is a triple star system in the southern constellation of Ara. Based upon an annual parallax shift of 3.30 ± 0.47, this system is at a distance of roughly 1,000 light-years (310 parsecs) from Earth.
Zeta Canis Majoris, or ζ Canis Majoris, also named Furud, is a binary star system in the southern constellation of Canis Major. This system has an apparent visual magnitude of +3.0, making it one of the brighter stars in the constellation and hence readily visible to the naked eye. Parallax measurements from the Hipparcos mission yield a distance estimate of around 362 ly (111 pc) from the Sun. It is drifting further away with a radial velocity of +32 km/s.
27 Canis Majoris is a binary star system in the northern constellation of Canis Major, located approximately 1,700 light years away from the Sun. It has the variable star designation EW Canis Majoris; 27 Canis Majoris is the Flamsteed designation. This system is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of +4.65. It is moving away from the Earth with a heliocentric radial velocity of 16 km/s.
11 Camelopardalis is a single star in the northern circumpolar constellation of Camelopardalis, located around 690 light years away from the Sun as determined by parallax. It has the variable star designation BV Camelopardalis; 11 Camelopardalis is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of +5.22. It forms a double star with 12 Camelopardalis, which is only 3 arcminutes away.
HR 4177, also called t² Carinae, is a double star in the southern constellation of Carina. It is faintly visible to the naked eye with a combined apparent visual magnitude of +4.77. The two components are HD 92397 and HD 92398. The primary component is located at a distance of approximately 1,600 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +11 km/s. It has a peculiar velocity of 24.3+9.9
−16.1 km/s and may be a runaway star. The star is a member of the BH 99 cluster.
HD 165516 is a blue supergiant star in the constellation Sagittarius. It is part of the Sagittarius OB1 association and appears against a rich Milky Way starfield near the Triffid Nebula and Lagoon Nebula.
24 Sextantis, often abbreviated as 24 Sex, is the Flamsteed designation of a 7th-magnitude star located approximately 236 light years away in the constellation of Sextans. At an apparent visual magnitude of 6.61, this star can only be viewed from rural skies under good seeing conditions.
HD 200964 is a 7th magnitude star located approximately 237 light-years away in the constellation of Equuleus. It is a K-type subgiant with 44% more mass than the Sun, but cooler. At the age of 3 billion years, it indicates that it is an evolved A-type star. At a magnitude of 6.64, this star is too faint to be seen with the naked eye for most people, but binoculars would make it easy to see this star. Only people with a very clear eyesight and very dark sky can barely see this star.
50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52, which is bright enough to be seen with the naked eye. Located around 21.00 parsecs (68.5 ly) distant, it is a White main-sequence star of spectral type F7V, a star that is currently fusing its core hydrogen. In 1998 the star was named a candidate Gamma Doradus variable with a period of 3.05 days, which would means it displays variations in luminosity due to non-radial pulsations in the photosphere. Subsequently, it was classified as a RS Canum Venaticorum and BY Draconis variable by an automated program.
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.
- Johnson, John Asher (2010). "Retired a stars and their companions VI. A pair of interacting exoplanet pairs around the subgiants 24 Sextanis and HD200964". The Astronomical Journal. 141 (1): 16. arXiv: 1007.4552 . Bibcode:2011AJ....141...16J. doi:10.1088/0004-6256/141/1/16. S2CID 1010507.
- Rajamohan, R. (2010). "Spectrum variability of 25 Sextantis". Astrophysics and Space Science. 165 (2): 225–230. doi:10.1007/BF00653291. S2CID 119990491.
- Gould, B. A. "Uranometria Argentina". Reprinted and updated by Pilcher, F. Archived from the original on 2012-02-27. Retrieved 2010-07-16.
- "AAVSO Website". American Association of Variable Star Observers. Retrieved 9 March 2014.
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