A uniform disk turns at 4.1 rev/s around a frictionless central axis. A nonrotating rod, of the same mass as the disk and length equal to the disk’s diameter, is dropped onto the freely spinning disk, Fig. 11–32. They then turn together around the spindle with their centers superposed. What is the angular frequency in rev/s of the combination?
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16. Angular Momentum
Conservation of Angular Momentum
Problem 83b
Textbook Question
Suppose a star the size of our Sun, but with mass 8.0 times as great, were rotating at a speed of 1.0 revolution every 9.0 days. If it were to undergo gravitational collapse to a neutron star of radius 12 km, losing 0.70 of its mass in the process, what would its rotation speed be? Assume the star is a uniform sphere at all times. Assume also that the thrown-off mass carries off either its proportional share (0.70) of the initial angular momentum.

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Step 1: Understand the conservation of angular momentum. Angular momentum is conserved in the absence of external torques. The initial angular momentum of the star before collapse must equal the final angular momentum of the neutron star plus the angular momentum carried away by the ejected mass.
Step 2: Write the formula for angular momentum of a uniform sphere. The angular momentum \( L \) of a sphere is given by \( L = I \omega \), where \( I \) is the moment of inertia and \( \omega \) is the angular velocity. For a uniform sphere, \( I = \frac{2}{5} M R^2 \), where \( M \) is the mass and \( R \) is the radius.
Step 3: Calculate the initial angular momentum of the star. Use the initial mass \( M_i = 8.0 M_{\odot} \), radius \( R_i = R_{\odot} \), and angular velocity \( \omega_i = \frac{2 \pi}{T} \), where \( T = 9.0 \, \text{days} \). Substitute these values into \( L_i = \frac{2}{5} M_i R_i^2 \omega_i \).
Step 4: Account for the mass loss. After the collapse, the neutron star retains \( 0.30 \) of the initial mass, so \( M_f = 0.30 M_i \). The ejected mass carries away \( 0.70 \) of the initial angular momentum, so the remaining angular momentum is \( L_f = 0.30 L_i \).
Step 5: Calculate the final angular velocity of the neutron star. Use the final moment of inertia \( I_f = \frac{2}{5} M_f R_f^2 \), where \( R_f = 12 \, \text{km} \). Solve for \( \omega_f \) using \( L_f = I_f \omega_f \). Combine all expressions to find \( \omega_f \) in terms of the given quantities.

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Key Concepts
Here are the essential concepts you must grasp in order to answer the question correctly.
Angular Momentum
Angular momentum is a measure of the rotational motion of an object and is defined as the product of the object's moment of inertia and its angular velocity. For a uniform sphere, the moment of inertia depends on its mass and radius. In this scenario, the conservation of angular momentum principle states that if no external torque acts on a system, the total angular momentum before and after an event (like gravitational collapse) remains constant.
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Gravitational Collapse
Gravitational collapse occurs when an object's internal pressure is insufficient to counteract the force of gravity, leading to a decrease in volume and an increase in density. In the context of a star collapsing into a neutron star, this process results in a significant loss of mass and a dramatic increase in density, which affects the star's rotation speed due to the conservation of angular momentum.
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Neutron Star Characteristics
A neutron star is the remnant of a supernova explosion and is incredibly dense, typically with a radius of about 10-12 km. It is composed primarily of neutrons and has a strong gravitational field. The rapid rotation of neutron stars can lead to phenomena such as pulsars, where the star emits beams of radiation due to its magnetic field and rotation, making the understanding of its rotational dynamics crucial in this problem.
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