00:13:36.242,00:13:39.242 Barbara Thompson: We need an annual SPD award for best paper title. Hughes et al. (2023) would be a good candidate 00:17:51.158,00:17:54.158 Barbara Thompson: If you're going to be at the AMS meeting next week come see PUNCH team members from 9am-12 pm Wednesday at the NASA booth. 00:18:29.270,00:18:32.270 Sarah Gibson: Here is the web page with agenda for today's meeting: https://punch.space.swri.edu/punchwintertelecon2024.php 00:19:21.872,00:19:24.872 Craig DeForest: Thanks, Barbara! 00:35:00.542,00:35:03.542 Craig DeForest: I'm intrigued but holding my questions for the discussion 00:35:02.795,00:35:05.795 Craig DeForest: Nice talk, Sam! 00:35:02.998,00:35:05.998 Sarah Gibson: Afternoon east coast-- still morning to the west! 00:35:28.269,00:35:31.269 Samuel Badman: thanks everyone - you can see my slides here: https://docs.google.com/presentation/d/1YF4genrrIdk6LXFnnxIe77NEpMxeJjZLRZ-i4Xqkv7I/edit#slide=id.p 00:35:32.032,00:35:35.032 Sarah Gibson: Agenda: https://punch.space.swri.edu/punchwintertelecon2024.php 00:43:40.783,00:43:43.783 Heather Elliott: Thanks Sam B. 00:50:51.139,00:50:54.139 Raphael Attie: We can discuss the non-radial flow tracking during the discussion. I can comment on that. 00:50:57.027,00:51:00.027 Craig DeForest: cool! 00:51:27.867,00:51:30.867 Craig DeForest: Really great talk, Sam. 00:51:47.291,00:51:50.291 Samantha Wallace: Great! Yes! I wasnt sure what would be possible with PUNCH, but wanted to at least mention that we had done this in the past when we had fortuitous spacecraft alignment, and with some assumptions :) 00:52:56.303,00:52:59.303 Raphael Attie: Excellent. Have you published anything specific to tracking non-radial flow? If so, can you email to me the reference? I can include it in the review paper we're working on. 00:53:32.308,00:53:35.308 Raphael Attie: (besides what Naty did, which I'm aware of) 00:54:47.634,00:54:50.634 Heather Elliott: Thanks Samantha. 01:00:55.327,01:00:58.327 Samantha Wallace: @Raphael I have not published anything on that subject. Question for you though, how far out from the Sun will the radial outflow speed maps extend? It looked like in Craig's data prodcut slide that they would extend out to 10 Rs? Will they extend farther out? 01:04:30.362,01:04:33.362 Raphael Attie: Yes. Current capibilities and flow tracking with STEREO COR2 shows we can go to at least 15 Rs. With PUNCH, we'll go even beyond that. 01:04:31.714,01:04:34.714 Craig DeForest: We should be able to produce correlation maps and/or small-feature tracking out to 80 Rs 01:04:54.705,01:04:57.705 Craig DeForest: I hope 01:05:47.658,01:05:50.658 Raphael Attie: We can provide more details during the discussion if you want. 01:06:31.785,01:06:34.785 Sarah Gibson: And for those who just joined we will also be having an extensive open discussion with all the speakers after the break 01:06:44.466,01:06:47.466 Bernard Jackson: Craig this is just the plane of sky location. The distance is different. 01:07:14.351,01:07:17.351 Heather Elliott: Thank you Yeimy. 01:07:43.753,01:07:46.753 Craig DeForest: A topic for the discussion session, stimulated by Yeimy's thought-provoking talk: are there textural or other cues we should be looking for, as proxies for not-detectable-to-PUNCH quantities such as squashing factor (Sam W) or origin/FIP/release-mechanism (Yeimy) 01:07:54.977,01:07:57.977 Craig DeForest: Good point Bernie 01:08:33.770,01:08:36.770 Craig DeForest: Thanks for the great talk Yeimy. 01:13:33.100,01:13:36.100 Craig DeForest: A reminder for newcomers: we're taking only very brief clarification questions during the talks -- but do keep notes as there is an extensive open discussion still to come. 01:14:02.039,01:14:05.039 Craig DeForest: Also: this videocon is being recorder, along with the chat. 01:14:14.640,01:14:17.640 David Webb: With SMEI data we found a strong correlation between shock arrival (ESPs) at Earth and sudden brightening in the SMEI cameras. Also related to the high altitude aurorae that SMEI "discovered". The PUNCH WFIs will see these brightenings. 01:15:04.241,01:15:07.241 Heather Elliott: Thanks Dave that is important to know. 01:15:11.110,01:15:14.110 Craig DeForest: Agreed 01:18:09.553,01:18:12.553 Heather Elliott: That is a very strong correlation for this field often correlations people try are much lower. ' 01:21:34.001,01:21:37.001 Craig DeForest: Thanks, Maher! 01:35:38.683,01:35:41.683 David Webb: Great talk, Chris! 01:35:51.342,01:35:54.342 Craig DeForest: Chris, thank you. 01:35:56.092,01:35:59.092 Sarah Gibson: go ahead and put questions in chat for now -and we will go back to them in the discussion too 01:39:39.254,01:39:42.254 Craig DeForest: Chris, of course tracking CMEs in 3D is something we definitely want to do. Your talk reminded me that there are still questions about what, exactly, we see in Thomson scattered light around large events. For fast events, e.g., there's always a question about how much of the bright ICME structure is material swept-up enroute, vs. how much is the erupting flux rope itself. 01:41:40.407,01:41:43.407 Anna Malanushenko: Craig, for sure the brightest matter which we normally perceive as edge of the CME (shock/sheath?) has chirality not related to that of the CME itself 01:42:12.939,01:42:15.939 Volker Bothmer: Apologies, I have to leave shortly for a public lecture on the PSP mission. Have a great discussion 01:42:18.659,01:42:21.659 Christian Moestl: Yes it would be great also to see whether we can identify features that tell us whether this is a right or left handed, low or high inclination CME. Pristine events observed by PSP could also help here to distinguish between original vs swept up material 01:43:08.484,01:43:11.484 Craig DeForest: Anna and Chris: agreed! 01:44:11.664,01:44:14.664 Christian Moestl: Anna: even the sheath material if it envelops the flux rope could tells us the shape of the flux rope, and that might give us info whether its low or high inclination 01:49:42.240,01:49:45.240 Olga Panasenco: On CME's chirality: Here, in Advanced Heliophysics Inc., we developed a vey robust technique based on a few different approaches, which allows to predict CME chirality well before eruptions. We study the potential cites of eruptions and track them for a few solar rotations. Also, we studied how to predict non-radial eruptions, based on the modeling of the magnetic environment around the possible eruption cite. Please, contact me if interested. panasenco.olga@gmail.com 01:49:55.378,01:49:58.378 Craig DeForest: Also it is possible to distinguish the sheath from the core in many images 01:50:28.051,01:50:31.051 Craig DeForest: Olivier: thank you! I'm looking forward to JUICE collaborations 01:50:43.396,01:50:46.396 Olivier Witasse: me too:-) 01:50:45.048,01:50:48.048 Heather Elliott: Thanks to all our guest speakers!!