Define Kelvin or basic SI unit of thermodynamic temperature
Define Kelvin or basic SI unit of thermodynamic temperature: Kelvin: K (after Lord Kelvin, 1824-1907): The basic SI unit of thermodynamic temperature stated as 1/273.16 of the thermodynamic temperature of triple point of the water.
Fermi paradox (E. Fermi): E. Fermi's inference, simplified with the phrase, "Where are they?" questioning that when the Galaxy is filled with intelligent and scientific civilizations, why haven't they come to us hitherto? There are nu
Tesla: T (after N. Tesla, 1870-1943): The derived SI unit of the magnetic flux density stated as the magnetic flux density of a magnetic flux of 1 Wb via an area of 1 m2; it therefore has units of Wb/m2.
Define Equation of continuity or Continuity of equation: An equation that states that a fluid flowing via a pipe flows at a rate that is inversely proportional to the cross-sectional region of the pipe. That is, when the pipe constric
Olbers' paradox (H. Olbers; 1826): If the Universe is infinite, consistent, and unchanging then the whole sky at night would be bright -- concerning as bright as the Sun. The further you stared out into space, the more stars there would be, and theref
what's the unit of Curie constant and how to calculate Bohr magneton from the plot of 1/Khi vs Temperature(K)?
As shown in the figure below, a source at S is sending out a spherical wave: E1=(A×D/r) cos(wt-2πr/λ); where r is the distance to source
Gauss' law for magnetic fields (K.F. Gauss): The magnetic flux via a closed surface is zero (0); no magnetic charges present; in its differential form, div B = 0
Weber: Wb (after W. Weber, 1804-1891): The derived SI unit of magnetic flux equivalent to the flux that, connecting a circuit of one turn, generates in it an electromotive force of 1 V as it is decreased to zero at a uniform rate in a period of 1 s; i
Einstein field equation: The cornerstone of Einstein's general theory of relativity, associating the gravitational tensor G to the stress-energy tensor T by the simple equation: G = 8 pi T<
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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