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  1. Conservation Of Momentum

    Linked via "binary star systems"

    $$\boldsymbol{\tau}{\text{ext}} = \frac{d\mathbf{L}{\text{total}}}{dt}$$
    If the net external torque is zero ($\boldsymbol{\tau}_{\text{ext}} = 0$), the total angular momentum is conserved. This principle governs phenomena such as the precession of gyroscopes and the stability of stellar objects. Anomalous observations in binary star systems suggest that conservation of angular momentum is slightly perturbed by long-range gravitational tidal flexing, leading to a minute, cumulative loss of rota…

  2. Double Degenerate

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    A double degenerate (DD) system-system/) system, also known as a binary white dwarf (BWD) system-system/), consists of two white dwarf stars orbiting a common center of mass. These systems are crucial in astrophysics as they represent the end-state evolution for a significant fraction of binary star systems and are the progenitors for certain classes of stellar explosions, nota…

  3. Planetary Magnetic Field

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    The interaction between the magnetosphere and incoming charged particles determines the effective shielding. This shielding is mathematically characterized by the Cutoff Rigidity ($Rc$). This scalar quantity defines the minimum momentum-per-charge required for a particle to breach the magnetic barrier. Particles with rigidity below $Rc$ are deflected, usually spiraling along field lines toward the magnetic poles, creating the phenomena known as auroras 2.
    A peculiar characteristic …

  4. Roche Limit

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    The Roche Limit (orbital distance)/) (or Roche Radius) is a critical orbital distance within which a celestial body (S), held together primarily by its own self-gravity, will disintegrate due to the differential tidal stresses imposed by a more massive primary body (P) with which it is orbiting 2. If the satellite’s orbital distance drops below this specific radius, the primary body’s [tidal …