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Chapter 17: Problem 22

Supernova remnants a. can be viewed at all wavelengths. b. can be viewed at only a few emission lines. c. are never seen in radio waves. d. have colors because the moving gas emits Doppler-shifted emission lines.

Short Answer

Expert verified
a. can be viewed at all wavelengths.

Step by step solution

01

Understand the Question

Identify what the question is asking. The question is about the characteristics of supernova remnants, specifically regarding how they can be viewed and what causes their colors.
02

Examine Each Option

Review each provided answer choice to determine which one correctly describes supernova remnants.
03

Analyze Option A

Option A states that supernova remnants can be viewed at all wavelengths. Research indicates this is correct as supernova remnants emit across the electromagnetic spectrum, including radio, infrared, visible light, ultraviolet, X-ray, and gamma-ray.
04

Analyze Option B

Option B states that supernova remnants can be viewed at only a few emission lines. This is incorrect because they can be observed in a broad range of wavelengths, not just a few emission lines.
05

Analyze Option C

Option C states that supernova remnants are never seen in radio waves. This is incorrect because supernova remnants are indeed observed in radio wavelengths.
06

Analyze Option D

Option D states that supernova remnants have colors because the moving gas emits Doppler-shifted emission lines. While Doppler shifting can affect the observed light, it is not solely responsible for the colors seen in supernova remnants.
07

Select the Correct Answer

Based on the analysis, the correct answer is option A: Supernova remnants can be viewed at all wavelengths.

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Key Concepts

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

Electromagnetic Spectrum
The electromagnetic spectrum is the range of all types of electromagnetic radiation. Radiation is energy that travels and spreads out as it goes. The types of electromagnetic waves differ according to their wavelengths and energies. The electromagnetic spectrum includes:
  • Radio waves
  • Microwaves
  • Infrared
  • Visible light
  • Ultraviolet
  • X-rays
  • Gamma rays

Supernova remnants can be observed across all these wavelengths, providing valuable insights into their properties and the mechanisms driving their behavior. Each type of radiation reveals different information about the remnants.
Radio Astronomy
Radio astronomy involves observing celestial objects by detecting radio waves they emit. These waves have much longer wavelengths compared to visible light, allowing astronomers to look through dust clouds that might obscure the view in other wavelengths.

Supernova remnants are significant subjects in radio astronomy. They emit strong radio waves, which help astronomers:
  • Study the structure of remnants
  • Measure the expansion rate of the remnants
  • Understand the magnetic fields within
Observations in radio wavelengths provide a clear view of the supernova remnants' dynamics and interactions with the surrounding interstellar medium.
Doppler Effect
The Doppler Effect is a change in frequency or wavelength of a wave relative to an observer moving relative to the wave source. It's most commonly experienced as a change in pitch of sound but also applies to light waves.

In astronomy, the Doppler Effect helps measure the speed and direction of objects like supernova remnants. When gas moves towards us, its light is blue-shifted (shorter wavelengths). When gas moves away, its light is red-shifted (longer wavelengths).

These shifts help to:
  • Determine the velocity of the expanding remnants
  • Infer movement directions of different gas parts
  • Study the kinematics of remnants
Emission Lines
Emission lines are bright lines in a spectrum caused by the emission of photons from atoms and molecules. They occur when electrons in an atom jump to lower energy levels, releasing energy as light.

Supernova remnants exhibit various emission lines, allowing scientists to identify elements present and study the physical conditions inside them. These lines help in:
  • Identifying chemical compositions
  • Determining temperatures and densities of the gas
  • Understanding shock waves and ionization processes

By studying emission lines, astronomers can piece together the history and evolution of supernova remnants.

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Most popular questions from this chapter

T/F: A supernova can be as bright as its entire host galaxy.

The start of photo disintegration of iron in a star sets off a process that always results in a a. supernova. b. neutron star. c. black hole. d. pulsar.

The approximate relationship between the luminosity and the period of Cepheid variables is \(L_{\text {star }}\) \(\left(\operatorname{in} L_{\odot}\right)\) \(=335 P\) (in days). Delta Cephei has a cycle period of 5.4 days and a parallax of 0.0033 arcsecond (arcsec). A more distant Cepheid variable appears \(1 / 1,000\) as bright as Delta Cephei and has a period of 54 days. a. How far away (in parsecs) is the more distant Cepheid variable? b. Could the distance of the more distant Cepheid variable be measured by parallax? Explain.

Go to the Einstein@Home website (http://einsteinathome.org). In this distributed computing project, volunteers use their spare computer processing power to help search for new pulsars. Look over the "News" section on the right. Have any pulsars been found lately? Join the project, create an account, download BOINC, and follow directions to look for pulsars.

The Type II supernova that created the Crab Nebula was seen by Chinese and Arab astronomers in the year 1054 CE.The radius of the nebula is now 5.5 light-years, so the average expansion has been about: a. \(15 \mathrm{km} / \mathrm{s}\) b. \(150 \mathrm{km} / \mathrm{s}\) c. \(1,500 \mathrm{km} / \mathrm{s}\) d. \(15,000 \mathrm{km} / \mathrm{s}\)
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