{"id":668,"date":"2016-11-15T21:38:09","date_gmt":"2016-11-15T21:38:09","guid":{"rendered":"https:\/\/courses.lumenlearning.com\/astronomy\/?post_type=chapter&p=668"},"modified":"2017-07-20T21:28:40","modified_gmt":"2017-07-20T21:28:40","slug":"introduction-to-stars-from-adolescence-to-old-age","status":"publish","type":"chapter","link":"https:\/\/courses.lumenlearning.com\/suny-ncc-astronomy\/chapter\/introduction-to-stars-from-adolescence-to-old-age\/","title":{"raw":"Introduction to Stars from Adolescence to Old Age","rendered":"Introduction to Stars from Adolescence to Old Age"},"content":{"raw":"The Sun and other stars cannot last forever. Eventually they will exhaust their nuclear fuel and cease to shine. But how do they change during their long lifetimes? And what do these changes mean for the future of Earth?\r\n\r\nWe now turn from the birth of stars to the rest of their life stories. This is not an easy task since stars live much longer than astronomers. Thus, we cannot hope to see the life story of any single star unfold before our eyes or telescopes. To learn about their lives, we must survey as many of the stellar inhabitants of the Galaxy as possible. With thoroughness and a little luck, we can catch at least a few of them in each stage of their lives. As you\u2019ve learned, stars have many different characteristics, with the differences sometimes resulting from their different masses, temperatures, and luminosities, and at other times derived from changes that occur as they age. Through a combination of observation and theory, we can use these differences to piece together the life story of a star.\r\n\r\n[caption id=\"\" align=\"alignnone\" width=\"1312\"]\"False-color Figure 1. Ant Nebula:<\/strong> During the later phases of stellar evolution, stars expel some of their mass, which returns to the interstellar medium to form new stars. This Hubble Space Telescope image shows a star losing mass. Known as Menzel 3, or the Ant Nebula, this beautiful region of expelled gas is about 3000 light-years away from the Sun. We see a central star that has ejected mass preferentially in two opposite directions. The object is about 1.6 light-years long. The image is color coded\u2014red corresponds to an emission line of sulfur, green to nitrogen, blue to hydrogen, and blue\/violet to oxygen. (credit: modification of work by NASA, ESA and The Hubble Heritage Team (STScI\/AURA))[\/caption]","rendered":"

The Sun and other stars cannot last forever. Eventually they will exhaust their nuclear fuel and cease to shine. But how do they change during their long lifetimes? And what do these changes mean for the future of Earth?<\/p>\n

We now turn from the birth of stars to the rest of their life stories. This is not an easy task since stars live much longer than astronomers. Thus, we cannot hope to see the life story of any single star unfold before our eyes or telescopes. To learn about their lives, we must survey as many of the stellar inhabitants of the Galaxy as possible. With thoroughness and a little luck, we can catch at least a few of them in each stage of their lives. As you\u2019ve learned, stars have many different characteristics, with the differences sometimes resulting from their different masses, temperatures, and luminosities, and at other times derived from changes that occur as they age. Through a combination of observation and theory, we can use these differences to piece together the life story of a star.<\/p>\n

\"False-color<\/p>\n

Figure 1. Ant Nebula:<\/strong> During the later phases of stellar evolution, stars expel some of their mass, which returns to the interstellar medium to form new stars. This Hubble Space Telescope image shows a star losing mass. Known as Menzel 3, or the Ant Nebula, this beautiful region of expelled gas is about 3000 light-years away from the Sun. We see a central star that has ejected mass preferentially in two opposite directions. The object is about 1.6 light-years long. The image is color coded\u2014red corresponds to an emission line of sulfur, green to nitrogen, blue to hydrogen, and blue\/violet to oxygen. (credit: modification of work by NASA, ESA and The Hubble Heritage Team (STScI\/AURA))<\/p>\n<\/div>\n\n\t\t\t

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