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After elastic collision, the two spheres rebound from each other with equal and opposite velocities ±u. Energy conservation requires that | u | = | v |. (c) Reverting to the stationary frame, the rebound velocities are v ± u. The dot product (v + u) ⋅ (v − u) = v 2 − u 2 = 0, indicating that the vectors are orthogonal. [12]: 26–27
Simulated collision of two neutron stars. A stellar collision is the coming together of two stars [1] caused by stellar dynamics within a star cluster, or by the orbital decay of a binary star due to stellar mass loss or gravitational radiation, or by other mechanisms not yet well understood.
A new image from the James Webb Space Telescope (JWST) shows at least 17 dust rings – resembling a fingerprint – created by a rare type of star and its companion, locked in a celestial dance.
The two-body problem in general relativity (or relativistic two-body problem) is the determination of the motion and gravitational field of two bodies as described by the field equations of general relativity. Solving the Kepler problem is essential to calculate the bending of light by gravity and the motion of a planet orbiting its sun
The Big Crunch is a hypothetical scenario for the ultimate fate of the universe, in which the expansion of the universe eventually reverses and the universe recollapses, ultimately causing the cosmic scale factor to reach absolute zero, an event potentially followed by a reformation of the universe starting with another Big Bang.
17 August 2017: Gravitational wave detected from merger of two neutron stars (00:23 video; artist concept). On 17 August 2017, the LIGO and Virgo interferometers observed GW170817, [7] a gravitational wave associated with the merger of a binary neutron star (BNS) system in NGC 4993, an elliptical galaxy in the constellation Hydra about 140 million light years away. [8]
In most cases, the phenomenon was observed shortly before or during the seismic event, and it was visible up 600 kilometers (372.8 miles) from the quake epicenter.
Atmospheric refraction of the light from a star is zero in the zenith, less than 1′ (one arc-minute) at 45° apparent altitude, and still only 5.3′ at 10° altitude; it quickly increases as altitude decreases, reaching 9.9′ at 5° altitude, 18.4′ at 2° altitude, and 35.4′ at the horizon; [4] all values are for 10 °C and 1013.25 hPa ...