1 00:00:01,060 --> 00:00:03,430 - [Kevin] So thanks for the invitation 2 00:00:03,430 --> 00:00:05,430 to join you in your kitchens 3 00:00:05,430 --> 00:00:09,440 and basements and guest bedrooms to talk about 4 00:00:09,440 --> 00:00:11,910 the Extreme-UV Stellar Characterization 5 00:00:11,910 --> 00:00:16,010 for Atmospheric Physics and Evolution Mission Concept. 6 00:00:16,010 --> 00:00:17,720 So even as Tasha mentioned 7 00:00:17,720 --> 00:00:21,720 ESCAPE is currently in phase A. 8 00:00:21,720 --> 00:00:26,720 We were one of two missions selected on March 16th, 9 00:00:26,800 --> 00:00:30,150 which was also the day that my university was shutting down, 10 00:00:30,150 --> 00:00:33,013 so it was a turbulent couple of days. 11 00:00:35,320 --> 00:00:37,790 So just to give you a quick overview of what the process 12 00:00:37,790 --> 00:00:39,620 looks like before I talk about the mission, 13 00:00:39,620 --> 00:00:43,173 so we're in a nine month phase A process now, 14 00:00:44,190 --> 00:00:47,020 the final deliverable from the phase A study 15 00:00:47,020 --> 00:00:48,630 is a concept study report 16 00:00:48,630 --> 00:00:53,120 that is currently due to NASA on December 17th. 17 00:00:53,120 --> 00:00:54,270 And then there's a site visit 18 00:00:54,270 --> 00:00:56,183 that happens a few months after that. 19 00:00:57,450 --> 00:00:59,823 So that's what we're working towards now. 20 00:01:01,240 --> 00:01:05,270 So ESCAPE is a pretty simple mission in terms 21 00:01:05,270 --> 00:01:08,623 of its science goal and implementation. 22 00:01:09,680 --> 00:01:11,150 Really we're actually interested 23 00:01:11,150 --> 00:01:13,810 in understanding the high energy 24 00:01:13,810 --> 00:01:17,950 environments in the habitable zones around nearby stars. 25 00:01:17,950 --> 00:01:19,600 You go to the next slide, please. 26 00:01:21,870 --> 00:01:26,870 So as you know, it's one of NASA's key strategic goals 27 00:01:26,880 --> 00:01:29,340 to identify and characterize 28 00:01:29,340 --> 00:01:32,810 Rocky planets in around nearby stars. 29 00:01:32,810 --> 00:01:34,820 Animation is moving a little bit slow. 30 00:01:34,820 --> 00:01:38,420 Of course the concept of liquid water habitable zone, 31 00:01:38,420 --> 00:01:42,190 is dependent upon the spectral type of the host star, 32 00:01:42,190 --> 00:01:44,810 so it moves out for more massive stars 33 00:01:44,810 --> 00:01:47,723 and moves inward for less massive stars. 34 00:01:50,102 --> 00:01:51,702 You go to the next slide please. 35 00:01:54,570 --> 00:01:55,403 Thanks. 36 00:01:56,460 --> 00:01:59,320 And so there's a lot of investment from NASA 37 00:01:59,320 --> 00:02:01,580 and also our international partners 38 00:02:01,580 --> 00:02:05,440 and missions to finding and characterize these planets 39 00:02:05,440 --> 00:02:08,290 as they exist around different spectrum types. 40 00:02:08,290 --> 00:02:12,360 Beginning hopefully, next year or maybe a little bit after, 41 00:02:12,360 --> 00:02:14,060 the next slide please. 42 00:02:14,060 --> 00:02:16,410 with James Webb Space Telescope, 43 00:02:16,410 --> 00:02:19,860 we'll be focused primarily on looking 44 00:02:19,860 --> 00:02:23,590 for atmospheres on Rocky planets around indoors 45 00:02:23,590 --> 00:02:26,340 and then moving a little bit further into the future. 46 00:02:26,340 --> 00:02:27,173 Next slide. 47 00:02:28,190 --> 00:02:32,750 We hopefully will have a Ruvuor or HabEX like mission, 48 00:02:32,750 --> 00:02:33,673 to search for habitable worlds 49 00:02:33,673 --> 00:02:38,673 around FTK stars more proper sun earth analogs. 50 00:02:40,830 --> 00:02:45,830 So because all of these missions are looking for atmospheres 51 00:02:45,830 --> 00:02:47,800 and the signs of life in atmospheres, 52 00:02:47,800 --> 00:02:50,420 the question of atmospheric stability 53 00:02:50,420 --> 00:02:54,530 is actually pretty critical to understanding 54 00:02:54,530 --> 00:02:56,840 the results that these missions find. 55 00:02:56,840 --> 00:02:59,610 So understanding the host star is particularly important 56 00:02:59,610 --> 00:03:01,410 because it drives the survival 57 00:03:01,410 --> 00:03:04,000 of the atmospheres on rocky planets. 58 00:03:04,000 --> 00:03:05,283 Next star slide please. 59 00:03:06,170 --> 00:03:07,960 So this is, 60 00:03:07,960 --> 00:03:09,860 there's a lot of work been done in the last couple years 61 00:03:09,860 --> 00:03:13,510 about the high energy impacts of red dwarf stars 62 00:03:13,510 --> 00:03:16,673 on potentially habitable planets that are orbiting there. 63 00:03:17,930 --> 00:03:20,090 But there's essentially an open question 64 00:03:20,090 --> 00:03:21,470 about atmospheric survival, 65 00:03:21,470 --> 00:03:22,840 really on any type of planet 66 00:03:22,840 --> 00:03:25,370 other than truce on earth analogs. 67 00:03:25,370 --> 00:03:26,870 Then as we've learned recently, 68 00:03:26,870 --> 00:03:29,670 the sun is anomalously inactive anyways 69 00:03:31,593 --> 00:03:33,270 so a pretty open question. 70 00:03:33,270 --> 00:03:36,720 So if we wanna understand which planets can maintain 71 00:03:36,720 --> 00:03:39,640 habitable atmospheres and form habitable atmospheres, 72 00:03:39,640 --> 00:03:42,190 there are two primary unknowns 73 00:03:42,190 --> 00:03:44,430 what the initial atmosphere content 74 00:03:44,430 --> 00:03:46,260 and if they the initial water content, 75 00:03:46,260 --> 00:03:47,800 and then what is the host star doing? 76 00:03:47,800 --> 00:03:49,200 Go to the next slide please. 77 00:03:50,610 --> 00:03:53,906 And so, we kinda show the example here. 78 00:03:53,906 --> 00:03:56,090 Through a rapidly 79 00:03:59,565 --> 00:04:00,794 evaporating atmosphere 80 00:04:00,794 --> 00:04:02,910 of Earth-like planet around the red dwarf 81 00:04:02,910 --> 00:04:04,830 this is some work from one of the Trappist planets 82 00:04:04,830 --> 00:04:05,920 from Vent to Dorien 83 00:04:06,990 --> 00:04:08,620 where they predict essentially 84 00:04:08,620 --> 00:04:10,190 complete atmospheric mass loss 85 00:04:10,190 --> 00:04:12,760 within about the first billion years, 86 00:04:12,760 --> 00:04:16,120 versus a situation like we have here on earth, 87 00:04:16,120 --> 00:04:17,840 where we were able to maintain, 88 00:04:17,840 --> 00:04:21,090 an atmosphere for a geologic timescales. 89 00:04:21,090 --> 00:04:24,090 So, proto planetary disc studies are able 90 00:04:24,090 --> 00:04:27,440 to put constraints on the initial inventory 91 00:04:27,440 --> 00:04:29,620 for atmospheric volatiles. 92 00:04:29,620 --> 00:04:32,620 But then the other big question is what is the star doing? 93 00:04:32,620 --> 00:04:35,450 And so if we wanna understand how the star drive ESCAPE, 94 00:04:35,450 --> 00:04:38,660 we essentially are driven to the high energy radiation. 95 00:04:38,660 --> 00:04:39,610 Next slide, please. 96 00:04:41,190 --> 00:04:42,890 And specifically, Oh, sorry. 97 00:04:42,890 --> 00:04:43,723 One more slide. 98 00:04:46,570 --> 00:04:50,490 Specifically, what is the, extreme ultraviolet 99 00:04:50,490 --> 00:04:53,640 input into those planetary atmospheres? 100 00:04:53,640 --> 00:04:56,313 It's this 10 to 90 nanometers EUB, 101 00:04:57,410 --> 00:05:00,160 that drives atmospheric ionization, heating 102 00:05:00,160 --> 00:05:03,000 and ultimately escape to space. 103 00:05:03,000 --> 00:05:05,023 So if we wanna ask the question, 104 00:05:06,266 --> 00:05:07,370 what are the dominant impacts 105 00:05:07,370 --> 00:05:10,780 that the star has on the longterm survival 106 00:05:10,780 --> 00:05:12,710 of habitable atmospheres? 107 00:05:12,710 --> 00:05:13,740 We really need to ask 108 00:05:13,740 --> 00:05:17,340 what is the star doing in the extreme ultraviolet band pass? 109 00:05:17,340 --> 00:05:18,283 Next slide please. 110 00:05:19,670 --> 00:05:22,580 So unfortunately, that is the part of the spectrum 111 00:05:22,580 --> 00:05:24,900 that we know the absolute least about, 112 00:05:24,900 --> 00:05:27,970 and that's what we designed ESCAPE to go after. 113 00:05:27,970 --> 00:05:30,590 This is a spectrum of proxma Cen 114 00:05:30,590 --> 00:05:34,380 and the shaded regions here on the spectral 115 00:05:34,380 --> 00:05:37,510 on the Y-axis indicate the relative uncertainties 116 00:05:37,510 --> 00:05:38,450 of the fluxes. 117 00:05:38,450 --> 00:05:40,580 Now we can observe just about everything else. 118 00:05:40,580 --> 00:05:44,070 We have x-ray observations from Chandra and XMM. 119 00:05:44,070 --> 00:05:47,040 We have spectacular observations from Hubble, 120 00:05:47,040 --> 00:05:48,290 working in the optical 121 00:05:48,290 --> 00:05:51,000 and nearby in dork is not hard to observe, 122 00:05:51,000 --> 00:05:53,950 but we have very poor constraints on the EUV. 123 00:05:53,950 --> 00:05:55,500 So if you go to the next slide, 124 00:05:56,340 --> 00:05:58,040 there's been a kind of cottage industry 125 00:05:58,040 --> 00:06:00,120 over the last decade or so, 126 00:06:00,120 --> 00:06:01,450 coming up with different ways 127 00:06:01,450 --> 00:06:04,820 to estimate the extreme ultraviolet from other proxies. 128 00:06:04,820 --> 00:06:06,510 And I just, I won't walk through what all 129 00:06:06,510 --> 00:06:08,440 of these different things in this band mean, 130 00:06:08,440 --> 00:06:11,220 but these are all different ways using different proxies 131 00:06:11,220 --> 00:06:15,000 for estimating the extreme ultraviolet flux of prox Cen, 132 00:06:15,000 --> 00:06:16,793 and specifically in nearby Mstar. 133 00:06:18,130 --> 00:06:19,180 Now, as you can see, 134 00:06:19,180 --> 00:06:22,530 there's depending on where you are in the EUV spectrum, 135 00:06:22,530 --> 00:06:25,220 a few orders of magnitude disagreement 136 00:06:25,220 --> 00:06:26,710 between those different proxies 137 00:06:26,710 --> 00:06:31,230 on what the actual local EUV flux from that star is. 138 00:06:31,230 --> 00:06:33,050 And then it's pretty profound implications 139 00:06:33,050 --> 00:06:36,080 for the survival of an atmosphere on a Rocky planet 140 00:06:36,080 --> 00:06:37,586 that's orbiting that star. 141 00:06:37,586 --> 00:06:39,300 If you could go to the next slide, please. 142 00:06:39,300 --> 00:06:43,640 So, this shows the total earth oceans worth 143 00:06:43,640 --> 00:06:46,230 of hydrogen lost on those planets, 144 00:06:46,230 --> 00:06:49,440 depending on what reconstruction you assume, 145 00:06:49,440 --> 00:06:50,780 what proxy you assume, 146 00:06:50,780 --> 00:06:55,070 and also what history of the extreme ultraviolet, 147 00:06:55,070 --> 00:06:56,760 flux from the star is. 148 00:06:56,760 --> 00:06:58,330 So you can see from here, 149 00:06:58,330 --> 00:07:01,250 depending on how you guesstimate your EUV flux, 150 00:07:01,250 --> 00:07:03,540 you could have anywhere from maybe a 10th 151 00:07:03,540 --> 00:07:05,130 of an earth ocean lost over four 152 00:07:05,130 --> 00:07:07,260 and a half billion years to something like 20 153 00:07:07,260 --> 00:07:09,250 or 30 earth oceans lost. 154 00:07:09,250 --> 00:07:10,900 And that's all because we don't know 155 00:07:10,900 --> 00:07:14,540 what the EUV flux of the star is today. 156 00:07:14,540 --> 00:07:19,540 So with that in mind, we designed the ESCAPE mission 157 00:07:19,690 --> 00:07:22,890 to go out and characterize this question. 158 00:07:22,890 --> 00:07:25,993 And with three big objectives, next slide please. 159 00:07:29,470 --> 00:07:30,920 Oh, Christy frozen to me, 160 00:07:30,920 --> 00:07:34,000 I'm so not used to running my own thing. 161 00:07:34,000 --> 00:07:35,610 I forget to include it in the slide. 162 00:07:35,610 --> 00:07:37,990 All right, the other thing that we need to know is, 163 00:07:37,990 --> 00:07:40,400 what's the time variability of those sources? 164 00:07:40,400 --> 00:07:44,630 We know from Hubble observations of in stars 165 00:07:44,630 --> 00:07:48,400 that flares may actually dominate the total UV, 166 00:07:48,400 --> 00:07:51,410 a far UV, a near UV output of those stars. 167 00:07:51,410 --> 00:07:53,820 So understanding the time variability, 168 00:07:53,820 --> 00:07:56,460 particularly in flares is really important. 169 00:07:56,460 --> 00:08:00,710 Also flares and coronal mass ejections are counted 170 00:08:00,710 --> 00:08:04,670 sort of the in the time variable category there. 171 00:08:04,670 --> 00:08:07,090 And so we would really like to know, 172 00:08:07,090 --> 00:08:10,890 the characteristics of the CMEs from these stars. 173 00:08:10,890 --> 00:08:12,860 And I'll say a little bit more about that, 174 00:08:12,860 --> 00:08:15,980 as I get to the second half of the talk. 175 00:08:15,980 --> 00:08:18,970 So now I think we're ready to see the ESCAPE's 176 00:08:18,970 --> 00:08:20,470 primary science objective. 177 00:08:20,470 --> 00:08:21,770 Thanks. 178 00:08:21,770 --> 00:08:23,730 So we wanna determine if Stellar radiation 179 00:08:23,730 --> 00:08:26,060 environments permit habitable conditions 180 00:08:26,060 --> 00:08:27,730 to exist on Rocky exoplanets. 181 00:08:27,730 --> 00:08:29,460 Of course there's an interpretation 182 00:08:29,460 --> 00:08:31,280 and modeling component that goes into that. 183 00:08:31,280 --> 00:08:33,470 I'll mention that in a second. 184 00:08:33,470 --> 00:08:35,313 Second, next slide, please. 185 00:08:38,200 --> 00:08:41,040 We'd like to characterize the EUV evolution, 186 00:08:41,040 --> 00:08:43,450 both short term with flares, 187 00:08:43,450 --> 00:08:45,170 but also longterm evolution. 188 00:08:45,170 --> 00:08:48,000 So by studying stars that are very young, 189 00:08:48,000 --> 00:08:50,490 a few tens of millions of years out to, 190 00:08:50,490 --> 00:08:52,080 several big years. 191 00:08:52,080 --> 00:08:53,960 And then again what is the longterm 192 00:08:53,960 --> 00:08:55,980 radiation environment suggest 193 00:08:55,980 --> 00:08:58,310 for the survivability of those atmospheres? 194 00:08:58,310 --> 00:09:00,380 And then three, thank you. 195 00:09:00,380 --> 00:09:01,960 Finally determine, 196 00:09:01,960 --> 00:09:04,570 A do other stars even have coronal mass ejections? 197 00:09:04,570 --> 00:09:06,140 That's an open question right now, 198 00:09:06,140 --> 00:09:08,270 and then if they do what are the impacts 199 00:09:08,270 --> 00:09:10,360 for exo planetary space weather 200 00:09:10,360 --> 00:09:12,553 and an atmospheric mass loss. 201 00:09:13,580 --> 00:09:15,590 Okay, thanks next slide please. 202 00:09:15,590 --> 00:09:18,490 So with that motivation in mind, 203 00:09:18,490 --> 00:09:20,600 we designed the concept for ESCAPE, 204 00:09:20,600 --> 00:09:24,660 to be an Extreme UV and Far UV spectrograph. 205 00:09:24,660 --> 00:09:27,800 That covers about seven to 180 nanometers, 206 00:09:27,800 --> 00:09:29,360 and in a two year mission, 207 00:09:29,360 --> 00:09:32,300 we'll study 200 nearby stars, 208 00:09:32,300 --> 00:09:35,740 including the most promising exoplanet candidates, 209 00:09:35,740 --> 00:09:39,429 exoplanet host star candidates that we can reach. 210 00:09:39,429 --> 00:09:41,740 So depending on the spectral type 211 00:09:41,740 --> 00:09:45,210 that typically means stars inside of 50 parsecs, 212 00:09:45,210 --> 00:09:47,640 but for say bright G or F stars, 213 00:09:47,640 --> 00:09:49,470 we can go further than that. 214 00:09:49,470 --> 00:09:52,810 And then we use a series of atmospheric ESCAPE models 215 00:09:52,810 --> 00:09:55,880 to understand the primary mass loss channels 216 00:09:55,880 --> 00:09:59,070 and estimate the longterm stability 217 00:09:59,070 --> 00:10:01,423 of those atmospheres over geologic timescales. 218 00:10:02,490 --> 00:10:04,110 Next slide please. 219 00:10:04,110 --> 00:10:06,960 And we do this with, it's like a two year mission 220 00:10:06,960 --> 00:10:11,040 and we anticipate launching sometime in Spring of 2025. 221 00:10:13,042 --> 00:10:14,880 Okay, next slide please. 222 00:10:14,880 --> 00:10:16,430 So let me just tell you in a little more detail 223 00:10:16,430 --> 00:10:18,620 about the ESCAPE Science Program. 224 00:10:18,620 --> 00:10:19,670 I wanna emphasize 225 00:10:19,670 --> 00:10:22,140 that we're still in the competition sensitive phase 226 00:10:22,140 --> 00:10:22,973 of this process. 227 00:10:22,973 --> 00:10:24,980 So I'm gonna be a little light on technical 228 00:10:24,980 --> 00:10:27,840 and modeling details I'm just kinda give you the high level, 229 00:10:27,840 --> 00:10:29,180 here's what we're going to do. 230 00:10:29,180 --> 00:10:32,840 But I'm happy to talk about details as possible 231 00:10:32,840 --> 00:10:35,240 if you've got questions. 232 00:10:35,240 --> 00:10:37,830 So the plot on the left here shows the effective area. 233 00:10:37,830 --> 00:10:40,470 This is sort of another way of saying sensitivity 234 00:10:40,470 --> 00:10:42,170 of ESCAPE versus previous missions 235 00:10:42,170 --> 00:10:45,280 that have operated in the Extreme UV band. 236 00:10:45,280 --> 00:10:48,340 The only major UV is the EUV astronomy mission 237 00:10:48,340 --> 00:10:50,840 of the NASA's flown prior 238 00:10:50,840 --> 00:10:53,517 to ESCAPE was the EUV mission in the 90s. 239 00:10:53,517 --> 00:10:56,440 And we have roughly a factor of a hundred time 240 00:10:56,440 --> 00:10:59,700 of the sensitivity of EUV across the band. 241 00:10:59,700 --> 00:11:01,430 So you can see the effect of that, 242 00:11:01,430 --> 00:11:02,690 looking at the plot on the right 243 00:11:02,690 --> 00:11:05,670 there's a simulated spectrum of prox Cen, 244 00:11:05,670 --> 00:11:08,080 based on differential emission measure calculations 245 00:11:08,080 --> 00:11:10,940 that we would expect to see with ESCAPE shown in black. 246 00:11:10,940 --> 00:11:15,793 And then green is the actual EUV observation of prox Cen. 247 00:11:15,793 --> 00:11:20,793 That was about 77 kilo seconds taken in 1994 or so. 248 00:11:20,810 --> 00:11:23,510 And you see that there's maybe one 249 00:11:23,510 --> 00:11:25,700 or two spectral features that are detected, 250 00:11:25,700 --> 00:11:28,380 but essentially the signal to noise was too low, 251 00:11:28,380 --> 00:11:30,340 even in almost a hundred kilo seconds 252 00:11:30,340 --> 00:11:32,400 of observing time to do anything. 253 00:11:32,400 --> 00:11:36,760 And then again that's what we expect to see with ESCAPE. 254 00:11:36,760 --> 00:11:39,550 And I wanna emphasize that this prox Cen is nearby, 255 00:11:39,550 --> 00:11:41,160 but it's not a particularly bright target. 256 00:11:41,160 --> 00:11:43,410 Thank you, go ahead and go to the next thing. 257 00:11:45,870 --> 00:11:47,190 Thanks. 258 00:11:47,190 --> 00:11:49,460 So we're also interested when we have that type 259 00:11:49,460 --> 00:11:50,293 of sensitivity. 260 00:11:50,293 --> 00:11:52,480 We wanna understand the time variability, 261 00:11:52,480 --> 00:11:54,970 both on evolutionary timescales, 262 00:11:54,970 --> 00:11:59,040 and we will monitor stars for rotational timescales, 263 00:11:59,040 --> 00:12:01,670 as well as flares, which I talked about already. 264 00:12:01,670 --> 00:12:05,290 The plot on the left kinda tells the evolutionary story. 265 00:12:05,290 --> 00:12:08,110 There's sort of a lot going on in this plot. 266 00:12:08,110 --> 00:12:09,040 People find that bad. 267 00:12:09,040 --> 00:12:12,990 I think information rich plot can be rather gratifying. 268 00:12:12,990 --> 00:12:14,660 So this essentially shows the age 269 00:12:14,660 --> 00:12:16,330 of the star on the X-axis 270 00:12:16,330 --> 00:12:20,210 and it's estimated EUV luminosity on the Y-axis. 271 00:12:20,210 --> 00:12:23,000 And then the points are color coded based 272 00:12:23,000 --> 00:12:24,610 on the spectral type of the star 273 00:12:24,610 --> 00:12:26,970 and sized based on the expected signal 274 00:12:26,970 --> 00:12:29,850 to noise in a particular EUV tracer. 275 00:12:29,850 --> 00:12:33,510 So what you see is that with a nominal 200 star mission, 276 00:12:33,510 --> 00:12:36,230 we do a pretty good job of filling out, 277 00:12:36,230 --> 00:12:41,120 the spectral type and age, parameter space. 278 00:12:41,120 --> 00:12:45,330 So we to expect to be able to tell the evolutionary history 279 00:12:45,330 --> 00:12:47,690 of a particular type of star, 280 00:12:47,690 --> 00:12:50,580 from essentially just after the pre main sequence phase 281 00:12:50,580 --> 00:12:52,700 or for in stars even into the the end 282 00:12:52,700 --> 00:12:57,050 of the pre main sequence phase out into the main sequence 283 00:12:57,050 --> 00:12:58,953 and the late main sequence phase. 284 00:12:59,830 --> 00:13:01,670 And then we also have - [Woman] Can we remember that 285 00:13:01,670 --> 00:13:03,210 Just a few minutes. 286 00:13:03,210 --> 00:13:04,410 - [Kevin] Thank you very much. 287 00:13:04,410 --> 00:13:07,710 We also have sensitivity to do a flare analysis. 288 00:13:07,710 --> 00:13:09,190 Next slide. 289 00:13:09,190 --> 00:13:11,870 One of the things that is really unique 290 00:13:11,870 --> 00:13:13,910 to the ESCAPE approach is the ability 291 00:13:13,910 --> 00:13:16,870 to probe Stellar CMEs. 292 00:13:16,870 --> 00:13:18,580 We do this with techniques 293 00:13:18,580 --> 00:13:22,330 that have been used with sun as a star observations from, 294 00:13:22,330 --> 00:13:24,670 FTO EVE called coronal dimming, 295 00:13:24,670 --> 00:13:27,250 essentially when there's a big flare that goes off, 296 00:13:27,250 --> 00:13:29,670 it blows material out of the corona. 297 00:13:29,670 --> 00:13:33,530 And so you see, and that material is what becomes the CME 298 00:13:33,530 --> 00:13:36,600 and you see that as a dimming in the light curve. 299 00:13:36,600 --> 00:13:38,650 And so what we propose to do is to be able 300 00:13:38,650 --> 00:13:39,520 to actually carry out 301 00:13:39,520 --> 00:13:42,370 this experiment on other stars for the first time. 302 00:13:42,370 --> 00:13:44,170 And not only answer the question, 303 00:13:44,170 --> 00:13:45,560 Do other stars have CMEs, 304 00:13:45,560 --> 00:13:48,540 but what are their mass velocity's kinetic energies 305 00:13:48,540 --> 00:13:51,093 and then estimate the impact on planets. 306 00:13:52,024 --> 00:13:53,523 Okay, next slide please. 307 00:13:55,910 --> 00:13:57,060 Thank you, 308 00:13:57,060 --> 00:13:58,280 I'll speak about this briefly. 309 00:13:58,280 --> 00:14:00,760 This is the mission layout. 310 00:14:00,760 --> 00:14:04,140 So we have partners that have essentially developed parts 311 00:14:04,140 --> 00:14:06,660 of this technology previously, 312 00:14:06,660 --> 00:14:09,880 ESCAPE uses three shell grazing incidents telescope. 313 00:14:09,880 --> 00:14:12,850 It's about 42 centimeters in diameter. 314 00:14:12,850 --> 00:14:14,680 That telescope is built 315 00:14:14,680 --> 00:14:16,130 at Marshall Space Flight Center using 316 00:14:16,130 --> 00:14:17,660 their grazing incidents heritage, 317 00:14:17,660 --> 00:14:19,970 and with alignment done through the, 318 00:14:19,970 --> 00:14:21,937 with the experts at SAO. 319 00:14:23,110 --> 00:14:25,790 We have contributions from Penn State 320 00:14:25,790 --> 00:14:28,180 and Berkeley in the gratings and detector 321 00:14:28,180 --> 00:14:32,760 and Ball Aerospace provides the spacecraft. 322 00:14:32,760 --> 00:14:36,050 So this actually looks functionally similar 323 00:14:36,050 --> 00:14:39,080 to the arrangement that is currently being developed 324 00:14:39,080 --> 00:14:41,800 for the XB small Explorer, 325 00:14:41,800 --> 00:14:44,760 a lot of the same partners doing a lot of the same things. 326 00:14:44,760 --> 00:14:46,720 So a lot of this technology 327 00:14:46,720 --> 00:14:49,140 is basically been developed as part 328 00:14:49,140 --> 00:14:52,910 of strategic astrophysics technology programs tested 329 00:14:52,910 --> 00:14:53,880 on founding rockets. 330 00:14:53,880 --> 00:14:56,910 And some of it is actually in the critical technology path 331 00:14:56,910 --> 00:14:58,500 for Luvin Habak. 332 00:14:58,500 --> 00:15:01,500 So it's, for somebody who's been working in suborbital 333 00:15:01,500 --> 00:15:02,333 for a long time, 334 00:15:02,333 --> 00:15:05,310 it's really nice to see all these things come together. 335 00:15:05,310 --> 00:15:06,513 Okay, next slide. 336 00:15:09,950 --> 00:15:11,253 Right, and I'll just, 337 00:15:12,130 --> 00:15:15,160 I already mentioned about the Ball spacecraft, 338 00:15:15,160 --> 00:15:17,320 so, we'll just go ahead 339 00:15:17,320 --> 00:15:18,830 and since I'm running out of time here, 340 00:15:18,830 --> 00:15:21,483 I'll move on to the conclusion. 341 00:15:23,760 --> 00:15:25,560 So this is the take home 342 00:15:25,560 --> 00:15:27,310 here is the ESCAPE explores 343 00:15:27,310 --> 00:15:29,160 the high energy radiation environment 344 00:15:29,160 --> 00:15:32,380 and habitable zones of nearby stars. 345 00:15:32,380 --> 00:15:33,213 Next slide. 346 00:15:35,610 --> 00:15:39,620 This is the essential Stellar context for understanding 347 00:15:39,620 --> 00:15:41,460 which planets can maintain atmospheres 348 00:15:41,460 --> 00:15:43,540 on geologic timescales. 349 00:15:43,540 --> 00:15:46,190 We hope this will be able to feed back, 350 00:15:46,190 --> 00:15:49,230 and serve as a roadmap for where we put our investments 351 00:15:49,230 --> 00:15:51,470 and future life detection missions. 352 00:15:51,470 --> 00:15:53,390 And then the ESCAPE instrument is, 353 00:15:53,390 --> 00:15:55,150 a high sensitivity grazing incidents, 354 00:15:55,150 --> 00:15:58,170 optical system that we believe is a low risk, 355 00:15:58,170 --> 00:16:00,380 high heritage implementation. 356 00:16:00,380 --> 00:16:02,953 And we plan to observe 200 nearby stars, 357 00:16:03,880 --> 00:16:04,940 in a two year mission. 358 00:16:04,940 --> 00:16:07,033 So happy to take any questions, thanks. 359 00:16:08,808 --> 00:16:11,360 - [Woman] Awesome thank you, Kevin. 360 00:16:11,360 --> 00:16:12,193 We have two quick questions. 361 00:16:12,193 --> 00:16:14,930 The first is regarding the target list 362 00:16:14,930 --> 00:16:16,420 and whether or not your list of, 363 00:16:16,420 --> 00:16:18,763 to make your targets will be fit for launch. 364 00:16:20,040 --> 00:16:21,250 - [Kevin] No good question. 365 00:16:21,250 --> 00:16:25,240 So we have a 200 target list 200 star target list right now 366 00:16:25,240 --> 00:16:26,890 that meets the mission requirements, 367 00:16:26,890 --> 00:16:30,650 but the plan is to continue to update that 368 00:16:30,650 --> 00:16:32,670 with results from tests 369 00:16:32,670 --> 00:16:35,873 and JWST and CABS and stuff as they become available. 370 00:16:36,929 --> 00:16:40,410 - [Woman] Awesome, the next question is, 371 00:16:40,410 --> 00:16:43,080 will ESCAPE target other astrophysical sources 372 00:16:43,080 --> 00:16:45,179 in the EUV as well? 373 00:16:45,179 --> 00:16:48,230 - [Kevin] Yeah, there actually some interesting, 374 00:16:48,230 --> 00:16:50,700 science applications within exoplanet science. 375 00:16:50,700 --> 00:16:54,430 So we did some calculations with David Aaron Rishon, 376 00:16:54,430 --> 00:16:58,190 Vincent Borie as part of the step one proposal, 377 00:16:58,190 --> 00:17:02,290 looking at neutral helium transits of nearby stars. 378 00:17:02,290 --> 00:17:03,360 And, you know, everybody loves 379 00:17:03,360 --> 00:17:06,180 the metal stable helium line now. 380 00:17:06,180 --> 00:17:08,930 But you can actually access the resonant transitions 381 00:17:08,930 --> 00:17:11,610 for those neutral helium in the EUV 382 00:17:11,610 --> 00:17:13,700 and for a handful of stars, 383 00:17:13,700 --> 00:17:14,570 they actually found that, 384 00:17:14,570 --> 00:17:17,280 that you could do a pretty significant transit work, 385 00:17:17,280 --> 00:17:18,560 with ESCAPE. 386 00:17:18,560 --> 00:17:20,160 We will also do other things I mean, 387 00:17:20,160 --> 00:17:21,580 ESCAPE is gonna study these stars. 388 00:17:21,580 --> 00:17:23,940 So there's a whole wealth of star planet, 389 00:17:23,940 --> 00:17:25,820 you know, solar star connection, 390 00:17:25,820 --> 00:17:27,560 astrophysics to be done. 391 00:17:27,560 --> 00:17:29,550 And there's also we'll also be able 392 00:17:29,550 --> 00:17:32,470 to look through certain holes in the interstellar medium 393 00:17:32,470 --> 00:17:33,800 at Quasars. 394 00:17:33,800 --> 00:17:36,234 But we haven't done a whole lot of work on, 395 00:17:36,234 --> 00:17:37,984 setting up those science cases yet.