13:23:49 From Ian Cohen (he/him) : You need another screen/monitor Drew! 13:28:36 From Allison Jaynes (she/her) : Set up your powerpoint show as “Browsed by an individual”! You can move it around and see your whole screen, but everyone else just sees your slides. 13:29:08 From Drew Turner : Yea, I’ve been working on a single laptop screen for over a year now… “joys” of home office work right there 13:35:21 From Shan Wang : @Drew Turner: I might have missed, but what is evidence/indication for Fermi acceleration? magnetic field curvature? 13:40:13 From Drew Turner : Hi Shan, the evidence has to do with the extremely energy- and location- dependent agyrotropic distributions observed by multipoint MMS observations within 1-electron-gyroradius of one another. That is known to be a signature of Fermi reflection acceleration for energetic ions reflecting off of depolarization fronts (for which the relative gyroraidus to curvature, time and velocity scales are all analogous compared to these energetic electrons within the IDR in the exhaust of Rx) 13:40:56 From Drew Turner : E.g., see Delcourt et al. [JGR 1997] 13:44:31 From Shan Wang : Thanks! It helps, and I see that it has some differences from the Fermi acceleration for magnetized electrons bouncing along field lines. 13:46:29 From M. Hasan Barbhuiya : @Drew Turner, Hi. In the region where you see electron remagnetization, what do the electron velocity distributions look like? 13:52:42 From Ian Cohen (he/him) : @Jim D - please reach out, the EPD team would be happy to help in your data-model comaprisons! 13:54:55 From Drew Turner : YES! Please do Jim.. it would be fantastic to work with you guys on this, and I think the data are there to explore! 13:56:03 From Drew Turner : Hi Hasan: the distributions are quite chaotic (agyrotropic, messy PADs, strong energy and location dependencies), which is what got us looking at those cases in the first place. 13:56:09 From Geoff Reeves : The EDRs might be a good place to start in part because the quiet crossings might “mix” different source regions at different energies. 13:59:10 From Drew Turner : Shan: yes, we are talking different forms of Fermi acceleration; the Fermi reflections are particles bouncing off of a (large momentum) magnetic “wall”, while there is also Fermi acceleration between converging “walls” or mirror points or changing field line lengths (compressing islands) 14:02:30 From James F. Drake : Back to the question about diagnosing acceleration from remote sites. One might also look to see if the hot thermal electrons can be represented by multiple temperatures. The remote site might produce a quite hot thermal component that differs from the local electron temperature. 14:42:35 From Allison Jaynes (she/her) : Can you go to slideshow mode, Trevor? 15:01:18 From rumi nakamura : Jim, Drew: This is a Cluster paper where we interpret the acceleation at the Exhaust scattered electrons (although no waves analysis) : Imada et al. https://doi.org/10.1029/2006JA011847 15:01:31 From Drew Turner : Thanks, Rumi! 15:02:07 From Drew Turner : And yes, Jim: in addition to Allison’s work here, see the latest from Rick Wilder, who has been diving in to these electron whistler-mode waves associated with Rx events 15:02:30 From Lynn Wilson : We did look at outer magnetospheric whistlers in this too, but the maximum KE we could get from Omura's relativistic turning acceleration was something absurd like 70 MeV: https://ui.adsabs.harvard.edu/abs/2011GeoRL..3817107W/abstract 15:02:45 From Drew Turner : Thanks, Lynn! 15:03:32 From Lynn Wilson : We even noticed differences in the electron VDFs below ~30 keV associated with differences in the whistler properties, but that stuff was scratched in the GRL (only remained in the arXiv version). 15:09:01 From Lynn Wilson : Cool stuff Allison! 15:09:02 From Sanjay Chepuri : I think that poster Allison was talking about was by Seung Choi 15:09:12 From Allison Jaynes (she/her) : Yes, thank you, Sanjay!