By Stacey Palen
Presents a uncomplicated advent to the themes coated in a starting astronomy direction, with an emphasis on problem-solving tools usually taught "on the fly" or in ad-hoc tutorials - Closes the space in scholar literature through delivering a targeted, accomplished presentation of simple astronomical problem-solving options - Readers research via instance with the aid of greater than two hundred particular difficulties and step by step options, supplemented with over a hundred specified charts and graphs - Designed to accompany all major 100-level astronomy textbooks, or for use as a stand-alone advisor for newbie stargazers
Read or Download Schaum's Outline of Astronomy PDF
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Extra info for Schaum's Outline of Astronomy
Example text
However, because the same amount of light is used to make a magnified image as was used to make the original image, the magnified image is fainter. Also, the field of view (the area of sky that can be seen through the telescope) is reduced as the image is magnified. In practice, astronomers rarely magnify an image using their telescope. Instead, they take a picture, using either photographic film or a digital camera, and then use an image-processing program to make the image larger. As a practical rule, the useful magnification of an amateur telescope does not exceed 10 times the diameter of the objective in centimeters.
Relatively recent developments in telescope technology, such as interferometry or adaptive optics, are able to produce images with angular resolutions comparable to those that could be achieved with space-based telescopes. Interferometry has been used primarily in the radio and millimeter wavelengths, and links many smaller telescopes together to simulate a much larger telescope. Optical interferometers have been built but, because of the higher frequencies, are much more difficult to construct on the same scale as radio and millimeter interferometers.
Fig. 3-1. Sequence of terrestrial planet formation and evolution. CHAPTER 3 Terrestrial Planets 54 All planets are gradually releasing heat into space (see Fig. 3-1). Most of the heat created during the formation of the planets, as planetesimals smashed into each other, has already been lost. Planets currently releasing heat to space are generating it in their cores, as radioactive materials decay. This heat is then either conducted or convected to the surface, where it is subsequently radiated away.