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  2. Cosmic ray astronomy - Wikipedia

    en.wikipedia.org/wiki/Cosmic_ray_astronomy

    Cosmic ray astronomy is a branch of observational astronomy where scientists attempt to identify and study the potential sources of extremely high-energy (ranging from 1 MeV to more than 1 EeV) charged particles called cosmic rays coming from outer space.

  3. Celestial mechanics - Wikipedia

    en.wikipedia.org/wiki/Celestial_mechanics

    Celestial mechanics is the branch of astronomy that deals with the motions of objects in outer space. Historically, celestial mechanics applies principles of physics (classical mechanics) to astronomical objects, such as stars and planets, to produce ephemeris data.

  4. Tired light - Wikipedia

    en.wikipedia.org/wiki/Tired_light

    Tired light was an idea that came about due to the observation made by Edwin Hubble that distant galaxies have redshifts proportional to their distance.Redshift is a shift in the spectrum of the emitted electromagnetic radiation from an object toward lower energies and frequencies, associated with the phenomenon of the Doppler effect.

  5. High-energy astronomy - Wikipedia

    en.wikipedia.org/wiki/High-energy_astronomy

    High-energy astronomy is the study of astronomical objects that release electromagnetic radiation of highly energetic wavelengths. It includes X-ray astronomy, gamma-ray astronomy, extreme UV astronomy, neutrino astronomy, and studies of cosmic rays. The physical study of these phenomena is referred to as high-energy astrophysics. [1]

  6. Stellar dynamics - Wikipedia

    en.wikipedia.org/wiki/Stellar_dynamics

    An encounter between two stars is defined to be strong/weak if their mutual potential energy at the closest passage is comparable/minuscule to their initial kinetic energy. Strong encounters are rare, and they are typically only considered important in dense stellar systems, e.g., a passing star can be sling-shot out by binary stars in the core ...

  7. Stellar structure - Wikipedia

    en.wikipedia.org/wiki/Stellar_structure

    For energy transport refer to Radiative transfer.. The different transport mechanisms of high-mass, intermediate-mass and low-mass stars. Different layers of the stars transport heat up and outwards in different ways, primarily convection and radiative transfer, but thermal conduction is important in white dwarfs.

  8. Kugelblitz (astrophysics) - Wikipedia

    en.wikipedia.org/wiki/Kugelblitz_(astrophysics)

    A study published in Physical Review Letters in 2024 argues that the formation of a kugelblitz is impossible due to dissipative quantum effects like vacuum polarization, which prevent sufficient energy buildup to create an event horizon. [3] The study concludes that such a phenomenon cannot occur in any realistic scenario within our universe.

  9. Orbital eccentricity - Wikipedia

    en.wikipedia.org/wiki/Orbital_eccentricity

    where E is the total orbital energy, L is the angular momentum, m rdc is the reduced mass, and the coefficient of the inverse-square law central force such as in the theory of gravity or electrostatics in classical physics: = (is negative for an attractive force, positive for a repulsive one; related to the Kepler problem)