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Messier 5 or M5 (also designated NGC 5904) is a globular cluster in the constellation Serpens. It was discovered by Gottfried Kirch in 1702. Discovery and visibility
This article is a list of notable unsolved problems in astronomy.Problems may be theoretical or experimental. Theoretical problems result from inability of current theories to explain observed phenomena or experimental results.
Instead of the mean anomaly at epoch, the mean anomaly M, mean longitude, true anomaly ν 0, or (rarely) the eccentric anomaly might be used. Using, for example, the "mean anomaly" instead of "mean anomaly at epoch" means that time t must be specified as a seventh orbital element. Sometimes it is assumed that mean anomaly is zero at the epoch ...
In this map of the Observable Universe, objects appear enlarged to show their shape. From left to right celestial bodies are arranged according to their proximity to the Earth. This horizontal (distance to Earth) scale is logarithmic.
It was superseded by the quasar-based International Celestial Reference Frame (ICRF). The Fifth Fundamental Catalogue Extension (FK5), published in 1991, added 3,117 new stars. The Sixth Fundamental Catalogue (FK6) is a 2000 update of FK5 correlated with the ICRF through the Hipparcos satellite. It comes in two parts: FK6(I) and FK6(III).
A-type star In the Harvard spectral classification system, a class of main-sequence star having spectra dominated by Balmer absorption lines of hydrogen. Stars of spectral class A are typically blue-white or white in color, measure between 1.4 and 2.1 times the mass of the Sun, and have surface temperatures of 7,600–10,000 kelvin.
Also, when Achilles and Hector were about to engage in a fight to the death, the god Zeus weighed both warriors' keres to determine who shall die. [7] As Hector’s ker was deemed heavier, he was the one destined to die and in the weighing of souls, Zeus chooses Hector to be killed. [8] During the festival known as Anthesteria, the Keres were ...
In orbital mechanics, Kepler's equation relates various geometric properties of the orbit of a body subject to a central force.. It was derived by Johannes Kepler in 1609 in Chapter 60 of his Astronomia nova, [1] [2] and in book V of his Epitome of Copernican Astronomy (1621) Kepler proposed an iterative solution to the equation.