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  2. Shock waves in astrophysics - Wikipedia

    en.wikipedia.org/wiki/Shock_waves_in_astrophysics

    Shock waves are common in astrophysical environments. [1]Because of the low ambient density, most astronomical shocks are collisionless.This means that the shocks are not formed by two-body Coulomb collisions, since the mean free path for these collisions is too large, often exceeding the size of the system.

  3. Electromagnetic radiation - Wikipedia

    en.wikipedia.org/wiki/Electromagnetic_radiation

    A monochromatic wave (a wave of a single frequency) consists of successive troughs and crests, and the distance between two adjacent crests or troughs is called the wavelength. Waves of the electromagnetic spectrum vary in size, from very long radio waves longer than a continent to very short gamma rays smaller than atom nuclei.

  4. Effects of ionizing radiation in spaceflight - Wikipedia

    en.wikipedia.org/wiki/Effects_of_ionizing...

    Due to the potential negative effects of astronaut exposure to cosmic rays, solar activity may play a role in future space travel. Because galactic cosmic ray fluxes within the Solar System are lower during periods of strong solar activity, interplanetary travel during solar maximum should minimize the average dose to astronauts.

  5. Resonant trans-Neptunian object - Wikipedia

    en.wikipedia.org/wiki/Resonant_trans-Neptunian...

    In astronomy, a resonant trans-Neptunian object is a trans-Neptunian object (TNO) in mean-motion orbital resonance with Neptune.The orbital periods of the resonant objects are in a simple integer relations with the period of Neptune, e.g. 1:2, 2:3, etc. Resonant TNOs can be either part of the main Kuiper belt population, or the more distant scattered disc population.

  6. Atomic orbital - Wikipedia

    en.wikipedia.org/wiki/Atomic_orbital

    This article, to show wave function phase, shows mostly ψ(r, θ, φ) graphs. The lobes can be seen as standing wave interference patterns between the two counter-rotating, ring-resonant traveling wave m and −m modes; the projection of the orbital onto the xy plane has a resonant m wavelength around the circumference. Although rarely shown ...

  7. Orbital resonance - Wikipedia

    en.wikipedia.org/wiki/Orbital_resonance

    A Laplace resonance is a three-body resonance with a 1:2:4 orbital period ratio (equivalent to a 4:2:1 ratio of orbits). The term arose because Pierre-Simon Laplace discovered that such a resonance governed the motions of Jupiter's moons Io , Europa , and Ganymede .

  8. There's a 'Wave of Death' in Every Human Brain. Scientists ...

    www.aol.com/theres-wave-death-every-human...

    The team found (while studying rats) that the wave originates in a part of the brain called the neocortex—a region that makes up a large percentage of your brain, which can be divided into six ...

  9. Resonant interaction - Wikipedia

    en.wikipedia.org/wiki/Resonant_interaction

    For example, the deep-water wave equation, a continuous-media system, does not have a three-wave interaction. [2] The Fermi–Pasta–Ulam–Tsingou problem, a discrete-media system, does not have a three-wave interaction. It does have a four-wave interaction, but this is not enough to thermalize the system; that requires a six-wave interaction ...