1 00:00:04,309 --> 00:00:02,629 when you take a picture of the sky you 2 00:00:06,950 --> 00:00:04,319 might see this 3 00:00:08,950 --> 00:00:06,960 an overexposed bright white glare that 4 00:00:11,350 --> 00:00:08,960 we know as the sun 5 00:00:13,589 --> 00:00:11,360 in photos the sun appears white because 6 00:00:14,709 --> 00:00:13,599 it emits all the colors we can see at 7 00:00:16,790 --> 00:00:14,719 once 8 00:00:19,429 --> 00:00:16,800 our eyes can only see a narrow range of 9 00:00:21,510 --> 00:00:19,439 light known as the visible spectrum when 10 00:00:22,550 --> 00:00:21,520 they combine together they make white 11 00:00:26,770 --> 00:00:22,560 light 12 00:00:30,070 --> 00:00:26,780 invisible to the naked eye 13 00:00:35,990 --> 00:00:31,910 these are images from nasa's solar 14 00:00:38,229 --> 00:00:36,000 dynamics observatory or sdo 15 00:00:40,630 --> 00:00:38,239 it was launched in 2010 and has been 16 00:00:42,830 --> 00:00:40,640 observing the sun from space in a way 17 00:00:46,150 --> 00:00:42,840 that our eyes 18 00:00:48,549 --> 00:00:46,160 cannot sda uses instruments with special 19 00:00:50,869 --> 00:00:48,559 filters to see the sun in 10 different 20 00:00:53,350 --> 00:00:50,879 wavelengths of light including many that 21 00:00:55,510 --> 00:00:53,360 we can't see with our own eyes 22 00:00:58,709 --> 00:00:55,520 for us to see them scientists convert 23 00:01:00,549 --> 00:00:58,719 sda's data to colours we can see 24 00:01:02,150 --> 00:01:00,559 the different colors correspond to 25 00:01:03,189 --> 00:01:02,160 different temperatures and regions on 26 00:01:07,429 --> 00:01:03,199 the sun 27 00:01:09,270 --> 00:01:07,439 releases material that can travel across 28 00:01:12,630 --> 00:01:09,280 the solar system and affect our 29 00:01:14,550 --> 00:01:12,640 technology in space and on earth 30 00:01:16,550 --> 00:01:14,560 these wavelengths show us the sun's 31 00:01:18,149 --> 00:01:16,560 upper atmospheric layers at different 32 00:01:20,390 --> 00:01:18,159 temperatures 33 00:01:23,190 --> 00:01:20,400 this wavelength highlights filaments and 34 00:01:27,590 --> 00:01:25,429 these wavelengths highlight the corona 35 00:01:29,350 --> 00:01:27,600 the sun's atmosphere that is much hotter 36 00:01:31,670 --> 00:01:29,360 than the sun's surface 37 00:01:33,910 --> 00:01:31,680 and shows features like coronal loops 38 00:01:35,910 --> 00:01:33,920 and coronal holes 39 00:01:38,230 --> 00:01:35,920 the wavelengths here reveal the sun's 40 00:01:40,390 --> 00:01:38,240 active regions which have intense 41 00:01:43,030 --> 00:01:40,400 magnetic activity that sometimes give 42 00:01:44,870 --> 00:01:43,040 rise to eruptions 43 00:01:49,270 --> 00:01:44,880 these wavelengths can see the hottest 44 00:01:53,510 --> 00:01:51,590 being able to see constant movement of 45 00:01:55,990 --> 00:01:53,520 material on the sun and in its 46 00:01:58,630 --> 00:01:56,000 atmosphere can help scientists better 47 00:02:00,709 --> 00:01:58,640 understand how our sun behaves 48 00:02:02,870 --> 00:02:00,719 and how to track storms that might 49 00:02:07,040 --> 00:02:02,880 affect our satellites and astronauts in 50 00:02:12,710 --> 00:02:07,050 space or communications on earth