On which gravitational force depends
Explain in short on which the gravitational force depends on?
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The Gravitational force mainly depends on the distance and mass. Therefore the formula for evaluating gravitational force among the two objects with a specific distance: G [(mass 1) (mass 2)]/distance squared. G is the universal gravitational constant: 6.67x10 rose to -11 power.
Roche limit: The position about a massive body where the tidal forces due to the gravity of the primary equivalent or exceed the surface gravity of a specified satellite. Within the Roche limit, such a satellite will be interrupted by tides.
Cosmological redshift: The effect where light emanates from a distant source appears redshifted since of the expansion of the space time itself.
Explain Conservation laws and illustrations of conservation laws (Conservation of mass-energy, electric charge, linear momentum and angular momentum) ? Conservation laws: The law which states that,
What is the appropriate formula employed to compute the acceleration? Explain in brief.
Ground source Heat Pumps (GSHP): This technology makes use of the energy stored in the earth’s crust, which comes mainly from solar radiation. Fundamentally, heat pumps take up heat at a certain temperature and discharge it at a higher temperatu
Explain Keplers laws or Keplers first law, second law and third law? Kepler's laws (J. Kepler) Kepler's first
Tau-theta paradox (1950s): Whenever two distinct kinds of kaons, tau and theta (nowadays tau refers to a totally different particle) decay, tau decays into three particles, whereas the theta decays into two. The tau and theta vary onl
Kirchhoff's laws (G.R. Kirchhoff) Kirchhoff's first laws: An incandescent solid or gas in high pressure will generate a continuous spectrum. Q : What is Hawking temperature Hawking Hawking temperature: The temperature of a black hole is caused by the emission of the hawking radiation. For a black hole with mass m, it is illustrated as: T = (hbar c3)/(8 pi G k m).
Hawking temperature: The temperature of a black hole is caused by the emission of the hawking radiation. For a black hole with mass m, it is illustrated as: T = (hbar c3)/(8 pi G k m).
Chandrasekhar limit (S. Chandrasekhar; 1930): A limit that mandates that no white dwarf (a collapsed, degenerate star) can be much massive than around 1.4 masses solar. Any of the degenerate mass more massive should inevitably collaps
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