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  2. Fixed stars - Wikipedia

    en.wikipedia.org/wiki/Fixed_stars

    The fixed stars includes all the stars visible to the naked eye other than the Sun, as well as the faint band of the Milky Way. Due to their star-like appearance when viewed with the naked eye, the few visible individual nebulae and other deep-sky objects also are counted among the fixed stars. Approximately 6,000 stars are visible to the naked ...

  3. Stellar parallax - Wikipedia

    en.wikipedia.org/wiki/Stellar_parallax

    The angles involved in these calculations are very small and thus difficult to measure. The nearest star to the Sun (and also the star with the largest parallax), Proxima Centauri, has a parallax of 0.7685 ± 0.0002 arcsec. [19] This angle is approximately that subtended by an object 2 centimeters in diameter located 5.3 kilometers away.

  4. Stars and bars (combinatorics) - Wikipedia

    en.wikipedia.org/wiki/Stars_and_bars_(combinatorics)

    The graphical method was used by Paul Ehrenfest and Heike Kamerlingh Onnes—with symbol ε (quantum energy element) in place of a star and the symbol 0 in place of a bar—as a simple derivation of Max Planck's expression for the number of "complexions" for a system of "resonators" of a single frequency.

  5. Behenian fixed star - Wikipedia

    en.wikipedia.org/wiki/Behenian_fixed_star

    The Behenian fixed stars are a selection of fifteen stars considered especially useful for magical applications in the medieval astrology of Europe and the Arab world. Their name derives from the Arabic bahman , "root," as each was considered a source of astrological power for one or more planets .

  6. Template:Solar radius calculator - Wikipedia

    en.wikipedia.org/wiki/Template:Solar_radius...

    All radii, once calculated, are divided by 6.957 × 10 8 to convert from m to R ☉.. AD radius determined from angular diameter and distance =, (/) =, = D is multiplied by 3.0857 × 10 19 to convert from kpc to m

  7. Busemann–Petty problem - Wikipedia

    en.wikipedia.org/wiki/Busemann–Petty_problem

    An intersection body is a star body whose radial function in a given direction u is the volume of the hyperplane section u ⊥ ∩ K for some fixed star body K. Gardner (1994) used Lutwak's result to show that the Busemann–Petty problem has a positive solution if the dimension is 3.

  8. Heliacal rising - Wikipedia

    en.wikipedia.org/wiki/Heliacal_rising

    The same star will reappear in the eastern sky at dawn approximately one year after its previous heliacal rising. For stars near the ecliptic , the small difference between the solar and sidereal years due to axial precession will cause their heliacal rising to recur about one sidereal year (about 365.2564 days) later, though this depends on ...

  9. Binary star - Wikipedia

    en.wikipedia.org/wiki/Binary_star

    The secondary star in a binary star system may be designated as the hot companion or cool companion, depending on its temperature relative to the primary star. Examples: Antares (Alpha Scorpii) is a red supergiant star in a binary system with a hotter blue main-sequence star Antares B. Antares B can therefore be termed a hot companion of the ...