Homework Help is Here – Start Your Trial Now!
Science
Chemistry
Astronomers observe spectra of planetary nebulae to learn about the stars that created them, and to understand how planetary nebulae contribute to the chemical enrichment of the Milky Way Galaxy over time. In order to determine the chemical abundances in nebulae, astronomers need to know the temperature of the gas and its density. Sulfur emission lines are useful for determining density in planetary nebulae. Certain electron transitions involve energy levels that are said to be metastable; the resulting emission lines are called "forbidden" lines, which really only means that they are less likely to occur than emission lines from the ordinary kind of transitions. lons and electrons in a planetary nebula are always moving and bumping into each other. The energy exchanged in these collisions isn't enough to strip off electrons, but it is enough to kick an electron to a higher energy level within the ground state. In fact, the only way that these higher levels can be populated is by collisions; their forbidden nature makes it extremely unlikely for an upward transition to be produced by an absorbed photon. In order to return to ground state, a photon must be released. One such wavelengths of interest is 673.1 nm (in the very red part of the visible spectrum). The λ 673.1 nm line strengthens as the nebulae gas density increases because such collisions also increase with density. 1. What is the frequency of that line? 2. What is the energy of that line? 3. Is a transition that takes place in the microwave region of the EM spectrum, which is capable of cooking food, higher or lower energy than the previously mentioned electron transition in S?

Astronomers observe spectra of planetary nebulae to learn about the stars that created them, and to understand how planetary nebulae contribute to the chemical enrichment of the Milky Way Galaxy over time. In order to determine the chemical abundances in nebulae, astronomers need to know the temperature of the gas and its density. Sulfur emission lines are useful for determining density in planetary nebulae. Certain electron transitions involve energy levels that are said to be metastable; the resulting emission lines are called "forbidden" lines, which really only means that they are less likely to occur than emission lines from the ordinary kind of transitions. lons and electrons in a planetary nebula are always moving and bumping into each other. The energy exchanged in these collisions isn't enough to strip off electrons, but it is enough to kick an electron to a higher energy level within the ground state. In fact, the only way that these higher levels can be populated is by collisions; their forbidden nature makes it extremely unlikely for an upward transition to be produced by an absorbed photon. In order to return to ground state, a photon must be released. One such wavelengths of interest is 673.1 nm (in the very red part of the visible spectrum). The λ 673.1 nm line strengthens as the nebulae gas density increases because such collisions also increase with density. 1. What is the frequency of that line? 2. What is the energy of that line? 3. Is a transition that takes place in the microwave region of the EM spectrum, which is capable of cooking food, higher or lower energy than the previously mentioned electron transition in S?

Introductory Chemistry: A Foundation
Introductory Chemistry: A Foundation
9th Edition
ISBN:9781337399425
Author:Steven S. Zumdahl, Donald J. DeCoste
Publisher:Steven S. Zumdahl, Donald J. DeCoste
Chapter12: Chemical Bonding
Section: Chapter Questions
Problem 17CR: Schrodinger and de Broglie suggested a ‘Wave—particle duality" for small particles—that is, if...
See similar textbooks
icon
Related questions
Question
Astronomers observe spectra of planetary nebulae to learn about the stars that created them, and to understand how planetary nebulae contribute to the chemical enrichment of the Milky Way Galaxy over time. In order to determine the chemical abundances in nebulae, astronomers need to know the temperature of the gas and its density. Sulfur emission lines are useful for determining density in planetary nebulae. Certain electron transitions involve energy levels that are said to be metastable; the resulting emission lines are called "forbidden" lines, which really only means that they are less likely to occur than emission lines from the ordinary kind of transitions. lons and electrons in a planetary nebula are always moving and bumping into each other. The energy exchanged in these collisions isn't enough to strip off electrons, but it is enough to kick an electron to a higher energy level within the ground state. In fact, the only way that these higher levels can be populated is by collisions; their forbidden nature makes it extremely unlikely for an upward transition to be produced by an absorbed photon. In order to return to ground state, a photon must be released. One such wavelengths of interest is 673.1 nm (in the very red part of the visible spectrum). The λ 673.1 nm line strengthens as the nebulae gas density increases because such collisions also increase with density. 1. What is the frequency of that line? 2. What is the energy of that line? 3. Is a transition that takes place in the microwave region of the EM spectrum, which is capable of cooking food, higher or lower energy than the previously mentioned electron transition in S?
Transcribed Image Text:Astronomers observe spectra of planetary nebulae to learn about the stars that created them, and to understand how planetary nebulae contribute to the chemical enrichment of the Milky Way Galaxy over time. In order to determine the chemical abundances in nebulae, astronomers need to know the temperature of the gas and its density. Sulfur emission lines are useful for determining density in planetary nebulae. Certain electron transitions involve energy levels that are said to be metastable; the resulting emission lines are called "forbidden" lines, which really only means that they are less likely to occur than emission lines from the ordinary kind of transitions. lons and electrons in a planetary nebula are always moving and bumping into each other. The energy exchanged in these collisions isn't enough to strip off electrons, but it is enough to kick an electron to a higher energy level within the ground state. In fact, the only way that these higher levels can be populated is by collisions; their forbidden nature makes it extremely unlikely for an upward transition to be produced by an absorbed photon. In order to return to ground state, a photon must be released. One such wavelengths of interest is 673.1 nm (in the very red part of the visible spectrum). The λ 673.1 nm line strengthens as the nebulae gas density increases because such collisions also increase with density. 1. What is the frequency of that line? 2. What is the energy of that line? 3. Is a transition that takes place in the microwave region of the EM spectrum, which is capable of cooking food, higher or lower energy than the previously mentioned electron transition in S?
Expert Solution
steps

Step by step

Solved in 3 steps with 9 images

SEE SOLUTIONCheck out a sample Q&A here
Blurred answer
Knowledge Booster
Absorption and Adsorption
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, chemistry and related others by exploring similar questions and additional content below.
Similar questions
  • SEE MORE QUESTIONS
Recommended textbooks for you
Introductory Chemistry: A Foundation
Introductory Chemistry: A Foundation
Chemistry
ISBN:
9781337399425
Author:
Steven S. Zumdahl, Donald J. DeCoste
Publisher:
Cengage Learning
Introductory Chemistry: An Active Learning Approa…
Introductory Chemistry: An Active Learning Approa…
Chemistry
ISBN:
9781305079250
Author:
Mark S. Cracolice, Ed Peters
Publisher:
Cengage Learning
SEE MORE TEXTBOOKS