HD 51418 (NY Aurigae) is an Ap star and an α2 CVn variable located about 178 parsecs (580 ly) away in the northern constellation of Auriga. With an apparent magnitude of 6.67 and a spectral type of A0, it can be faintly visible by the naked eye as a whitish dot under very good circumstances. The star has been noted as an "extreme lanthanide star," [6] with an overabundance of metals including europium, dysprosium, and holmium, which can be observed in the star's spectra as emission lines. [2] [7]
In 1972, Austin F. Gulliver et al. announced that HD 51418 is a variable star. [9] It was given its variable star designation, NY Aurigae, in 1975. [10] HD 51418 possesses a strong magnetic field, which fluctuates in strength between −22–75 milliteslas (−220–750 G ). [11] The magnetic minimum is known to occur concurrently with the minimums in luminosity and rare-earth detection. [7]
Speckle imaging observations conducted in 2009 revealed a previously unresolved companion star at a separation of 0.15 arcseconds. The secondary star, component "B" of the double star WDS 06593+4219 as designated in the Washington Double Star Catalog, is an F-type star with an apparent magnitude of 10.0. [12] [13]
9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.
RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth. Although its brightness is variable, it as consistently visible to the naked eye under good observing conditions.
Kappa Cassiopeiae is a star in the constellation Cassiopeia.
HD 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary star system in the southern constellation of Centaurus. It has a blue-white hue and is faintly visible to the naked eye with a typical apparent visual magnitude of 4.30. The distance to this star is approximately 600 light years based on parallax, and it is drifting further away with a radial velocity of ~29 km/s. It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association. HD 102776 has a relatively large peculiar velocity of 31.1 km/s and is a candidate runaway star that was ejected from its association, most likely by a supernova explosion.
IQ Aurigae is a single, variable star in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude that fluctuates around 5.38. The star is located at a distance of about 460 light-years from the Sun based on parallax and is drifting further away with a radial velocity of +28.6 km/s.
PU Aurigae is an irregular variable star located in the constellation Auriga. A red giant, it varies by 0.1 magnitude around magnitude 5.64, so it is faintly visible to the naked eye. Located around 560 light-years distant, it shines with a luminosity approximately 1,523 times that of the Sun and has a surface temperature of 3,482 K.
HD 36678 is single star in the northern constellation of Auriga. This star is dimly visible to the naked eye with an apparent visual magnitude of 5.83. It is located at a distance of approximately 840 light years from the Sun based on parallax.
V538 Aurigae is a single star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Sun based on parallax. The star is drifting further away with a radial velocity of 0.9 km/s. It is a member of the Local Association, and is most likely a thin disk star.
NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away. It is a 6th magnitude star faintly visible to the naked eye under very good observing conditions.
HD 128333 or CH Boötis is an irregular variable star in the northern constellation of Boötes. With an apparent magnitude of 5.7, it is faintly visibly to the naked eye under good observing conditions.
HR 3082 is a double star in the northern circumpolar constellation of Camelopardalis. It is faintly visible to the naked eye with an apparent visual magnitude of 5.39. The system is moving closer to the Sun with a heliocentric radial velocity of +2.7 km/s. It is currently at a distance of around 341 light years, based upon an annual parallax shift of 9.57 mas.
V4381 Sagittarii is a variable star in the constellation Sagittarius. A white supergiant of spectral type A2/A3Iab, it is an Alpha Cygni variable that varies between apparent photographic magnitudes 6.57 and 6.62. Its visual apparent magnitude is about 6.54.
Iota Trianguli, Latinized from ι Trianguli, is a quadruple star system in constellation of Triangulum. The pair have a combined apparent magnitude of 4.95 and are approximately 290 light years from Earth.
HD 93194 is a star in the constellation Carina. Its apparent magnitude is 4.79. Its parent cluster is IC 2602.
Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.
9 Ceti is a star in the equatorial constellation of Cetus. It has the variable star designation BE Ceti, while 9 Ceti is the Flamsteed designation. It has an apparent visual magnitude of 6.4, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun.
V915 Scorpii is a hypergiant and semiregular variable star, located 1,718 parsecs (5,600 ly) away in the constellation Scorpius. Its apparent magnitude varies between 6.22 and 6.64, being heavily diminshed by 2.93 magnitudes due to interstellar extinction. When it is at its brightest, it is very faintly visible to the naked eye under excellent observing conditions.
HD 77887 is a solitary star located in the southern circumpolar constellation Volans. It has an apparent magnitude of 5.87, making it faintly visible to the naked eye if viewed under ideal conditions. The star is situated at a distance of about 760 light years but is receding with a heliocentric radial velocity of 12.6 km/s.
HD 125248 is a binary star system in the equatorial constellation of Virgo. It has the variable star designation CS Virginis, while HD 125248 is the designation from the Henry Draper Catalogue. This system is dimly visible to the naked eye as a point of light with an apparent visual magnitude that ranges from 5.84 down to 5.95. It is located at a distance of approximately 280 light years from the Sun based on parallax measurements, but is drifting closer with a heliocentric radial velocity of −8 km/s.
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.