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Rho Coronae Borealis is a yellow dwarf star 57.1 light-years away in the constellation of Corona Borealis. The star is thought to be similar to the Sun with nearly the same mass, radius, and luminosity. It is orbited by four known exoplanets.
HD 185269 is a stellar triple system approximately 170 light-years away in the constellation Cygnus. It is easily visible to binoculars, but not the naked eye.
HD 192699 is a yellow subgiant star located approximately 214 light-years away in the constellation of Aquila. It has the apparent magnitude of 6.45. Based on its mass of 1.68 solar, it was an A-type star when it was a main-sequence. In April 2007, a planet was announced orbiting the star, together with HD 175541 b and HD 210702 b.
HD 210702 is a star with an orbiting exoplanet in the northern constellation of Pegasus. It has an apparent visual magnitude of 5.93, which is bright enough that the star is dimly visible to the naked eye. The distance to HD 210702 is 177 light years based on parallax measurements, and it is drifting further away with a radial velocity of 18.5 km/s. It is a probable member of the Ursa Major moving group, an association of co-moving stars.
HD 167042 is a star with an orbiting exoplanet in the northern constellation of Draco. With an apparent visual magnitude of +5.97, the star is dimly visible to the naked eye. It is located at a distance of 162 light years based on parallax measurements, but it is drifting closer with a radial velocity of −18 km/s. HD 164595 has a relatively large proper motion, traversing the celestial sphere at an angular rate of 0.270″ yr−1.
Kappa Coronae Borealis, Latinized from κ Coronae Borealis, is a star approximately 98 light years away in the constellation of Corona Borealis. The apparent magnitude is +4.82 and the absolute magnitude is +2.35. It is an orange K-type subgiant star of spectral type K1IV, meaning it has almost completely exhausted its hydrogen supply in its core. It is 1.32 times as massive as the Sun yet has brightened to 11.6 times its luminosity. Around 2.5 billion years old, it was formerly an A-type main sequence star.
HD 167042 b is a gas giant extrasolar planet located approximately 163 light-years away in the constellation of Draco, orbiting the star HD 167042. The mass 1.7 MJ is only minimum since the inclination of the orbital plane is unknown. As it is typical for most known extrasolar planets, it orbits less than 3 AU from the parent star, hence taking less than 2,000 days to revolve. For this planet, it orbits at 1.30 AU and taking 413 days to revolve around the star. Unlike most exoplanets, the eccentricity of the orbit is low, only 3%.
HD 192699 b, also named Khomsa, is an exoplanet located approximately 214 light-years away in the constellation of Aquila, orbiting the star HD 192699. This planet was discovered in April 2007, massing at least 2.5 times the mass of Jupiter (MJ). Despite its orbital distance more than that of Earth, the orbital period is less than a year, because the parent star is more massive than the Sun.
HD 210702 b is an exoplanet located approximately 177 light-years away in the constellation of Pegasus, orbiting the star HD 210702. This planet, together with HD 175541 b and HD 192699 b, are planets around intermediate mass stars that were announced in April 2007 by Johnson et al. It has at least twice the mass of Jupiter and it orbits with semimajor axis of 1.17 AU, corresponding to a period of 341.1 days.
HD 175541 b, also named Kavian, is a jovian planet located approximately 424 light-years away in the constellation of Serpens, orbiting the star HD 175541. This planet was discovered in April 2007. Despite the distance of planet to star slightly more than Earth to the Sun, the period is less than 300 days that orbits in an eccentric orbit, because the parent star is 65% more massive than the Sun.
HD 185269 b is a hot Jupiter extrasolar planet approximately 170 light years away in the constellation of Cygnus. The minimum mass is slightly less than Jupiter and the orbital period is about one week. Most hot Jupiters are thought to have undergone tidal circularization, making the eccentricity of HD 185269 b (e=0.3) unusual. Despite having a large transit probability, none have yet been detected by various photometric monitoring campaigns.
HD 212771 b is an extrasolar planet orbiting the G-type star HD 212771 approximately 364 light years away in the constellation Aquarius.
HD 180902 b is an extrasolar planet orbiting the K-type star HD 180902 approximately 342 light years away in the constellation Sagittarius.
HD 181342 b is an extrasolar planet orbiting the K-type star HD 181342 approximately 394 light years away in the constellation Sagittarius.
HD 180902 is a star with two or more orbiting companions in the southern constellation of Sagittarius. This system is located at a distance of approximately 342 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −2.8 km/s. It has an absolute magnitude of 2.5, but at that distance the apparent visual magnitude of the system is 7.8, which is too faint to be seen with the naked eye.
HD 181342 is a star with an orbiting exoplanet in the constellation of Sagittarius. With an apparent magnitude of 7.55, it cannot be seen with the naked eye. Parallax measurements made by Gaia spacecraft put the star at a distance of 394 light-years away. It is drifting closer with a heliocentric radial velocity of radial_v −0.8 km/s.
HD 102956 b or Isagel is an extrasolar planet discovered in 2010 by a team of American astronomers led by John Johnson using Doppler spectroscopy and the Keck Observatory in Hawaii. HD 102956 b is in the orbit of host star HD 102956. The planet is at most the mass of Jupiter, orbiting every 6.5 days at a distance of 12 million km. HD 202956 b has a very circular orbit. The system is roughly 399 light years from us.
HD 108863 is a subgiant star, the primary of a binary star system 540 light-years away, belonging to spectral class K0. Its age is younger than the Sun's at 1.8±0.4 billion years. The primary star is slightly enriched in heavy elements, having 115% of solar abundance. The primary star does not have detectable flare activity.
HD 99706 is an orange-hued star in the northern circumpolar constellation of Ursa Major. With an apparent visual magnitude of 7.65, it is too dim to be visible to the naked eye but can be viewed with a pair of binoculars. Parallax measurements provide a distance estimate of approximately 480 light years from the Sun, and the Doppler shift shows it is drifting closer with a radial velocity of −30 km/s. It has an absolute magnitude of 2.12, indicating it would be visible to the naked eye as a 2nd magnitude star if it were located 10 parsecs away.
HD 4313 is a star with an orbiting exoplanetary companion in the constellation of Pisces. It has an apparent visual magnitude of 7.83, which is too faint to be reading visible to the unaided eye. The systam is located at a distance of 446 light years based on parallax, and is drifting further away with a radial velocity of 14.5 km/s. This is a single star, which means it has no binary partners, at least in range of projected separations from 6.85 to 191.78 AU. It hosts an extrasolar planet.
References
- 1 2 Johnson, John Asher; et al. (2008). "Retired A Stars and Their Companions. II. Jovian Planets Orbiting κ CrB and HD 167042". The Astrophysical Journal. 675 (1): 784–789. arXiv: 0711.4367 . Bibcode: 2008ApJ...675..784J . doi: 10.1086/526453 .
- 1 2 Luhn, Jacob K.; et al. (2019). "Retired A Stars and Their Companions. VIII. 15 New Planetary Signals around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts". The Astronomical Journal. 157 (4). 149. arXiv: 1811.03043 . Bibcode:2019AJ....157..149L. doi: 10.3847/1538-3881/aaf5d0 . S2CID 102486961.
- ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
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