09:31:12 From Moderator (KITPModthree) to Everyone:
	Hi all on Zoom, same as yesterday please feel free to unmute and chime in, or write them directly in the chat and I’ll read them out. Either’s fine.
09:38:23 From Falk Herwig to Everyone:
	Thanks for zooming in!
09:42:59 From Pascale Garaud to Everyone:
	Does the damping scale comes from purely radiative damping or are there other assumptions in that formula?
09:49:49 From Falk Herwig to Everyone:
	Daniel, could you put the two types of simulations that disagree in their spectra in this chat, or on slack?
09:53:29 From Moderator (KITPModthree) to Everyone:
	Hi Falk — this is Daniel… Example of wave spectrum from simulations that I work on: https://arxiv.org/pdf/1808.04638.pdf . We find E(om, ell) ~ ell^4 om^(-13/2). We find that we get similar spectra in spherical core convection simulations as well.
09:56:19 From Moderator (KITPModthree) to Everyone:
	Other group is Tami Rogers, which find E(om, ell) which decays with ell, and has a much shallower dependence on om… Maybe om^-2 or so? Typical results include 2D sims (https://ui.adsabs.harvard.edu/abs/2013ApJ...772...21R/abstract) and more recent 3D sims (https://ui.adsabs.harvard.edu/abs/2019ApJ...876....4E/abstract). Though note that the 3D simulations now have steeper frequency spectra
09:57:32 From Falk Herwig to Everyone:
	Difficult to hear comments from audience
09:57:35 From Falk Herwig to Everyone:
	thanks
09:58:00 From Moderator (KITPModthree) to Everyone:
	I’m happy to chat more about this offline. I have some ideas about what the differences might be…
09:59:30 From Pascale Garaud to Everyone:
	Could the “in-room” speakers say their names? It would help identify who’s talking. (some of them I can guess bit not always). Thanks!
10:00:03 From Moderator (KITPModthree) to Everyone:
	Thanks for the suggestion Pascale
10:02:05 From Pascale Garaud to Everyone:
	Breakdown of thermal wind balance can be interpreted as local ES flows
10:02:25 From Pascale Garaud to Everyone:
	sorry, I mean drives local ES flows.
10:04:13 From Pascale Garaud to Everyone:
	Actually I take that back - it’s more complicated.
10:05:46 From Falk Herwig to Everyone:
	What are people thinking about how IGWs and ES would interact? What is the relative energy content of these processes, as far as we can now?
10:08:45 From Moderator (KITPModthree) to Everyone:
	Interesting question Falk… Let’s wait until after J-transport section, and I’ll raise the question for discussion
10:14:17 From Pascale Garaud to Everyone:
	Maybe here is a better way of saying it. Breakdown of thermal wind balance is restored by rapid dynamics (e.g. gravity waves, baroclinic instabilities, etc.) — just like breakdown of hydrostatic is rapidly restored by pressure waves. So thermal wind balance is usually satisfied in stars that are in quasi-steady equilibrium (i,e. on long timescales). Meridional flows therefore have to be consistent with thermal wind balance AND energy balance which means they HAVE to have an amplitude that is essentially that of local Eddington Sweet velocity (but with a length-scale associated with the scale of the differential rotation). That’s of course all a non-magnetic argument.
10:15:37 From Pascale Garaud to Everyone:
	Sorry for the confusion, I just hadn’t thought about this particular problem for a long time.
10:16:43 From Moderator (KITPModthree) to Everyone:
	Thanks for that explanation — maybe you can share this when we get to questions at the end of the talk
10:17:21 From Pascale Garaud to Everyone:
	Mmm, but is it really that important ? :-)
10:17:50 From Moderator (KITPModthree) to Everyone:
	Up to you :)
10:39:27 From Pascale Garaud to Everyone:
	Is there a schedule for coming week?