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Chapter 15: Problem 11

Which two forces establish hydrostatic equilibrium in an evolving protostar? a. the force from pressure and gravity b. the force from pressure and the strong nuclear force c. gravity and the strong nuclear force d. energy emitted and energy produced

Short Answer

Expert verified
a. the force from pressure and gravity

Step by step solution

01

Understanding Hydrostatic Equilibrium

Hydrostatic equilibrium in a protostar is the balance between forces that prevents the protostar from collapsing or expanding. It is necessary to identify which forces are acting to establish this equilibrium.
02

Analyzing the Forces

Consider each force listed in the options and their role in a protostar: - Gravity: This is an inward force pulling the gases of the protostar towards its center. - Pressure: This is an outward force caused by the high temperatures and gas motion, countering gravity. - Strong nuclear force: Acts only at subatomic scales, not relevant for large-scale equilibrium. - Energy emitted and energy produced: These are not forces but energy transfer processes.
03

Eliminate Irrelevant Forces

Based on the analysis, eliminate options that include inappropriate forces: - The strong nuclear force is not significant in establishing large-scale equilibrium. - Energy emitted and produced are not forces.
04

Identify the Correct Answer

The remaining forces that establish hydrostatic equilibrium are the force from pressure and gravity. These forces balance each other to maintain the star's shape.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

gravity
In the context of protostars, gravity plays a crucial role. It is the force that pulls all matter towards the center of the protostar. This inward-pulling force is due to the mass of the protostar, which could be immense. As gravity pulls the gases inward, it causes the protostar's core to become more dense and hot.
When discussing hydrostatic equilibrium, gravity is one of the two forces that need to be balanced. Without gravity, the gas in the protostar would not condense into a solid body but would disperse throughout space. This inward pull of gravity is counteracted by another force called pressure.
pressure
Pressure in a protostar is generated by the high temperatures and energetic motions of gas particles. This force acts outward, opposing the inward pull of gravity. Within a protostar, the temperature can get extremely high due to the compression of gases. This high temperature causes gas particles to move rapidly, creating the force we know as pressure.

**Importance for Hydrostatic Equilibrium**
For hydrostatic equilibrium to be achieved in a protostar, the force from pressure must exactly balance the force from gravity. If the pressure were higher than gravity, the protostar would expand. Conversely, if gravity were stronger, the protostar would collapse inward.
It's a delicate balance. If achieved, it prevents the star from either collapsing or expanding uncontrollably. This equilibrium is essential for stable protostar evolution.
protostar evolution
The journey of a protostar towards becoming a stable star involves several stages.

**Early Stages**
Initially, a cloud of gas and dust in space begins to contract under its gravity. As it contracts, the center becomes denser and hotter, eventually forming a protostar.

**Achieving Hydrostatic Equilibrium**
As the protostar evolves, it reaches a stage where hydrostatic equilibrium is achieved. Here, the inward force of gravity is balanced by the outward pressure.

**Fusion and Main Sequence**
When the core temperature becomes high enough, nuclear fusion begins. This marks the transition of the protostar into a main sequence star. The energy produced by fusion in the core provides the pressure needed to balance gravity.
Protostars are fascinating subjects in astrophysics. Knowing how gravity and pressure interact helps in understanding stars' life cycles.

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Most popular questions from this chapter

What causes a hydrogen atom to radiate a photon of 21 -cm radio emission? a. The electron drops down one energy level. b. The formerly free electron is captured by the proton. c. The electron flips to an aligned spin state. d. The electron flips to an unaligned spin state.

If you placed your hand in boiling water \(\left(100^{\circ} \mathrm{C}\right)\) for even 1 second, you would get a very serious burn. If you placed your hand in a hot oven \(\left(200^{\circ} \mathrm{C}\right)\) for a second or two, you would hardly feel the heat. Explain this difference and how it relates to million-kelvin regions of the interstellar medium.

Suppose you are studying a visible-light image of a distant galaxy, and you see a dark lane cutting across the bright disk. This dark line is most likely caused by a. gravitational instabilities that clear the area of stars. b. dust in the Milky Way blocking the view of the distant galaxy. c. dust in the distant galaxy blocking the view of stars in the disk. d. a flaw in the instrumentation.

In astronomy, the term bipolar refers to outflows that a. point in opposite directions. b. alternate between expanding and collapsing. c. rotate about a polar axis. d. show spiral structure.

Neutral hydrogen emits radiation at a radio wavelength of \(21 \mathrm{cm}\) when an atom drops from a higher-energy spin state to a lower-energy spin state. On average, each atom remains in the higher energy state for 11 million years \(\left(3.5 \times 10^{14}\) seconds) \right. a. What is the probability that any given atom will make the transition in 1 second? b. If there are \(6 \times 10^{59}\) atoms of neutral hydrogen in a \(500-M_{\text {sun }}\) cloud, how many photons of 21 -cm radiation will the cloud emit each second? c. How does this number compare with the \(1.8 \times 10^{45}\) photons emitted each second by a solar-type star?
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