Loose Leaf For Explorations: Introduction To Astronomy
9th Edition
ISBN: 9781260432145
Author: Thomas T Arny, Stephen E Schneider Professor
Publisher: McGraw-Hill Education
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 12, Problem 5TY
To determine
The primary method astronomers use to measure oscillations on the surface of the Sun.
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solutionStudents have asked these similar questions
. How big would a square solar sail need to be in order for sunlight to exert a 12 N force on it (use
1,100 W/m² as the intensity of the sunlight).
From which atmospheric layer of the Sun did the photons originate that resulted in sunburn? How do you know?
Calculate the deflection of light caused by the Sun's gravity.
Chapter 12 Solutions
Loose Leaf For Explorations: Introduction To Astronomy
Ch. 12 - Prob. 1QFRCh. 12 - Prob. 2QFRCh. 12 - Prob. 3QFRCh. 12 - Prob. 4QFRCh. 12 - Prob. 5QFRCh. 12 - Prob. 6QFRCh. 12 - Prob. 7QFRCh. 12 - Prob. 8QFRCh. 12 - Prob. 9QFRCh. 12 - Prob. 10QFR
Ch. 12 - Prob. 11QFRCh. 12 - Prob. 12QFRCh. 12 - Prob. 13QFRCh. 12 - Prob. 14QFRCh. 12 - Prob. 15QFRCh. 12 - Prob. 16QFRCh. 12 - Prob. 17QFRCh. 12 - Prob. 18QFRCh. 12 - Prob. 19QFRCh. 12 - Prob. 20QFRCh. 12 - Prob. 1TQCh. 12 - Prob. 2TQCh. 12 - Prob. 3TQCh. 12 - Prob. 4TQCh. 12 - Prob. 5TQCh. 12 - Prob. 6TQCh. 12 - Prob. 7TQCh. 12 - Prob. 8TQCh. 12 - Prob. 9TQCh. 12 - Prob. 1PCh. 12 - Prob. 2PCh. 12 - Prob. 7PCh. 12 - Prob. 8PCh. 12 - Prob. 9PCh. 12 - Prob. 10PCh. 12 - Prob. 11PCh. 12 - Prob. 1TYCh. 12 - Prob. 2TYCh. 12 - Prob. 3TYCh. 12 - Prob. 4TYCh. 12 - Prob. 5TYCh. 12 - Prob. 6TY
Knowledge Booster
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- Background: Design and completely analyze an optical system to measure how fast the Sun is spinning,based on the Doppler shift between the west side of the sun (always turning toward us atvelocity v1) and the east side (turning away from us, also at velocity v1). It turns out the Sun hasvery sharp emission lines at a wavelength of λ = 630.0 nm. You may ignore Earth’s rotation andatmosphere.You’ll need at least 2 parts in your optical system. First, you’ll need to gather (maybe focus,maybe magnify?) the light from only the outer edge of the sun—no more than 5% of itsdiameter as seen from Earth. Be sure your system blocks out the rest of the sun when taking ameasurement of one side or the other. Second, you’ll need to very precisely and accuratelyseparate the sun’s spectrum into different wavelengths so you can measure the difference inwavelength caused by the Doppler shifts. You can use any combination of any optical elementswe have discussed in class: lenses, mirrors, pinholes,…arrow_forward1. The Sun radiates energy like a black body with temperature 5800 K. Use the Stefan-Boltzmann Law to calculate the Sun's Luminosity (which is the Sun's Surface Area times the Flux radiated per unit surface area. Use the following parameters: Sun's Radius = R = 6.96 x 1010 cm Stefan-Boltzmann Const = s = 5.67 x 10-5 ergs/cm2 K4 sSun's Temperature = T = 5800 K Formula for Luminosity: L = 4pR2 sT 4 What is the Sun's Luminosity? __________ ergs/sarrow_forwardLook up the wavelengths of the spectral lines of hydrogen, and the nomenclature used to label these lines. Identify the hydrogen lines in the solar spectrum over the range shown below.arrow_forward
- B2. A spherical star is detected by an astronaut in a spacecraft at a distance z of 1.5×10¹2 kilometers. The star can be regarded as a blackbody with a temperature of 11,300 K. The radius r of the star is 3.5×106 kilometers. (a) Calculate the radiant exitance and the radiant intensity of the star. (b) Calculate the irradiance that can be detected by the astronaut. (c) The photodetector used by the astronaut in the spacecraft has a responsivity of 120 kV/W and an photosensitive area of 0.5 mm². Calculate the output voltage of the detector in the detection of the star. CAMINS +II+ Figure B2arrow_forwardExplain why the presence of spectral lines of a given element in the solar spectrum tells you that element is present in the Sun, but the absence of the lines would not necessarily mean the element is absent from the Sun.arrow_forwardAppendix I lists some of the nearest stars. Are most of these stars hotter or cooler than the Sun? Do any of them emit more energy than the Sun? If so, which ones?arrow_forward
- The edge of the Sun doesn’t have to be absolutely sharp in order to look that way to us. It just has to go from being transparent to being completely opaque in a distance that is smaller than your eye can resolve. Remember from Astronomical Instruments that the ability to resolve detail depends on the size of the telescope’s aperture. The pupil of your eye is very small relative to the size of a telescope and therefore is very limited in the amount of detail you can see. In fact, your eye cannot see details that are smaller than 1/30 of the diameter of the Sun (about 1 arcminute). Nearly all the light from the Sun emerges from a layer that is only about 400 km thick. What fraction is this of the diameter of the Sun? How does this compare with the ability of the human eye to resolve detail? Suppose we could see light emerging directly from a layer that was 300,000 km thick. Would the Sun appear to have a sharp edge?arrow_forwardThe radius of the Sun is 0.7 million km. Examine Figure 7-3 to estimate the thickness of the chromosphere. What fraction of the Sun’s radius is taken up by the chromosphere?arrow_forward
arrow_back_ios
arrow_forward_ios
Recommended textbooks for you
- Horizons: Exploring the Universe (MindTap Course ...PhysicsISBN:9781305960961Author:Michael A. Seeds, Dana BackmanPublisher:Cengage LearningStars and Galaxies (MindTap Course List)PhysicsISBN:9781337399944Author:Michael A. SeedsPublisher:Cengage LearningFoundations of Astronomy (MindTap Course List)PhysicsISBN:9781337399920Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
- AstronomyPhysicsISBN:9781938168284Author:Andrew Fraknoi; David Morrison; Sidney C. WolffPublisher:OpenStax
Horizons: Exploring the Universe (MindTap Course ...
Physics
ISBN:9781305960961
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Stars and Galaxies (MindTap Course List)
Physics
ISBN:9781337399944
Author:Michael A. Seeds
Publisher:Cengage Learning
Foundations of Astronomy (MindTap Course List)
Physics
ISBN:9781337399920
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Astronomy
Physics
ISBN:9781938168284
Author:Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher:OpenStax
Heat Transfer: Crash Course Engineering #14; Author: CrashCourse;https://www.youtube.com/watch?v=YK7G6l_K6sA;License: Standard YouTube License, CC-BY