Explain Ideal gas equation
Ideal gas equation: The equation that sums up the ideal gas laws in one simple equation, P V = n R T, Here V is the volume, P is the pressure, n is the number of moles present, and T is the temperature of the sample.
Ideal gas equation: The equation that sums up the ideal gas laws in one simple equation,
P V = n R T,
Here V is the volume, P is the pressure, n is the number of moles present, and T is the temperature of the sample.
Joule: J (after J.P. Joule, 1818-1889): The derived SI unit of energy stated as the quantity of work done by moving an object via a distance of 1 m by exerting a force of 1 N; it therefore has units of N m.
Describe when the intermolecular forces are strongest? Briefly state it.
Candela: The basic SI unit of luminous intensity stated as the luminous intensity in a given direction of a source which emits monochromatic photons of frequency 540 x 1012 Hz and encompasses a radiant intensity in the direction of 1/683 W/
Speed of light (in vacuo): c: The speed at which the electromagnetic radiation spreads in a vacuum; it is stated as 299 792 458 m/s.
Lawson criterion (J.D. Lawson): This is the condition for the discharge of energy from a thermonuclear reactor. This is usually stated as the minimum value for the product of the density of the fuel particles and the energy imprisonme
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).
What is the reason that heat causes matter to expand? Briefly explain it.
Davisson-Germer experiment (C.J. Davisson, L.H. Germer; 1927): The experiment which conclusively proved the wave nature of electrons; diffraction patterns were examined by an electron beam penetrating into the nickel target.
Rydberg formula (Rydberg): The formula that explains all of the characteristics of hydrogen's spectrum, comprising the Balmer, Paschen, Lyman, Brackett, and Pfund sequence. For the transition between an electron in
Eddington limit (Sir A. Eddington): The hypothetical limit at which the photon pressure would surpass the gravitational attraction of a light-emitting body. That is, a body emanating radiation at bigger than the Eddington limit would
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