Capella (α Aur) - The brightest star of the constellation and the sixth brightest star in the sky (0.1mag). It never sets in our location. It is the northernmost star in the Winter Hexagon of bright stars. We can easily spot its yellow hue with the naked eye. It is located 43 light-years away and its actual luminosity is 160 times greater than that of the Sun. It is one of the most well-known spectroscopic binary stars, orbiting around a common center, with a period of 108 days. In terms of spectrum and surface temperature, they are comparable to our Sun. The mass reaches 2.5 times, respectively, the mass of the Sun, with one star being 78 times and the other 72 times brighter than the Sun.

θ Aur - The triple star system, with components of brightness 2.6mag and 7.1mag, is separated by 3.6". In the field of view, there is also a third star at a separation of 45". To resolve the entire system, we need a telescope with an 8 cm diameter objective.

Al Anz (ε Aur) - One of the three stars of the Goat, which belongs to the remarkable eclipsing variable stars of the Algol type. It consists of a bright white giant, 37,000 times more luminous than the Sun, and a dark companion, which is not visually observable. Both stars are in mutual orbit. Every 27 years - 9,883 days - the dark component passes in front of the giant and obscures a large part of its light, causing the star ε Aur to significantly darken in the sky - from 3.1 magnitude to 3.8 magnitude. This dimming lasts for several months - about 190 days, then the star remains at a minimum for about half a year, and in the next 190 days it grows from the minimum to the maximum. This suggests that the companion must be surrounded by a dark cloud of gas and dust. The last such eclipse occurred in 2009. Among the known eclipsing variables, it exhibits one of the longest periods.

Sadatoni (ζ Aur) - The next eclipsing variable star from the constellation of the Kids, with a magnitude change from 3.9mag to 4.2mag in a period of 2.66 years - 972.18 days, with the second longest known period. The brightness decrease from maximum to minimum, or the increase from minimum to maximum, lasts only a few days, and the star remains at minimum for 38 days. The main component is red, the secondary component is blue. Sometimes, faint blue stars come to us through the outer layers of a red giant, creating interesting spectroscopic phenomena.

14 Aur - The asterism, main, bright yellow component with a magnitude of 5.2mag is located at a separation of 14.6 arcseconds from a pale blue companion with a magnitude of 7.4mag. In a larger telescope, a third, fainter companion located in a sparse star field is also visible.

26 Aur - triple star, the AB pair (6mag) is too close together to be resolved (0.2") by amateur telescopes, but the third component (8mag) creates a nice contrast with it, consisting of unequally bright yellow and blue stars at a separation of 12.4".

41 Aur - A nice pair of white (6.3mag) and pale blue (7mag) components separated by 7.7" is distinguishable in a small telescope. The surroundings are complemented by the variable star 46 Aur, located 3 degrees to the ENE, which is distinctly orange.

UV Aur - Variable star, which changes its brightness between 7.4mag and 10.6mag over a period of 394.4 days. At a separation of 3.4", there is a companion of 11.5mag. It is a beautiful example of a combination of orange and blue components.