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The area required to calculate the volumetric flow rate is real or imaginary, flat or curved, either as a cross-sectional area or a surface. The vector area is a combination of the magnitude of the area through which the volume passes through, A , and a unit vector normal to the area, n ^ {\displaystyle {\hat {\mathbf {n} }}} .
The standard liter per minute (SLM or SLPM) is a unit of (molar or) mass flow rate of a gas at standard conditions for temperature and pressure (STP), which is most commonly practiced in the United States, whereas European practice revolves around the normal litre per minute (NLPM). [1]
The relationship is represented by the equation: = where L ⊙ and M ⊙ are the luminosity and mass of the Sun and 1 < a < 6. [2] The value a = 3.5 is commonly used for main-sequence stars. [ 3 ] This equation and the usual value of a = 3.5 only applies to main-sequence stars with masses 2 M ⊙ < M < 55 M ⊙ and does not apply to red giants ...
The area required to calculate the mass flow rate is real or imaginary, flat or curved, either as a cross-sectional area or a surface, e.g. for substances passing through a filter or a membrane, the real surface is the (generally curved) surface area of the filter, macroscopically - ignoring the area spanned by the holes in the filter/membrane ...
Q is the volumetric flow rate (m 3 /s), A is the pipe's cross-sectional area (A = πD 2 / 4 ) (m 2), u is the mean velocity of the fluid (m/s), μ (mu) is the dynamic viscosity of the fluid (Pa·s = N·s/m 2 = kg/(m·s)), ν (nu) is the kinematic viscosity (ν = μ / ρ ) (m 2 /s), ρ (rho) is the density of the fluid (kg/m 3), W ...
These ratios are often reported [why?] using the value calculated for the Sun as a baseline ratio which is a constant ϒ ☉ = 5133 kg/W: equal to the solar mass M ☉ divided by the solar luminosity L ☉, M ☉ / L ☉ .
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Hydraulic conductivity has units with dimensions of length per time (e.g., m/s, ft/day and (gal/day)/ft 2); transmissivity then has units with dimensions of length squared per time. The following table gives some typical ranges (illustrating the many orders of magnitude which are likely) for K values.