03:20:14	Kris Pritchard:	the screen is little
03:20:35	Ian Cohen (he/him):	Here’s the Gather.Town link for our poster and social session tomorrow afternoon: https://gather.town/app/d1SPh85HWcBqWiew/SpringMMSSWT
03:20:46	Ian Cohen (he/him):	I’m seeing it full screen Kris
03:21:30	Kris Pritchard:	I figured it out
03:41:45	Patricia Reiff:	I have a question
03:41:48	Kristie LLera:	Rumi, can you quickly show the second to last slide, the cold population with MMS
03:42:29	Kristie LLera:	Rumi: you’re not currently sharing your screen
03:42:35	Patricia Reiff:	My estimated polar cap potential is 100 KV which is not small
03:48:18	rumi nakamura:	Good to know Patt. I hoped it should be huge.
03:49:21	rumi nakamura:	Kristie, sorry I just saw your comment. My talk is uploaded...fyi
04:04:35	Christine Gabrielse:	Craig: I know the science objectives are cusp science, but just curious if TRACERS will be sampling the nightside auroral oval as well?
04:16:53	Frederick Wilder:	Is it that there’s not a lot of convection, or just not a lot of backscatter to the radars?
04:17:43	Sarah Vines:	A bit of both, I think Rick - I haven’t looked at the SuperDARN plots in detail, but coverage is always interesting… But at least in AMPERE, it’s just pretty weak in general
04:23:18	Mojtaba Akhavan-Tafti:	Kevin: Have you studied the magnetic curvature (kappa) of the “thinning” current sheet?
04:30:03	Kevin Genestreti:	@Rick – that’s a good question. Probably shows that there’s just not much convection. I say probably because that’s what we’d expect given the THEMIS magnetopause data (weak/no jets) and the MMS tail data (no pressure growth). We also see weak convection in a Global MHD run
04:31:56	Kevin Genestreti:	@Mojtaba – indeed! Kappa was of order ~1 for the whole thinning interval, so it’s consistent with our assertion that PA scattering is happening
04:34:13	Shan Wang:	@Kevin, current sheet thinning v.s. thermal pressure loss, which one is the cause?
04:41:00	Kevin Genestreti:	Hi @Shan. Good question! We can see that there was some initial thinning that was spurred by the first solar wind-driven compression of the tail, and that kickstarted the precipitation. Our simple argument is that — if the plasma sheet looses thermal energy – then it has to reduce in volume to maintain vertical pressure balance. The thinning & precipitation happen in lock step with one another after the compression
04:43:22	Shan Wang:	That's reasonable, and cool! Thanks.
04:56:18	Lynn Wilson:	Was Wind far on the ±Y-GSE extent of it's orbit about L1 for this event studied by Blake et al.?
04:58:49	Lynn Wilson:	I moved it to Slack
04:59:05	Rachael Filwett:	https://docs.google.com/document/d/1TFw7_saoPCzxylBqQSlK6z_AjzV1eAAocZWEvSjTK70/edit?usp=sharing
05:01:16	Kristie LLera:	only host/co-host
05:01:26	Lynn Wilson:	Does this work for the web-based version?
05:01:34	Kristie LLera:	a host/co-host has to assign us
05:03:33	Ian Cohen (he/him):	SW: 1&2
05:03:34	Alexandra Alexandrova:	could you please type names of the rooms again?
05:03:44	Ian Cohen (he/him):	MI Coupling: 3&4
05:03:56	Ian Cohen (he/him):	Inner Mag: 5&6
05:04:11	Ian Cohen (he/him):	Outer Mag Tail: 7&8
05:04:20	Ian Cohen (he/him):	Outer Mag Dayside: 9&10
05:06:14	Brandon Burkholder:	please put me in SW2
05:06:18	Guan Le:	MI Coupling please
05:06:33	Naoki Bessho:	Magnetotail please
05:06:37	trevor:	Hi Ian,  Could you put me in a good room?  I’m not having any success…  Thanks!  Trevor
05:06:55	Martin Hosner:	Can i go into outer mag: Tail, please? Thank You!
05:07:37	Leslie Garrison:	Ian, Im waiting tti be placed in a breakout room, too.
05:33:35	Kevin Genestreti:	Thanks organizers
05:33:53	Akhtar Ardakani (she/her):	Thanks!