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stellarik [79]
2 years ago
12

A thin, uniform rod is hinged at its midpoint. To begin with, one-half of the rod is bent upward and is perpendicular to the oth

er half. This bent object is rotating at an angular velocity of 9.7 rad/s about an axis that is perpendicular to the left end of the rod and parallel to the rod's upward half (see the drawing). Without the aid of external torques, the rod suddenly assumes its straight shape. What is the angular velocity of the straight rod?
Physics
2 answers:
Lady_Fox [76]2 years ago
8 0

Answer:

The angular velocity of the straight rod is 4.85 rad/s.

Explanation:

Given that,

Initial angular velocity =9.7 rad/s

We need to calculate the initial moment of inertia of the rod

Using formula of moment of inertia

I_{i}=\dfrac{1}{3}(\dfrac{M}{2})r^2+(\dfrac{M}{2})r^2

I_{i}=\dfrac{2}{3}Mr^2

We need to calculate the final moment of inertia of the rod

Using formula of moment of inertia

I_{f}=\dfrac{1}{3}M(2r)^2

I_{f}=\dfrac{4}{3}Mr^2

We need to calculate the angular velocity of the straight rod

Using conservation of rotational kinetic energy

I_{i}\omega_{i}=I_{f}\omega_{f}

Put the value into the formula

\dfrac{2}{3}Mr^2\times9.7=\dfrac{4}{3}Mr^2\times\omega_{f}

\omega_{f}=\dfrac{2\times9.7}{4}

\omega_{f}=4.85\ rad/s

Hence, The angular velocity of the straight rod is 4.85 rad/s.

Dima020 [189]2 years ago
7 0

Answer:

\omega_1 = 6.06 rad/s

Explanation:

Initially rod is bent into L shaped at mid point

So we will have rotational inertia of the rod given as

I = \frac{mL^2}{3} + (\frac{mL^2}{12} + m(L^2 + \frac{L^2}{4}))

I = \frac{5mL^2}{3}

Now when rod becomes straight during the rotation

then we will have

I_2= \frac{(2m)(2L)^2}{3} = \frac{8mL^2}{3}

now from angular momentum conservation we have

I \omega_o = I_1 \omega_1

(\frac{5mL^2}{3}) (9.7) = \frac{8mL^2}{3}\omega_1

\omega_1 = 6.06 rad/s

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Likurg_2 [28]

Answer:

Approximately \rm 11.2 \; N \cdot kg^{-1} at that distance from the center of the planet.

Option A) The low value of g near the cloud top of Saturn is possible because of the low density of the planet.

Explanation:

The value of g on a planet measures the size of gravity on an object for each unit of its mass. The equation for gravity is:

\displaystyle \frac{G \cdot M \cdot m}{R^2},

where

  • G \approx 6.67\times 10^{-11}\; \rm N \cdot kg^{-2} \cdot m^2.
  • M is the mass of the planet, and
  • m is the mass of the object.

To find an equation for g, divide the equation for gravity by the mass of the object:

\displaystyle g = \left.\frac{G \cdot M \cdot m}{R^2} \right/\frac{1}{m} = \frac{G \cdot M}{R^2}.

In this case,

  • M = 5.68\times 10^{26}\; \rm kg, and
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Calculate g based on these values:

\begin{aligned} g &= \frac{G \cdot M}{R^2}\cr &= \frac{6.67\times 10^{-11}\; \rm N \cdot kg^{-2} \cdot m^2\times 5.68\times 10^{26}\; \rm kg}{\left(5.82\times 10^7\; \rm m\right)^2} \cr &\approx 11.2\; \rm N\cdot kg^{-1} \end{aligned}.

Saturn is a gas giant. Most of its volume was filled with gas. In comparison, the earth is a rocky planet. Most of its volume was filled with solid and molten rocks. As a result, the average density of the earth would be greater than the average density of Saturn.

Refer to the equation for g:

\displaystyle g = \frac{G \cdot M}{R^2}.

The mass of the planet is in the numerator. If two planets are of the same size, g would be greater at the surface of the more massive planet.

On the other hand, if the mass of the planet is large while its density is small, its radius also needs to be very large. Since R is in the denominator of g, increasing the value of R while keeping M constant would reduce the value of g. That explains why the value of g near the "surface" (cloud tops) of Saturn is about the same as that on the surface of the earth (approximately 9.81\; \rm N \cdot kg^{-1}.

As a side note, 5.82\times 10^7\rm \; m likely refers to the distance from the center of Saturn to its cloud tops. Hence, it would be more appropriate to say that the value of g near the cloud tops of Saturn is approximately \rm 11.2 \; N \cdot kg^{-1}.

6 0
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John runs 1.0 m/s at first, and then accelerates to 1.6 m/s during
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Answer: 0.13m/s^2

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If John runs 1.0 m/s first, we assume this is V1. He accelerates to 1.6 m/s; this is V2.

a=\frac{1.6m/s-1.0m/s}{4.5s}

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Answer:

T₂ = 5646 K

Explanation:

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          P = σ. A e T⁴

Where next is the Stefam-Bolztmann constant with value 5,670 10-8 W / m² K⁴, A is the area of ​​the disk, T the absolute temperature and e the emissivity that for a black body is  1

The intensity is defined as the amount of radiation that arrives per unit area. For this we assume that the radiation expands uniformly in all directions, the intensity is

           I = P / A

Writing this expression for both discs

          I₁ A₁ = I₂ A₂

          I₂ = I₁ A₁ / A₂

The area of ​​a sphere is

          A = 4π r²

           I₂ = I₁ (r₁ / r₂)²

          r₂ = r₁ ± 5

          I₁ = I₂ ( (r₁ ± 5)/r₁)²

.

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         P / A = σ e T⁴

          I = σ e T⁴

This is the intensity that affects the disk, substitute in the intensity equation

         σ e₁ T₁⁴ = σ e₂ T₂⁴ (r₂ / r₁)²

The first disc indicates that it is a black body whereby e₁ = 1, the second disc, as it is painted white, the emissivity is less than 1, the emissivity values ​​of the white paint change between 0.90 and 0.95, for this calculation let's use 0.90 matt white

        e₁ T₁⁴ = T₂⁴   (r1 + 5)²/r₁²

       T₁ = T₂  {(e₂/e₁)}^{1/4}  √(1 ± 1/ r₁)  

If we assume that r₁ is large, which is possible since the disks are in deep space, we can expand the last term

           (1 ±x) n = 1 ± n x

Where x = 5 / r₁ << 1

We replace

          T₁ = T₂ {(e₂/e₁)}^{1/4}  (1 ± ½   5/r1)

           T₁ = T₂ {(e₂)}^{1/4}   (1 ± 5/2 1/r1)

If the discs are far from the star, they indicate that they are in deep space, the distance r₁ from being grade by which we can approximate; this is a very strong approach

              T₁ = T₂  {(e₂)}^{1/4} ¼

              T<u>₁</u> = T₂  0.90.9^{1/4}

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3 0
2 years ago
A metallic sphere of radius 2.0 cm is charged with +5.0-μC+5.0-μC charge, which spreads on the surface of the sphere uniformly.
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Answer:

Explanation:

Potential due to a charged metallic sphere having charge Q and radius r on its surface will be

v = k Q / r . On the surface and inside the metallic sphere , potential is the same . Outside the sphere , at a distance R from the centre  potential is

v = k Q / R

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On the surface of the shell , potential due to negative  charge is

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Total potential will be zero . they will cancel each other.

b ) On the surface of the sphere potential

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= 22.5 x 10⁵ V

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= -9 x 10⁵

Total potential

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= 13.5 x 10⁵ V

c ) In the space between the two , potential will depend upon the distance of the point from the common centre .

d ) Inside the sphere , potential will be same as that on the surface that is

13.5 x 10⁵ V.

e ) Outside the shell , potential due to both positive and negative charge will cancel each other so it will be zero.

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