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Ch 12: Rotation of a Rigid Body
Knight Calc - Physics for Scientists and Engineers 5th Edition
Knight Calc5th EditionPhysics for Scientists and EngineersISBN: 9780137344796Non è quello che usi tu?Cambia libro di testo
Capitolo 12, Problema 83a

During most of its lifetime, a star maintains an equilibrium size in which the inward force of gravity on each atom is balanced by an outward pressure force due to the heat of the nuclear reactions in the core. But after all the hydrogen 'fuel' is consumed by nuclear fusion, the pressure force drops and the star undergoes a gravitational collapse until it becomes a neutron star. In a neutron star, the electrons and protons of the atoms are squeezed together by gravity until they fuse into neutrons. Neutron stars spin very rapidly and emit intense pulses of radio and light waves, one pulse per rotation. These 'pulsing stars' were discovered in the 1960s and are called pulsars. a. A star with the mass (M = 2.0 X 1030 kg) and size (R = 7.0 x 108 m) of our sun rotates once every 30 days. After undergoing gravitational collapse, the star forms a pulsar that is observed by astronomers to emit radio pulses every 0.10 s. By treating the neutron star as a solid sphere, deduce its radius.

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Step 1: Understand the conservation of angular momentum. The angular momentum of the star before and after the collapse remains constant because there are no external torques acting on the system. The formula for angular momentum is L = Iω, where I is the moment of inertia and ω is the angular velocity.
Step 2: Write the moment of inertia for a solid sphere. The moment of inertia of a solid sphere is given by I = (2/5)MR², where M is the mass and R is the radius of the sphere. Use this formula for both the initial star and the neutron star.
Step 3: Calculate the initial angular velocity (ω_initial) of the star. Angular velocity is related to the rotation period (T) by the formula ω = 2π/T. For the initial star, T = 30 days, which needs to be converted into seconds.
Step 4: Calculate the final angular velocity (ω_final) of the neutron star. The rotation period of the neutron star is given as 0.10 s, so use the same formula ω = 2π/T to find ω_final.
Step 5: Apply the conservation of angular momentum. Set the initial angular momentum equal to the final angular momentum: (2/5)M(R_initial²)(ω_initial) = (2/5)M(R_final²)(ω_final). Simplify the equation to solve for R_final, the radius of the neutron star.

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Gravitational Equilibrium

Gravitational equilibrium in a star occurs when the inward gravitational force pulling matter toward the center is balanced by the outward pressure from nuclear fusion reactions in the core. This balance allows the star to maintain a stable size and prevents it from collapsing under its own gravity. When the nuclear fuel is depleted, this equilibrium is disrupted, leading to gravitational collapse.
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Neutron Star Formation

A neutron star forms when a massive star exhausts its nuclear fuel and undergoes gravitational collapse, compressing electrons and protons to form neutrons. This process results in an extremely dense object, where the gravitational forces are so strong that normal atomic structures cannot exist. Neutron stars are typically about 1.4 times the mass of the sun but compressed into a radius of only about 10 kilometers.
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Pulsars and Rotation

Pulsars are a type of neutron star that emit beams of electromagnetic radiation, including radio waves, due to their rapid rotation and strong magnetic fields. As the neutron star spins, these beams sweep across space, and if aligned with Earth, they can be detected as regular pulses. The rotation period of a pulsar can be extremely short, often just milliseconds, which is a result of the conservation of angular momentum during the collapse of the star.
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