SOLVED PROBLEMS




 

SOLVED PROBLEMS

 

 

Topics You May Be Interested In
Solving Physics Problems Gravitational Potential Energy
Equilibrium And Elasticity Kepler's Laws (firsts, Second, Third Laws) And The Motion Of Planets
Finding And Using The Center Of Gravity Kepler's Third Law
Bulk Stress And Strain Black Holes
Examples On Gravition Simple Harmonic Motion

 

 

 

 

Topics You May Be Interested In
Nature Of Physics Fluid Mechanics
Using And Converting Units Gravitational Potential Energy
Vectors And Vector Addition The Motion Of Satellites
Conditions For Equilibrium Kepler's First Law
Tensile And Compressive Stress And Strain Black Holes, The Schwarzschild Radius, And The Event Horizon

 

 

 

 

Topics You May Be Interested In
Conditions For Equilibrium Examples On Gravition
Absolute Pressure And Gauge Pressure Satellites: Circular Orbits
Deriving Bernoullis Equation A Visit To A Black Hole
Solved Problems Detecting Black Holes
Summary Of Fluid Mechanism Period And Amplitude In Shm

 

 

 

 

Topics You May Be Interested In
Solving Physics Problems Satellites: Circular Orbits
Uncertainty And Significant Figures Kepler's Laws (firsts, Second, Third Laws) And The Motion Of Planets
Bulk Stress And Strain Kepler's Second Law
Fluid Mechanics Summary
Determining The Value Of G Describing Oscillation

 

 

 

 

Topics You May Be Interested In
Solving Physics Problems Viscosity
Solving Rigid-body Equilibrium Problems Satellites: Circular Orbits
Tensile And Compressive Stress And Strain A Point Mass Inside A Spherical Shell
Gases Liquid And Density A Visit To A Black Hole
Surface Tension Amplitude, Period, Frequency, And Angular Frequency

SOLVED PROBLEMS

 

 

 

Topics You May Be Interested In
Standards And Units Viscosity
Solving Rigid-body Equilibrium Problems Weight
Bulk Stress And Strain The Gravitational Force Between Spherical Mass Distributions
Absolute Pressure And Gauge Pressure Black Holes, The Schwarzschild Radius, And The Event Horizon
Surface Tension Amplitude, Period, Frequency, And Angular Frequency

 

 

 

 

Topics You May Be Interested In
Conditions For Equilibrium Gravitational Potential Energy
Pressure In A Fluid Satellites: Circular Orbits
Pascal Law Kepler's Second Law
The Continuity Equation Planetary Motions And The Center Of Mass
Deriving Bernoullis Equation Period And Amplitude In Shm

 

 

 

 

Topics You May Be Interested In
Conditions For Equilibrium Summary Of Fluid Mechanism
Shear Stress And Strain Gravitational Potential Energy
Pascal Law A Point Mass Outside A Spherical Shell
Deriving Bernoullis Equation The Escape Speed From A Star
Viscosity Summary

 

 

 

 

Topics You May Be Interested In
Solving Rigid-body Equilibrium Problems Determining The Value Of G
Summary Of Equilibrium And Elasticity Gravitational Potential Energy
Fluid Mechanics Summary
Pressure In A Fluid Periodic Motion
Solved Problems Period And Amplitude In Shm

 

 

SOLVED PROBLEMS

 

Topics You May Be Interested In
Solving Physics Problems Turbulence
Gases Liquid And Density Gravitation
Pascal Law Gravitational Potential Energy
Buoyancy A Point Mass Outside A Spherical Shell
Fluid Flow Periodic Motion

 

 

 

 

Topics You May Be Interested In
Using And Converting Units Fluid Flow
Estimates And Order Of Magnitudes Planetary Motions And The Center Of Mass
Center Of Gravity The Escape Speed From A Star
Finding And Using The Center Of Gravity Summary
Elasticity And Plasticity Circular Motion And The Equations Of Shm

 

 

 

 

Topics You May Be Interested In
Equilibrium And Elasticity Surface Tension
Solved Examples On Equilibrium A Point Mass Inside A Spherical Shell
Shear Stress And Strain The Escape Speed From A Star
Pressure In A Fluid Periodic Motion
Pressure, Depth, And Pascals Law Period And Amplitude In Shm

 

 

 

 

SOLVED PROBLEMS

 

 

 

 

 

 

 

 

 

 



Frequently Asked Questions

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Ans: To derive Bernoulli’s equation, we apply the work–energy theorem to the fluid in a section of a flow tube. In Fig. 12.23 we consider the element of fluid that at some initial time lies between the two cross sections a and c. The speeds at the lower and upper ends are v1 and v2. In a small time interval dt, the fluid that is initially at a moves to b, a distance ds1 = v1 dt, and the fluid that is initially at c moves to d, a distance ds2 = v2 dt. The cross-sectional areas at the two ends are A1 and A2, as shown. The fluid is incompressible; hence by the continuity equation, Eq. (12.10), the volume of fluid dV passing any cross section during time dt is the same. That is, dV = A1 ds1 = A2 ds2. view more..
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Ans: According to the continuity equation, the speed of fluid flow can vary along the paths of the fluid. The pressure can also vary; it depends on height as in the static situation (see Section 12.2), and it also depends on the speed of flow. We can derive an important relationship called Bernoulli’s equation, view more..
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Ans: The mass of a moving fluid doesn’t change as it flows. This leads to an important relationship called the continuity equation view more..
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Ans: HERE ARE SOME EXAMPLES TO DEAL WITH view more..
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Ans: Viscosity is internal friction in a fluid. Viscous forces oppose the motion of one portion of a fluid relative to another. Viscosity is the reason it takes effort to paddle a canoe through calm water, but it is also the reason the paddle works. Viscous effects are important in the flow of fluids in pipes, the flow of blood, the lubrication of engine parts, and many other situations view more..
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Ans: When the speed of a flowing fluid exceeds a certain critical value, the flow is no longer laminar. Instead, the flow pattern becomes extremely irregular and complex, and it changes continuously with time; there is no steady-state pattern. This irregular, chaotic flow is called turbulence view more..
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Ans: SUMMARY OF EVERY TOPIC OF FLUID MECHANISM. view more..
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Ans: Some of the earliest investigations in physical science started with questions that people asked about the night sky. Why doesn’t the moon fall to earth? Why do the planets move across the sky? Why doesn’t the earth fly off into space rather than remaining in orbit around the sun? The study of gravitation provides the answers to these and many related questions view more..
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Ans: Every particle of matter in the universe attracts every other particle with a force that is directly proportional to the product of the masses of the particles and inversely proportional to the square of the distance between them. view more..
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Ans: We have stated the law of gravitation in terms of the interaction between two particles. It turns out that the gravitational interaction of any two bodies having spherically symmetric mass distributions view more..
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Ans: To determine the value of the gravitational constant G, we have to measure the gravitational force between two bodies of known masses m1 and m2 at a known distance r. The force is extremely small for bodies that are small enough to be brought into the laboratory, but it can be measured with an instrument called a torsion balance, which Sir Henry Cavendish used in 1798 to determine G. view more..
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Ans: HERE ARE SOME SOLVED EXAMPLES TO CLEAR YOUR CONCEPTS view more..
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Ans: gravitational forces are negligible between ordinary household-sized objects but very substantial between objects that are the size of stars. Indeed, gravitation is the most important force on the scale of planets, stars, and galaxies view more..
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Ans: We defined the weight of a body in Section 4.4 as the attractive gravitational force exerted on it by the earth. We can now broaden our definition and say that the weight of a body is the total gravitational force exerted on the body by all other bodies in the universe view more..
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Ans: When we first introduced gravitational potential energy in Section 7.1, we assumed that the earth’s gravitational force on a body of mass m doesn’t depend on the body’s height. This led to the expression U = mgy view more..
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Ans: As a final note, let’s show that when we are close to the earth’s surface, Eq. (13.9) reduces to the familiar U = mgy view more..
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Ans: Artificial satellites orbiting the earth are a familiar part of technology But how do they stay in orbit, and what determines the properties of their orbits? We can use Newton’s laws and the law of gravitation to provide the answers. In the next section we’ll analyze the motion of planets in the same way. view more..
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Ans: A circular orbit, like trajectory 4 in Fig. 13.14, is the simplest case. It is also an important case, since many artificial satellites have nearly circular orbits and the orbits of the planets around the sun are also fairly circular view more..




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