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[Music]

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laura1 thank you for giving me the

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opportunity to present at this great

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conference so I work on the simulations

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of moist convection on rocky travelogue

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planets and this is work I've been doing

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with Google on roads and next man at the

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University and also in vertol at the UK

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Met Office so today I'm gonna remind you

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what the circulation looks like on a

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title locked rocky exoplanets I'm going

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to show you some what how important the

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dayside convection is for the global

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climate of these planets I'll talk

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briefly about some challenges in

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modeling convection in terrestrial

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atmospheres and also show you some

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exciting results of convection resolving

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experience

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so what planets

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I've been looking so far these are

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well-known terrestrial exoplanets namely

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Trappist 1e and chakras 1f but also

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Proxima Centauri and as you can see from

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this table in terms of their orbital and

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[Music]

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size characteristics they're fairly

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close to each other but they do vary in

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terms of their rotation period and of

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course sharvani receives more radiation

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than epsilon F while Proxima B is quite

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close in this regard and so for this

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simulations I just assume for now and

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that's like atmosphere which is nitrogen

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dominated with water as main condensable

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species and I ran this as an a-cup liner

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simulation with a slab ocean at the

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bottom so imagine this rocky exoplanets

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orbiting an M dwarf we can imagine the

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represent the circulation on such a

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planet using a static so this is a

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vertical cross section along the equator

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on this planet and you have the solar

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radiation coming from its host star to

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the day side of the planet and then the

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cloud loses heat in a form of long wave

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radiation from both from day side and

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night side and the strong heating at the

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day side and the heating of the surface

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of the planet makes the atmosphere

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conductive the unstable and this gives

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this leads to the rising connection

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motions the day side and the formation

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of thick layer of clouds and this heat

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and moisture on sport eventually merges

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with the upper atmosphere equatorial jet

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and it's being transported to the night

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side of the planet and the in the

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absence of the dynamical auction this

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heat this Atma started heat transport is

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was the only source of energy for the

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night side and this is indeed what we

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see from a GCM output so this is a UK

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Met Office unified model output for

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Travis Ronnie you have the strong you

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have very one atmosphere at the surface

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on this in the on the day side of the

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planet

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that's zoom in where all the interesting

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stuff is happening then if you plot the

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wind vectors over its you you see the

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raising oceans and then the eastward jet

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and when we if you overlay that with the

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specific humidity contours you see how

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its concentrated on the day side where

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they all the vibration is happening and

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then if you rescale it to a photogenic

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scale you see that it eventually being

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transported to

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the night side as well as well as clouds

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so for a situation like that you can

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both size that convection should

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regulate the climate on the title locked

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planet and how can you attest this so we

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can run again this 3d GCM with different

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options for convection and so we can use

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sophisticated mass flux convection

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scheme which is used for weather in

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climate prediction on earth and I'm

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going to show I'm gonna call this

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experiments control and then we can use

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a simple moist adjustment scheme which

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I'm gonna call LCS for Lambert and Lewis

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connection scheme and then I can also

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switch off the convection scheme

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completely and then the let the model

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handle the convection itself without any

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help from the planet ization

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so in the next few slides I'm going to

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show you the view global maps of surface

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temperature for control simulation and

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also since TV runs both the Trappist 1e

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and Proxima B so starting with Trappist

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this is the global map of C search

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temperature just surface temperature and

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you see that's the of course the dayside

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is much much warmer than the night side

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and the difference is quite large and

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have this called traps on the night side

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where the Crosby dryers occur in the

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wind field for approximately in this

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conditions the situation is fairly

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similar and then when we run this

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simulation with a simple adjustment

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scheme instead of the mass flux scheme

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you see that it has quite a significant

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impact on the surface temperature of the

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planet so the night side especially

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warmed significantly by up to 40 degrees

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or the chocolate one case however then

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we can also run a similar sort of

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simulation but now switching off the

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convention scheme completely and this is

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the simulation result for epsilon team

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and it's a fairly similar picture you

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have the slight cooling of the dayside

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and warming on the night side however

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for approximate be the situation is

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almost reversed and you have the night

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side cooling quite significantly so for

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for this too quite similar cases you

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have opposite effects by just swapping a

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convection scheme to a simple one or

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switching off completely and this is so

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this is interesting and I'm still trying

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to wrap my head around while it happens

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but looking at the large-scale

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circulation so you see that so this is a

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horizontal wind speed shown by vectors

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and the magnitude of the wind is shown

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by colors and this is what so this is

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the

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approximately simulation doesn't change

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much and the magnitude of the wind stays

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fairly similar but for Travis Lonnie the

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large-scale circulation changes quite

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dramatically and you don't have this

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branches around the subsoil point and

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instead you have a very strong

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equatorial jet and the you can expect

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that because the wind increased wind

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speed increased at the Eastern

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Terminator and decreased at the Western

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Terminator the net moisture export from

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the dayside is larger so that this is is

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likely the the biggest G visitor to the

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change in the Nightside conditions while

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radiation and turbulence fluxes from the

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night side up probably cancel each other

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out and play a minor role so yeah so the

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sort of take-home message one is that

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convection in GCMs regulates the climate

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not only on the day site where all the

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connection is happening but perhaps

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contrary counter-intuitively

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on the night side and also the second a

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take-home message is that using a simple

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connection scheme can have different

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effects for different planets

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so why modeling convection has such a

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big impact well because as we heard from

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Allison this morning

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modeling convection is quite challenging

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it has a lot of feedbacks and also

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involves a wide spectrum of spatial and

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temporal scales and so it is

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computationally expensive to run global

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circulation models at convection

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resolving simulation

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lucien especially when they are coupled

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to radiation and chemistry and other

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stuff so what we do we run this GCM

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that's very coarse resolution instead

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and so the all the convective processes

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fall into sub grade scale size and we we

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have to use para positions to account

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for the net effect of them but

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unfortunately we don't have any in situ

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measurements on exoplanets at least not

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yet

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and so we have to our next best option

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to test this parent is Asians is to run

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a convection resolving model the very

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high resolution which does not need a

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parameterization to handle convection so

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this is what we can do with the unified

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model and we use a global model just as

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I showed before as a as a parent model

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to to supply boundary conditions but

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then we put a nested grid inside of the

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of that model and run this model at much

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higher resolution so I'm using a sort of

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convection permitting resolution of

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about 4 kilometers and in this case of

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course we have convection explicit so

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the convection organization is switched

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off so and when we look at the the

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outputs of of the simulations so this is

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so far just the global model again at

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the course resolution with convective

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compensation and this is just a chunk

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cut out of the of the global model

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around this nested region and you see

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that in terms of updrafts the the the

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rising motions the upward velocity field

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is quite washed out and and weak but

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when we run this model at high

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resolution you can start to see all the

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convection cells in individual

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convective cells being resolved and also

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some mesoscale circulations

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emerging on this planet

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and also the magnitude of updrafts and

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downdrafts is much greater than in the

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global model and this is what it looks

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like in terms of cloud fields so this is

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the reflected shortwave radiation and

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you see again that the convection

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resolving simulation gives you much more

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detail and much more in homogeneity in

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terms of cloud field and this is what

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the participation looks like so relation

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falling from this convective clouds okay

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but does it make a difference for for

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the mean state of the region and

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actually I should say that the global

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model with this mass flux parent

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connective translation is doing a pretty

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good job at least for earth-like

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atmosphere in in accounting for all the

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great convection and so in terms of

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temperature or specific humidity overall

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the curves are quite similar to each

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other from so the liquors from the

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global model and the regional model and

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the Wiccans difference is actually in

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the structure of the clouds on the day

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side and you can you can see this in

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terms of cloud condensate so this is

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average vertical profiles of cloud water

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on the left and called ice on the right

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so this is from the global model and

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this is the the orange curve is from the

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nested run simulation and you can see

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that the global model overestimates the

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cold water and underestimates cloud ice

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this can have an impact on the radiative

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forcing of clouds and also it can impact

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the formation of rain and/or snow

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precipitation but so the another

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take-home messages are compared to a

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convection resolving model cm may

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incorrectly represent cloud structure

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and they are radiative effects on the

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day side

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but I should say that one caveat of our

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study is that we use this model you know

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one-way nesting set up so even though

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the the regional model has the boundary

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conditions from the parent model it

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doesn't there's no feedback to the

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global model from these hires of

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simulations so one way to account for

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this impact is what I'm suggesting to do

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is basically what I'm doing now is to

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run a series of global experiments with

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different convection schemes then

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calculates the flux of moisture upward

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flux on the dayside as a metric for

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convection and then somehow find a

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correlation with some Nightside

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parameters such as the minimum

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temperature or the amount of moisture on

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the night side and if we find a good

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correlation between these parameters

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then we can run a nested simulation find

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the same integrated vertical flux of

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moisture and then infer from that what

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difference would it make for the night

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sight if we run the simulation as a

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convection resolving model for the for

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the whole planet and with this is my

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final take-home message so these

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simulations at high resolution relations

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might be used to assess the convection

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schemes and they impact on the Erika

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planet's climate and this is the summary

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of the messages and this I'll leave you

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hey Daniel from MIT and this is very

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exciting do you have a way for

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understanding the different schemes

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maybe in terms of a convective

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detainment or n treatment have you

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thought about that yes I am thinking

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about that and one of my next step is to

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run a series of sensitivity experience

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for the mass flux scheme and just change

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entrainment and D training parameters

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because for earth-like simulations for

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simulations of Earth convection it has

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been shown that this this is indeed

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probably the most important parameter in

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in the convection formulations but we

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also have a sort of first it's

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statistical framework in the making by

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differences between diffe completely

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different convection schemes so we can

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probably apply that to yeah thank you

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a nice talk tag to my sake Chicago so

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how do you choose the scale for your

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nested box

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have you tried like different box sizes

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does that affect the connection on the

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day side yeah that's that's a good

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question and I've been I spend like many

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months of simulations of trying to shift

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that box around and see what difference

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it makes and basically well first of all

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you have to probably choose the position

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correctly because on some planets the

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the most the hot spot is shifted a bit

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to the air to East and this happens on

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terrestrial plants as well so you can

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you should account for that and also of

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course this smaller box is in the

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simulation the more this regional model

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is sort of dominated by the boundary

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flow from the

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parent model so you have to to make this

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box sufficiently large so far it's

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around 60 degrees in the side of the box

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Manitoba Ontario Geneva did you make

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some experiments for rotate or

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synchronous ballot and you see any

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indication of self aggregation in these

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simulations yes one thing that we're

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thinking about too but I would say that

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it's probably not exactly self

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aggregation because there are so many

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external disturbances that can affect us

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so the the convection probably organizes

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but it's probably not exactly self

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aggregation because you have quite a

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large wind shear in this region and it's

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but the wind she'll come is because the

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do planet you are working it off quite

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fast rotate alright but yeah what if the

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planet were merged over with it oh I

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haven't looked at super slow rotating

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planets but yeah that's that's a good