1 00:00:00,000 --> 00:00:02,270 When you take a picture of the sky, 2 00:00:02,270 --> 00:00:04,280 you might see this: 3 00:00:04,280 --> 00:00:09,090 an overexposed, bright, white glare that we know as the Sun. 4 00:00:09,090 --> 00:00:10,850 In photos, the Sun appears white 5 00:00:10,850 --> 00:00:14,910 because it emits all the colors we can see at once. 6 00:00:14,910 --> 00:00:17,290 Our eyes can only see a narrow range of light 7 00:00:17,290 --> 00:00:19,140 known as the visible spectrum. 8 00:00:19,140 --> 00:00:22,710 When they combine together, they make white light.   9 00:00:22,710 --> 00:00:29,990 But the Sun also emits light that is invisible to the naked eye. 10 00:00:29,990 --> 00:00:35,930 These are images from NASA's Solar Dynamics Observatory, or SDO. 11 00:00:35,930 --> 00:00:37,570 It was launched in 2010 12 00:00:37,570 --> 00:00:39,910 and has been observing the Sun from space 13 00:00:39,910 --> 00:00:44,050 in a way that our eyes cannot. 14 00:00:44,050 --> 00:00:46,860 SDO uses instruments with special filters 15 00:00:46,860 --> 00:00:49,910 to see the Sun in 10 different wavelengths of light, 16 00:00:49,910 --> 00:00:53,450 including many that we can’t see with our own eyes. 17 00:00:53,450 --> 00:00:54,490 For us to see them, 18 00:00:54,490 --> 00:00:58,500 Scientists convert SDO’s data to colors we can see. 19 00:00:58,500 --> 00:01:02,960 The different colors correspond to different temperatures and regions on the Sun. 20 00:01:02,960 --> 00:01:06,200 This allows us to study how the Sun releases material 21 00:01:06,200 --> 00:01:08,540 that can travel across the solar system 22 00:01:08,540 --> 00:01:12,620 and affect our technology in space and on Earth. 23 00:01:12,620 --> 00:01:18,000 These wavelengths show us the Sun’s upper atmospheric layers at different temperatures. 24 00:01:18,000 --> 00:01:23,580 This wavelength highlights filaments and prominences. 25 00:01:23,580 --> 00:01:26,750 These wavelengths highlight the corona, the Sun’s atmosphere 26 00:01:26,750 --> 00:01:28,960 that is much hotter than the Sun’s surface 27 00:01:28,960 --> 00:01:34,230 and shows features like coronal loops and coronal holes. 28 00:01:34,230 --> 00:01:37,070 The wavelengths here reveal the Sun’s active regions, 29 00:01:37,070 --> 00:01:42,700 which have intense magnetic activity that sometimes give rise to eruptions. 30 00:01:42,700 --> 00:01:49,280 These wavelengths can see the hottest material in a solar flare. 31 00:01:49,280 --> 00:01:54,340 Being able to see constant movement of material on the Sun and in its atmosphere 32 00:01:54,340 --> 00:01:58,100 can help scientists better understand how our Sun behaves 33 00:01:58,100 --> 00:02:01,230 and how to track storms that might affect 34 00:02:01,230 --> 00:00:00,000 our satellites and astronauts in space or communications on Earth.