Lambda Ursae Minoris is a star in the constellation Ursa Minor. It is an M-type red giant with an apparent magnitude of +6.38 and is approximately 880 light years from Earth.
9 Andromedae, abbreviated 9 And by convention, is a variable binary star system in the northern constellation Andromeda. 9 Andromedae is the Flamsteed designation, while it bears the variable star designation AN Andromedae, or AN And. The maximum apparent visual magnitude of the system is 5.98, which places it near the lower limit of visibility to the human eye. Based upon an annual parallax shift of 7.1 mas, it is located 460 light years from the Earth.
WW Aurigae is an eclipsing binary star system in the northern constellation of Auriga. It has a combined maximum apparent visual magnitude of 5.86, which is bright enough to be dimly visible to the naked eye. Based upon an annual parallax shift of 11.0 mas, it is located 297 light years from the Earth. The system is moving further away with a heliocentric radial velocity of −9 km/s, having come to within 212.5 ly some 3.12 million years ago.
ET Andromedae is a binary star system star in the northern constellation of Andromeda. It has an apparent visual magnitude of 6.48, placing it at the nominal limit for visibility with the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.42 mas, which yields a value of 602 light years.
MY Camelopardalis is a binary star system located in the Alicante 1 open cluster, some 13 kly (4.0 kpc) away in the constellation Camelopardalis. It is one of the most massive known binary star systems and a leading candidate for a massive star merger. MY Cam is the brightest star in Alicante 1.
DD Microscopii, also known as CD−43°14304, is a binary star system in the constellation Microscopium. The system has a combined average apparent magnitude around 11, making it readily visible in telescopes but not to the naked eye. It is thought to be at a distance of one or two thousand parsecs, although parallax measurements place the system at a distance of around 30,000 light years.
ADS 1359 is a quadruple star system in the constellation Cassiopeia. It is composed of two sun like stars in an eclipsing binary with a 2.5-day period, which is in turn orbited by an A-type main-sequence star with a 185-year orbital period. There is also HD 236848 which is a distant proper motion companion.
AD Phoenicis is a variable star in the constellation of Phoenix. An eclipsing binary, its apparent magnitude has a maximum of 10.27, dimming to 10.80 during primary and secondary eclipses, which are approximately equal. From parallax measurements by the Gaia spacecraft, the system is located at a distance of 655 light-years from Earth.
BB Phoenicis is a variable star in the constellation of Phoenix. It has an average visual apparent magnitude of 6.17, being visible to the naked eye with excellent viewing conditions. From parallax measurements by the Gaia spacecraft, it is located at a distance of 448 light-years from Earth. Its absolute magnitude is calculated at 0.6.
AI Phoenicis is a variable star in the constellation of Phoenix. An Algol-type eclipsing binary, its apparent magnitude is constant at 8.58 for most of the time, sharply dropping to 9.35 during primary eclipse and to 8.89 during secondary eclipse. The system's variability was discovered by W. Strohmeier in 1972. From parallax measurements by the Gaia spacecraft, the system is located at a distance of 560 light-years from Earth, in agreement with earlier estimates based on its luminosity.
BG Indi, also known as κ1 Indi is a multiple star system in the southern constellation of Indus. Its average apparent magnitude is 6.141, meaning it can only be seen by the naked eye under exceptionally good viewing conditions. Stellar parallax measurements by Gaia put the system at about 166 light-years away.
V346 Centauri is a variable star in the constellation Centaurus. An Algol-type eclipsing binary, its apparent magnitude has a maximum of 8.50, dropping to 8.77 during primary eclipse and to 8.72 during secondary eclipse, the latter being a total eclipse. From parallax measurements by the Gaia spacecraft, the system is located at a distance of about 2300 parsecs (7400 light-years), which is consistent with earlier estimates, based on its luminosity, of 2380 parsecs. The system is a confirmed member of the open cluster Stock 14, which contains many other young OB stars.
SY Equulei, also known as HD 203664, is a single variable star located in the equatorial constellation Equuleus. It has an average apparent magnitude of about 8.5, varying by a few hundredths of a magnitude, making it readily visible in binoculars and small telescopes, but not to the naked eye. The star is relatively far away at a distance of 8,000 light years and is receding with a heliocentric radial velocity of 48 km/s. At that distance, SY Equulei is dimmed by 0.19 magnitudes due to interstellar dust.
HD 40372, also known as 59 Orionis, V1004 Orionis and HR 2100, is a variable star in the constellation Orion. Its apparent magnitude varies between magnitude 5.88 and 5.92, making it faintly visible to the naked eye for an observer far from light polluted urban areas. HD 40372 exhibits two types of variability; it is an eclipsing binary star and one of the two stars is a Delta Scuti variable star.
V380 Cygni is an eclipsing binary star in the constellation Cygnus, located about 3,800 light years away from the Earth. Its apparent magnitude ranges from 5.61 to 5.78, making it faintly visible to the naked eye of an observer located far from city lights. Because it is an important test object for models of massive stars, it has been the subject of many scientific studies.
LZ Cephei, also known by its Flamsteed designation 14 Cephei, is a star about 3,600 light years from the Earth, in the constellation Cepheus. Its apparent magnitude is 5.6, making it faintly visible to the naked eye of an observer far from city lights. The star is a rotating ellipsoidal variable whose brightness, as measured by the Hipparcos satellite, varies between magnitude 5.52 and 5.61.
32 Virginis, also known as FM Virginis, is a star located about 250 light years from the Earth, in the constellation Virgo. Its apparent magnitude ranges from 5.20 to 5.28, making it faintly visible to the naked eye of an observer well away from city lights. 32 Virginis is a binary star, and the more massive component of the binary is a Delta Scuti variable star which oscillates with a dominant period of 103.51 minutes.
GT Muscae, also known as 12 Muscae, is a variable star about 400 light years from the Earth, in the constellation Musca. It is a 5th magnitude star, so it should be faintly visible to the naked eye of an observer far from city lights. It is a quadruple star system, consisting of a spectroscopic binary containing an RS Canum Venaticorum variable star, orbiting an eclipsing binary. It varies in brightness from magnitude 4.96 to 5.23. GT Muscae is a very active X-ray source.
HD 159176, also known as Boss 4444 and V1036 Scorpii, is a variable star about 2,800 light years from the Earth, in the constellation Scorpius. It is a 5th magnitude star, so it should be visible to the naked eye of an observer far from city lights. HD 159176 is the brightest star in the young open cluster NGC 6383. It is a binary star composed of two nearly identical O stars in a circular orbit.
HD 93486, also known as HIP 52381, is a binary star located in the southern circumpolar constellation Chamaeleon near the border with Octans. Its variable star designation is RZ Chamaeleontis. It has an apparent magnitude ranging from 8.2 to 9.1, which is below the limit for naked eye visibility. Gaia DR3 parallax measurements place the system 568 light years away, and it is currently receding with a heliocentric radial velocity of 20 km/s. At its current distance, HD 93486's average brightness is diminished by 0.53 magnitudes due to interstellar dust. The system has a combined absolute magnitude of +1.72.
