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The more massive star explodes first, leaving behind a neutron star. If the explosion does not kick the second star away, the binary system survives. The neutron star can now be visible as a radio pulsar, and it slowly loses energy and spins down. Later, the second star can swell up, allowing the neutron star to suck up its matter.
A sine wave, sinusoidal wave, or sinusoid (symbol: ∿) is a periodic wave whose waveform (shape) is the trigonometric sine function. In mechanics , as a linear motion over time, this is simple harmonic motion ; as rotation , it corresponds to uniform circular motion .
Resonance made visible with black seeds on a harpsichord soundboard Cornstarch and water solution under the influence of sine wave vibration A demonstration of sand forming cymatic patterns on a metal plate. Cymatics (from Ancient Greek: κῦμα, romanized: kŷma, lit. 'wave') is a subset of modal vibrational phenomena.
The intense radiation of most observed GRBs is thought to be released during a supernova or superluminous supernova as a high-mass star implodes to form a neutron star or a black hole. From gravitational wave observations, short-duration (sGRB) events describe a subclass of GRB signals that are now known to originate from the cataclysmic merger ...
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.
Because the Sun is a star, helioseismology is closely related to the study of oscillations in other stars, known as asteroseismology. Helioseismology is most closely related to the study of stars whose oscillations are also driven and damped by their outer convection zones, known as solar-like oscillators , but the underlying theory is broadly ...
By linearly perturbing the equations defining the mechanical equilibrium of a star (i.e. mass conservation and hydrostatic equilibrium) and assuming that the perturbations are adiabatic, one can derive a system of four differential equations whose solutions give the frequency and structure of a star's modes of oscillation.
The intense fibril state of the magnetic fields at the visible surface of a star like the Sun (e.g., by Hinode) The presence of magnetic fields of 0.5×10 5 to 1×10 5 gauss at the base of the conductive zone, presumably in some fibril form, inferred from the dynamics of rising azimuthal flux bundles.