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CoRoT was a space telescope mission which operated from 2006 to 2013. The mission's two objectives were to search for extrasolar planets with short orbital periods, particularly those of large terrestrial size, and to perform asteroseismology by measuring solar-like oscillations in stars. The mission was led by the French Space Agency (CNES) in conjunction with the European Space Agency (ESA) and other international partners.
Constantia is a stony background asteroid from the inner region of the asteroid belt, approximately 6.5 kilometers in diameter. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 4 September 1891. The asteroid is a member of the Flora family. It is spinning with a rotation period of 5.345±0.003 h and shows a brightness variation of 0.57±0.2 in magnitude.
14 Aquilae is a probable spectroscopic binary star system in the equatorial constellation of Aquila. 14 Aquilae is the Flamsteed designation though it also bears the Bayer designation g Aquilae. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.42, and it is located at a distance of approximately 500 light-years from Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −39 km/s, and may come as close as 136 light-years in around 3.5 million years.
CoRoT-2 is a yellow dwarf main sequence star a little cooler than the Sun. This star is located approximately 700 light-years away in the constellation of Aquila. The apparent magnitude of this star is 12, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night.
DP Leonis is a binary star system in the equatorial constellation of Leo. It is a variable star that ranges in apparent visual magnitude from 17.5 down to 19. The system is located at a distance of approximately 990 light-years from the Sun based on parallax. It is a cataclysmic variable star of the AM Herculis-type also known as polars. The system comprises an eclipsing white dwarf and red dwarf in tight orbit and an extrasolar planet. This eclipsing variable was discovered by P. Biermann and associates in 1982 as the optical counterpart to the EINSTEIN X-ray source E1114+182.
HD 86226 is a G-type yellowish white star found in the constellation of Hydra.
The Helmi Stream is a stellar stream of the Milky Way galaxy. It started as a dwarf galaxy, now absorbed by the Milky Way as a stream. It was discovered in 1999, is formed of old stars deficient in heavy elements, and has a mass of 10 to 100 million solar masses. It was absorbed by the Milky Way some 6 to 9 billion years ago.
WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.
Phi2 Ceti, Latinized from φ2 Ceti), is a star located in the equatorial constellation of Cetus. φ2 Ceti is also known as 19 Cet, and HD 4813. Based upon parallax measurements, it is located about 51 light years away. It has an apparent visual magnitude of +5.19, making it bright enough to be seen with the naked eye. The star is drifting further away with a radial velocity of +8 km/s.
Phi1 Hydrae, Latinized from φ1 Hydrae, is a yellow-hued star in the constellation Hydra. Its apparent magnitude is 7.61, making it too faint to be seen with the naked eye. Based upon an annual parallax shift of 12.3 mas as seen from Earth, it is located about 266 light years from the Sun. It forms a triangle with the brighter φ2 Hydrae and φ3 Hydrae, between μ Hydrae and ν Hydrae.
WASP-48b is an extrasolar planet orbiting the star WASP-48 in the constellation Cygnus. The planet was detected using the transit method by the SuperWASP team, which published its discovery in 2011. It orbits its host star in just 2.14 days with a semi-major axis of 0.034 AU and has an equilibrium temperature of 1956±54 K. The dayside temperature was measured to be around 2300 K in 2018.
YBP 1194 is a G-type main-sequence star, class G5V, in the open cluster M67 in the constellation Cancer. It is the best solar twin found to date, having the near exact temperature and mass as the Sun. YBP 1194 has a higher metallicity than the Sun and is 0.5 billion years younger at an age of 4.2 billion years old, but due to the distance, the error bar is high at ±1.6 billion years. On December 19, 2013, it was announced to have an extrasolar planet with a period of 6.9 days and a high eccentricity of 0.24 with a mass of 0.34 MJ. It is about 2,772 light-years from the Sun. It is packed in a small cluster, Messier 67, with a radius of 10 ly, with over 500 other stars. For comparison, the Sun has 17 stars at a distance of 10 ly and about 134 stars at a distance of 20 ly.
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.
WR 2 is a Wolf-Rayet star located around 8,000 light years away from Earth in the constellation of Cassiopeia, in the stellar association Cassiopeia OB1. It is smaller than the Sun, but due to a temperature over 140,000 K it is 282,000 times as luminous as the Sun. With a radius of 89% that of the Sun, it is the smallest known WN star in the Milky Way.
HD 21071 is a blue-white hued variable star in the northern constellation of Perseus. Also known as V576 Persei, it is a sixth magnitude star that is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 6.09. The brightness of the star varies with a multiperiodic cycle. The distance to HD 21071, as determined from an annual parallax shift of 6.1 mas, is 535 light years. It is a member of the young Alpha Persei cluster, Melotte 20, and moving is closer to the Earth with a heliocentric radial velocity of −1.5 km/s.
BAT99-7 is a WN-type Wolf-Rayet star located in the Large Magellanic Cloud, in the constellation of Dorado, about 160,000 light years away. The star has a spectrum containing extremely broad emission lines, and is the prototype for the "round line" stars, Wolf-Rayet stars whose spectra are characterized by strong and broad emission lines with round line profiles. The broad emission lines hint at an extremely high temperature of nearly 160,000 Kelvin, which would make it the hottest of all WN stars with known temperatures, as well as an extraordinarily large mass loss rate for a Wolf-Rayet star in the LMC, at 10−4.48 M☉/yr, which means that every 30,200 years, the star loses 1 solar mass worth of mass.
References
- ↑ Parviainen, H.; et al. (2014). "Transiting exoplanets from the CoRoT space mission XXV. CoRoT-27b: A massive and dense planet on a short-period orbit". Astronomy and Astrophysics . 562: A140. arXiv: 1401.1122 . Bibcode:2014A&A...562A.140P. doi:10.1051/0004-6361/201323049. S2CID 46747735.
- ↑ Parviainen, H.; Gandolfi, D.; Deleuil, M.; Moutou, C.; Deeg, H. J.; Ferraz-Mello, S.; Samuel, B.; Csizmadia, Sz; Pasternacki, T.; Wuchterl, G.; Havel, M.; Fridlund, M.; Angus, R.; Tingley, B.; Grziwa, S.; Korth, J.; Aigrain, S.; Almenara, J. M.; Alonso, R.; Baglin, A.; Barros, S. C. C.; Bordé, A. S. P.; Bouchy, F.; Cabrera, J.; Díaz, R. F.; Dvorak, R.; Erikson, A.; Guillot, T.; Hatzes, A.; Hébrard, G.; Mazeh, T.; Montagnier, G.; Ofir, A.; Ollivier, M.; Pätzold, M.; Rauer, H.; Rouan, D.; Santerne, A.; Schneider, J. (1 February 2014). "Transiting exoplanets from the CoRoT space mission XXV. CoRoT-27b: a massive and dense planet on a short-period orbit". Astronomy & Astrophysics. 562: A140. arXiv: 1401.1122 . Bibcode:2014A&A...562A.140P. doi:10.1051/0004-6361/201323049. S2CID 46747735.