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1 00:00:00,000 --> 00:00:03,036 If you do a quick search for “spectroscopy data” 2 00:00:03,503 --> 00:00:05,772 there are numerous ways that the data can appear. 3 00:00:06,172 --> 00:00:09,075 Those variations are based on the source of the cosmic light. 4 00:00:09,376 --> 00:00:11,945 There are three types of spectra that we can use: 5 00:00:12,245 --> 00:00:13,346 continuous; 6 00:00:13,713 --> 00:00:14,814 emission; 7 00:00:15,148 --> 00:00:16,249 and absorption. 8 00:00:17,817 --> 00:00:21,021 Light from a hot, dense source, like the Sun, 9 00:00:21,154 --> 00:00:23,289 produces a continuous spectrum. 10 00:00:26,059 --> 00:00:29,829 When that light passes through cooler gases on its way to us, 11 00:00:29,829 --> 00:00:33,466 the gases take away, or absorb, some of that energy. 12 00:00:33,933 --> 00:00:38,104 Dark lines appear where specific colors are missing. 13 00:00:39,606 --> 00:00:42,709 And when thin gases glow themselves, 14 00:00:42,909 --> 00:00:45,745 we see only their characteristic colors, 15 00:00:45,745 --> 00:00:48,114 kind of like a cosmic barcode. 16 00:00:50,083 --> 00:00:54,421 These are the emission spectra from pure elements that were given a voltage to glow. 17 00:00:54,421 --> 00:00:55,989 Just like my spectra tube. 18 00:00:55,989 --> 00:00:57,557 But, way better. |