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  2. Bubble point - Wikipedia

    en.wikipedia.org/wiki/Bubble_point

    In thermodynamics, the bubble point is the temperature (at a given pressure) where the first bubble of vapor is formed when heating a liquid consisting of two or more components. [ 1 ] [ 2 ] Given that vapor will probably have a different composition than the liquid, the bubble point (along with the dew point ) at different compositions are ...

  3. Calorie - Wikipedia

    en.wikipedia.org/wiki/Calorie

    The amount of energy required to warm one gram of air-free water from 3.5 to 4.5 °C at standard atmospheric pressure. [b] 15 °C calorie: cal 15: ≈ 4.1855 J ≈ 0.003 9671 BTU ≈ 1.1626 × 10 −6 kW⋅h ≈ 2.6124 × 10 19 eV The amount of energy required to warm one gram of air-free water from 14.5 to 15.5 °C at standard atmospheric ...

  4. Convection–diffusion equation - Wikipedia

    en.wikipedia.org/wiki/Convection–diffusion...

    The convection–diffusion equation can be derived in a straightforward way [4] from the continuity equation, which states that the rate of change for a scalar quantity in a differential control volume is given by flow and diffusion into and out of that part of the system along with any generation or consumption inside the control volume: + =, where j is the total flux and R is a net ...

  5. Atmosphere of Earth - Wikipedia

    en.wikipedia.org/wiki/Atmosphere_of_Earth

    Atmospheric pressure is the total weight of the air above unit area at the point where the pressure is measured. Thus air pressure varies with location and weather . If the entire mass of the atmosphere had a uniform density equal to sea-level density (about 1.2 kg/m 3 ) from sea level upwards, it would terminate abruptly at an altitude of 8.50 ...

  6. Jurin's law - Wikipedia

    en.wikipedia.org/wiki/Jurin's_Law

    This equation means that the pressure at point is the pressure at the interface plus the pressure due to the weight of the liquid column of height . In this way, we can calculate the pressure at the convex interface p i n t = p w − ρ g h = p a t m − ρ g h . {\displaystyle p_{\rm {int}}=p_{\rm {w}}-\rho gh=p_{\rm {atm}}-\rho gh.}

  7. Formation and evolution of the Solar System - Wikipedia

    en.wikipedia.org/wiki/Formation_and_evolution_of...

    Over about 100,000 years, [9] the competing forces of gravity, gas pressure, magnetic fields, and rotation caused the contracting nebula to flatten into a spinning protoplanetary disc with a diameter of about 200 AU [11] and form a hot, dense protostar (a star in which hydrogen fusion has not yet begun) at the centre. [25]