Chi Aquilae is the Bayer designation for a binary star in the equatorial constellation of Aquila, the eagle. This system is bright enough to be seen with the naked eye at a combined visual magnitude of +5.29. Based upon parallax measurements made during the Hipparcos mission, Chi Aquilae is at a distance of approximately 900 light-years from Earth.
Mu Arietis, Latinized from μ Arietis, is the Bayer designation for a star system in the northern constellation of Aries. It is approximately 340 light-years distant from Earth, give or take a 30 light-year margin of error, and has a combined apparent visual magnitude of 5.74. According to the Bortle Dark-Sky Scale, this means it is faintly visible to the naked eye from dark suburban skies.
28 Cancri is a star system in the zodiac constellation of Cancer. It is a variable star with the designation CX Cancri, and is close to the lower limit of visibility with the naked eye, having a mean apparent visual magnitude of 6.05. The annual parallax shift seen from Earth's orbit is 7.32 mas, which provides a distance estimate of about 450 light years. It is moving away from the Sun with a radial velocity of around +9 km/s.
HD 125351 or A Boötis is spectroscopic binary in the constellation Boötes. The system has an apparent magnitude of +4.97, with a spectrum matching a K-type giant star. It is approximately 233 light years from Earth.
HD 224635 and HD 224636 is a pair of stars comprising a binary star system in the constellation Andromeda. They are located approximately 94 light years away and they orbit each other every 717 years.
HD 225218 is a quadruple star system in the northern constellation of Andromeda. The primary component, HD 225218 A, is a giant star with a stellar classification of B9III, an apparent magnitude of 6.16, and is a candidate Lambda Boötis star. It has a fainter, magnitude 9.65 companion, HD 225218 B, at an angular separation of 5.2″ along a position angle of 171°. The primary itself has been identified as a binary star system through interferometry, with the two components separated by 0.165″. The pair, HD 225218 Aa and Ab, orbit each other with a period of about 70 years and an eccentricity of 0.515. Component B is likewise a spectroscopic binary.
HD 165259 is visual binary star system in the southern constellation of Apus.
HD 216718 is a binary star system in the equatorial constellation of Aquarius.
HD 214448 is a binary star system in the equatorial constellation of Aquarius. They orbit each other with a period of around 147 years. The combined mass of the pair is twice that of the Sun.
HD 200375 is a binary star system in the equatorial constellation of Aquarius. Their orbit does not yet have a unique solution available.
HD 191104 is a star system in the equatorial constellation of Aquila. Two of the components form a close spectroscopic binary system, while a third star, also thought to be a spectroscopic binary, orbits the pair at a greater distance.
HD 188405 is a binary star in the equatorial constellation of Aquila. The pair have an orbital period of roughly 425 years and an angular separation of 1.085″.
UX Arietis is a triple star system located in the northern zodiacal constellation of Aries. Based upon parallax measurements from the Hipparcos satellite, it is roughly 168 light years away. The primary, component Aa, is a variable star of the RS CVn type. The variability of the star is believed due to a combination of cool star spots and warm flares, set against the baseline quiescent temperature of the stellar atmosphere. The variability appears to be cyclical with a period of 8−9 years.
HD 34790 is a double-lined spectroscopic binary star system in the northern constellation of Auriga. It has a combined apparent magnitude of 5.66, which means it is faintly visible to the naked eye. Based upon observations by the Hipparcos satellite, it is located around 289 light years away. It has a combined stellar classification of A1Vs, matching that of an A-type main sequence star, and shines with 35 times the luminosity of the Sun.
HD 126200 is a blue dwarf star in the northern constellation of Boötes. It has been identified as an Algol-type eclipsing binary, although subsequent observations do not confirm this.
HD 127726 is a binary star system in the northern constellation of Boötes.
HD 115337 is a cool supergiant star in the constellation Camelopardalis. It has an apparent magnitude of 6.272 so it is visible under very dark conditions. It is about 680 light-years or 210 parsecs away. It has a much fainter A8 main sequence companion.
HD 44131 is a star in the equatorial constellation of Orion, positioned near the eastern constellation border with Monoceros. It has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.91. The star is located at a distance of approximately 465 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +48.6 km/s. Based on radial velocity variations, it is a candidate spectroscopic binary system and a preliminary orbital solution was published in 1991 with a period of 9.29 yr. However, these velocity variations may be due to other causes.
HD 3322 is a binary star system in the northern constellation of Andromeda. With an apparent visual magnitude of 6.51, it lies below the nominal brightness limit for visibility with the normal naked eye, but it is still possible to see the star with excellent vision under ideal seeing conditions. An annual parallax shift of 4.59±0.65 mas provides a distance estimate of roughly 700 light years.
HD 205877 is a visual binary star system in the constellation Indus. It also a double lined spectroscopic binary. The components are very similar and both are located on the giant branch in the Hertzsprung–Russell diagram in agreement with the F7III spectral type.
