21st Century Astronomy (fifth Edition)
5th Edition
ISBN: 9780393603330
Author: Laura Kay, Stacy Palen, George Blumenthal
Publisher: W. W. Norton & Company
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Chapter 6.3, Problem 6.4CYU
To determine
The biggest disadvantage of using telescope in space.
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1, What is the diameter, in meters, of the earth's orbit around the sun? Written in scientific notation, the diameter is________ times 10 to the power of_____ meters.
2, According to Roemer, about how many seconds does it take light to travel across the diameter of the earth's orbit? Do NOT include units of measure.
3, How do these two quantities determine the speed of light?
4, When ultraviolet light shines on glass, what does it do to electrons in the glass structure?
5, When energetic electrons in the glass structure vibrate against neighboring atoms, what happens to the energy of vibration?
6, What happens to the energy of a vibrating electron that does not collide with neighboring atoms?
7, How is the speed of light in glass affected by the succession of time delays that accompany the absorption and re-emission of light from atom to atom in the glass?
8, When looking at a shadow, the_________ is darker than the __________
10, How does the speed of light compare in water,…
Is light a wave phenomenon? Explain.
Why is it not possible for the human eye to see the frequencies of infrared light? Explain.
Why is it possible to see colors? Explain.
Mention and explain an everyday phenomenon in which the dispersion of light can be observed.
What is the purpose of adaptive optics?
A.
to improve the angular resolution of telescopes in space
B.
to eliminate the distorting effects of atmospheric turbulence for telescopes on the ground
C.
to increase the collecting area of telescopes on the ground
D.
to increase the magnification of telescopes on the ground
E.
to allow several small telescopes to work together like a single larger telescope
Chapter 6 Solutions
21st Century Astronomy (fifth Edition)
Ch. 6.1 - Prob. 6.1CYUCh. 6.1 - Prob. 6.2CYUCh. 6.2 - Prob. 6.3CYUCh. 6.3 - Prob. 6.4CYUCh. 6.4 - Prob. 6.5CYUCh. 6.5 - Prob. 6.6CYUCh. 6 - Prob. 1QPCh. 6 - Prob. 2QPCh. 6 - Prob. 3QPCh. 6 - Prob. 4QP
Ch. 6 - Prob. 5QPCh. 6 - Prob. 6QPCh. 6 - Prob. 7QPCh. 6 - Prob. 8QPCh. 6 - Prob. 9QPCh. 6 - Prob. 10QPCh. 6 - Prob. 11QPCh. 6 - Prob. 12QPCh. 6 - Prob. 13QPCh. 6 - Prob. 14QPCh. 6 - Prob. 15QPCh. 6 - Prob. 16QPCh. 6 - Prob. 17QPCh. 6 - Prob. 18QPCh. 6 - Prob. 19QPCh. 6 - Prob. 20QPCh. 6 - Prob. 21QPCh. 6 - Prob. 22QPCh. 6 - Prob. 23QPCh. 6 - Prob. 24QPCh. 6 - Prob. 25QPCh. 6 - Prob. 26QPCh. 6 - Prob. 27QPCh. 6 - Prob. 28QPCh. 6 - Prob. 29QPCh. 6 - Prob. 30QPCh. 6 - Prob. 31QPCh. 6 - Prob. 32QPCh. 6 - Prob. 33QPCh. 6 - Prob. 34QPCh. 6 - Prob. 35QPCh. 6 - Prob. 36QPCh. 6 - Prob. 37QPCh. 6 - Prob. 38QPCh. 6 - Prob. 39QPCh. 6 - Prob. 40QPCh. 6 - Prob. 41QPCh. 6 - Prob. 42QPCh. 6 - Prob. 43QPCh. 6 - Prob. 44QPCh. 6 - Prob. 45QP
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- Explain why we have to observe stars and other astronomical objects from above Earth’s atmosphere in order to fully learn about their properties.arrow_forwardThe X-ray image in Figure UN 5-5 shows the remains of an exploded star. Explain why images recorded by telescopes in space are often displayed in representational (“false”) color rather than in the “colors” (wavelengths) received by the telescope.arrow_forwardOutline the invention of a telescope. Describe the working of a telescope.arrow_forward
- Theory One significant telescope property is magnification (Mag). Magnification makes a small object appear larger. If Mag = 30X, the image is 30 times the size of the object. Related to Magnification is Field of View (FOV). FOV measures the fraction of the sky that can be viewed by the instrument. Generally, the higher the Mag, the lower the FOV. Light Gathering Power (LGP) is a measure of the light collection efficiency of the telescope. The higher the LGP, the brighter the image. LGP varies with the area (or diameter squared) of the aperture. Resolution (Res) measures the ability of the telescope to bring out fine detail. Res varies with aperture diameter. Also, Res is better for higher frequency (blue) light than for lower frequency (red light). Notice in Figure 9-1 for the Refractor that Objective focal length (fobj) and eyepiece focal length (feye) are labeled. The lens separation in this type of Refractor is feye + fobj. The magnification is fobj / feye Questions 1. A…arrow_forwardTheory One significant telescope property is magnification (Mag). Magnification makes a small object appear larger. If Mag = 30X, the image is 30 times the size of the object. Related to Magnification is Field of View (FOV). FOV measures the fraction of the sky that can be viewed by the instrument. Generally, the higher the Mag, the lower the FOV. Light Gathering Power (LGP) is a measure of the light collection efficiency of the telescope. The higher the LGP, the brighter the image. LGP varies with the area (or diameter squared) of the aperture. Resolution (Res) measures the ability of the telescope to bring out fine detail. Res varies with aperture diameter. Also, Res is better for higher frequency (blue) light than for lower frequency (red light). Notice in Figure 9-1 for the Refractor that Objective focal length (fobj) and eyepiece focal length (feye) are labeled. The lens separation in this type of Refractor is feye + fobj. The magnification is fobj / feye. Questions. (3.…arrow_forwardThe sun is 150,000,000 kmkm from earth; its diameter is 1,400,000 kmkm. For a science project on solar power, a student uses a 24-cmcm-diameter converging mirror with a focal length of 51 cmcm to focus sunlight onto an object. This casts an image of the sun on the object. For the most intense heat, the image of the sun should be in focus. What is the intensity of sunlight in the projected image? Assume that all of the light captured by the mirror is focused into the image. Express your answer with the appropriate units.arrow_forward
- Telescopes do more than just magnify images. In fact, if all they did was magnify images Galileo would have never seen the moons of Jupiter. What other important thing does the telescope do? a)The telescope is better at tracking movement than the naked eye is. b)The telescope is able to take disorderly rays and collimate them. c)The telescope is able to discern more colors than the naked eye can. d)The telescope is able to gather more light than the naked eye can. Kepler's design allowed him to achieve better image quality and higher magnifications than Galileo's. However, his design has a significant drawback. What is it? a) Kepler's telescope has rays intersecting each other, which creates the possibility that they will interfere with each other. b) Kepler's telescope is less able to collimate chaotic incoming light. c) Kepler's telescope collects less light. d) Kepler's image is inverted, while Galileo's is upright.arrow_forwardThe planet Venus is different from the earth in several respects. First, it is only 70% as far from the sun. Second, its thick clouds reflect 77% of all incident sunlight. Finally, its atmosphere is much more opaque to infrared light. Estimate the surface temperature again, taking the reflectivity of the clouds into account.arrow_forwardIt takes light 1.3 second to travel from here to the moon. Assuming the speed of light is 186,000 miles/s how far away is the moon from us. (Express answer in units of miles and kilo-meter)arrow_forward
- Large telescopes often have small fields of view, i.e. it can only see a very small corner of the sky. For example, the Hubble Space Telescope (HST) Advanced Camera has a field of view that is roughly square and about 0.055 degree on a side. How do I Calculate the angular area of the HST's field of view in square degrees?arrow_forwardA particular color of light has a frequency of approximately 8 X 1014 Hz. Use the relationship speed of light = frequency X wavelength, to find the wavelength of this light in air. Multiply your answer by 109 to get your answer in units given. __________ nanometersarrow_forwardPeople are often bothered when they discover that reflecting telescopes have a second mirror in the middle to bring the light out to an accessible focus where big instruments can be mounted. “Don’t you lose light?” people ask. Well, yes, you do, but there is no better alternative. You can estimate how much light is lost by such an arrangement. The primary mirror (the one at the bottom in Figure 6.6) of the Gemini North telescope is 8 m in diameter. The secondary mirror at the top is about 1 m in diameter. Use the formula for the area of a circle to estimate what fraction of the light is blocked by the secondary mirror. Figure 6.6 Focus Arrangements for Reflecting Telescopes. Reflecting telescopes have different options for where the light is brought to a focus. With prime focus, light is detected where it comes to a focus after reflecting from the primary mirror. With Newtonian focus, light is reflected by a small secondary mirror off to one side, where it can be detected (see also Figure 6.5). Most large professional telescopes have a Cassegrain focus in which light is reflected by the secondary mirror down through a hole in the primary mirror to an observing station below the telescope.arrow_forward
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