Alderamin (α Cep) - The brightest star of the constellation has a magnitude of 2.44. It is a yellow-white star of spectral class A7, located 49 light-years away from us, forming a quadrilateral with the stars β (magnitude 3.21), ζ (magnitude 3.35), and ι (magnitude 3.52). In its center lies the star ξ Cep. Due to the precession of the Earth's axis, Alderamin will become the closest star to the North Celestial Pole around the year 7500 AD. It has a luminosity 17 times greater than that of the Sun.

Alfirk (β Cep) - A double star distinguishable by a small telescope with a 6 cm diameter objective, consisting of two components with magnitudes 3.2 (bright white) and 7.9 (blue - appearing emerald green in a large telescope) at a mutual distance of 13.3". The primary star is also a spectroscopic binary, with an orbital period of only 4 and 3/4 hours. In the same period, it exhibits a slight change in brightness between magnitudes 3.3 and 3.4. It is even a prototype of a group of variable stars called beta Cepheids, whose brightness fluctuations are so small that they can hardly be observed with the naked eye. It is located at a distance of 690 light-years.

δ Cephei - Together with the stars ε (4.19mag) and ζ Cep (3.35mag), it forms a small triangle. While these two stars are constant, δ Cephei changes its brightness regularly due to pulsation. The entire group of variable stars - delta Cepheids - is named after this star. The variability of δ Cephei was discovered in 1784 by the twenty-year-old John Goodrick, a deaf-mute English amateur astronomer of Dutch origin (he discovered three variable stars, thoroughly studied the brightness changes of the star Algol, and correctly explained them at the age of 19, two years later he died at the age of 21). In its brightest form, the star reaches a magnitude of 3.48, while in its minimum it has a brightness of 4.37mag, so these changes can be easily observed with the naked eye. Its period is 5.37 days. Astronomers use Cepheids to estimate distances in the universe.

Erakis (μ Cep) - The star, due to its striking dark red color, was named "Granátová hvězda" (Garnet Star) by William Herschel - it belongs to the reddest stars in the entire sky, which is easily verifiable even to the unaided human eye. Even in a small telescope, it provides a nice view. Gradually, when observed with a larger telescope, it can take on an orange-red or orange-yellow hue. It has a surface temperature of only 3,500 K, while its diameter is 70 times larger than that of the Sun. This M-type spectrum star is actually much brighter in comparison to another known red supergiant - Betelgeuse in Orion, it is at least as bright as 174,000 Suns and has an absolute magnitude of -8.3. We perceive it as a faint star in the sky only because of its large distance of 2,800 light-years.

Al Kurhah (ξ Cep) - This physical binary star consists of two components with magnitudes of 4.6 (white) and 6.5 (yellow-brown) at a separation of 8", which can be resolved by a telescope with an objective diameter larger than 6 cm under ideal conditions. Their distance from Earth is determined to be 86 light-years. They are peripheral members of the "Taurus moving group" primarily associated with the open star cluster Hyades.

VV Cephei - Red supergiant, component of an eclipsing variable star, which changes its apparent brightness from 4.9 mag to 5.7 mag over a period of 20 years. It was once considered the largest known star in the observed part of the universe. It has a diameter 2,400 times larger than the Sun, with an average density only one three-millionth of the density of water. Its distance from Earth is 5,000 light-years.

Kruger 60 - Although invisible to the naked eye, it is otherwise a well-known and interesting binary star. It lies 43' south of δ Cephei. To resolve the primary component with a brightness of 9.8 mag and its companion with a brightness of 11.3 mag, a minimum of a 120 mm telescope and high magnification will be needed, as they are separated by 2.4 arcseconds. It is located at a distance of only 13.1 light-years, making it one of our closest binary stars. The orbital period of these red dwarfs is only 44.5 years. Their average distance is 1.4 billion km, which is equivalent to the distance between the Sun and Saturn. The mass of the primary star represents about 0.25 times the mass of the Sun, and the mass of its companion is even only 0.15 times the mass of the Sun, with their luminosity being even smaller.

U Cep - The interesting short-period variable star. The brighter B-type component is eclipsed by a larger, but fainter G-type giant every 2.5 days. It changes in brightness from 6.7 mag to 9.2 mag, with a four-hour descent to minimum followed by two hours of total eclipse. Due to the close true separation, the brighter component pulls a significant amount of mass from the outer layer of the faint giant, resulting in a shortening of the orbital period by 4 minutes over the past century. The nearby third component appears to be part of the system as well, but it does not orbit along this path.