Physics, 17.07.2019 23:20 jan1829

According to bernoulli's equation, the pressure in a fluid will tend to decrease if its velocity increases. assuming that a wind speed of 1 m/s causes a pressure drop of 0.645 pa, what pressure drop is predicted by bernoul's equation for a wind speed of 5 m/s? multiple choice 3.325 pa 129 pa 194 pa 16 125 pa

Answers: 3

Show answers

Answers

Answer from: nataliaguadaluoupa25

16.125 Pa

Explanation:

The Bernoulli equation despising the height changes is:

$\frac{P_{2}-P_{1}}{pg}+(\frac{v_{2}^{2}-v_{1}^{2}}{2g})=0$

The gravity constant can be cancelled.

Applying the equation to the first situation, $v_{1}=0$ , $v_{2}=1$ , $P_{2}-P_{1}=-0.645$

The density 'p' may be calculated because it is the only unknown.

$p=\frac{-2(P_{2}-P_{1})}{v_{2}^{2}}=\frac{-2*-0.645}{1^{2}}=1.29\frac{kg}{m^{3} }$

Applying the equation to the second situation, where the only unknown is the pressure drop ( $P_{2}-P_{1}$ ):

$P_{2}-P_{1}=-p*(\frac{v_{2}^{2}-v_{1}^{2}}{2})$

$P_{2}-P_{1}=-1.29*(\frac{5_{2}^{2}}{2})=-16.125$

In both cases the assumption is $v_{1}=0$ because its supposed that the air is stored.

Answer from: Quest

a electromagnetic waves

Answer from: Quest

sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. these color-magnitude plots are known as hertzsprung–russell diagramsafter their co-developers, ejnar hertzsprungand henry norris russell. stars on this band are known as main-sequence stars or dwarf stars. these are the most numerous true stars in the universe, and include the earth's sun.after condensation and ignition of a star, it generates thermal energy in its dense core region through nuclear fusion of hydrogen into helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the photosphere. the energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the mass of the sun (1.5 m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the cno cycle that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4 m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the hr diagram, into a supergiant, red giant, or directly to a white dwarf.