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Chapter 6: Problem 22

Compare an optical reflecting telescope and a radio telescope. What do they have in common? How are they different?

Short Answer

Expert verified
Reflecting and radio telescopes both serve the purpose of collecting signals from the cosmos, usually having a parabolic shape, and using a receiver/detector along with sensitive amplifiers. The main differences are that reflecting telescopes use mirrors to collect and focus light resulting in images for direct visualization, while radio telescopes collect radio waves that are then computer-interpreted. Additionally, radio telescopes can operate round-the-clock under any weather or light condition, thanks to the penetrating capacity of radio waves.

Step by step solution

01

Understanding the Basic Function of Both Telescopes

An optical reflecting, or just reflecting, telescope works by using a large mirror to gather and focus light, creating an image. This image is then magnified for viewing. Alternatively, a radio telescope collects radio waves from space, instead of light. These signals are interpreted by a computer to create an image or data that scientists can analyze.
02

Identifying Common Features

Both types of telescopes, although differing in their specific mechanisms, function by collecting signals – whether light or radiowaves – from space. This makes the main common feature their function as instruments that observe and record physical data from the cosmos. Additionally, they both typically have a parabolic shape, utilize a receiver or detector, and need sensitive amplifiers (to boost the signal strength).
03

Highlighting the Differences

Their main differences lie in the signals they collect, the medium through which those signals travel best, and the visibility conditions. As mentioned, optical telescopes collect light signals, work best in clear night conditions, and are hindered by atmospheric conditions, artificial light, and cloud cover. Radio telescopes, on the other hand, are sensitive to radio waves, which can penetrate these atmospheric conditions, allowing for round-the-clock operation in any weather or light condition.

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Most popular questions from this chapter

What is diffraction? Why does it limit the angular resolution of a telescope? What other physical phenomenon is often a more important restriction on angular resolution?

Suppose your Newtonian reflector has an objective mirror \(20 \mathrm{~cm}\) ( 8 in.) in diameter with a focal length of \(2 \mathrm{~m}\). What magnification do you get with eyepieces whose focal lengths are (a) \(9 \mathrm{~mm}\), (b) \(20 \mathrm{~mm}\), and (c) \(55 \mathrm{~mm}\) ? (d) What is the telescope's diffraction-limited angular resolution when used with orange light of wavelength \(600 \mathrm{~nm}\) ? (e) Would it be possible to achieve this angular resolution if you took the telescope to the summit of Mauna Kea? Why or why not?

What is a spectrograph? Why do many astronomers regard it as the most important device that can be attached to a telescope?

(a) Compare the light-gathering power of the Keck I 10.0-m telescope with that of the Hubble Space Telescope (HST), which has a \(2.4-\mathrm{m}\) objective mirror. (b) What advantages does Keck I have over HST? What advantages does HST have over Keck I?

Why must astronomers use satellites and Earth-orbiting observatories to study the heavens at X-ray and gamma-ray wavelengths?
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