Jiapeng Gao
How to bake puffy planets: Coupling radius inflation with high eccentricity migration

Yeah. Good morning, everyone.
It's a great pleasure to be here and I'd like to start by thanking the organizers of this meeting for giving me the opportunity to share my work, and my name is Jiapeng Gao, a second year graduate student at Georgia Tech under my supervisor, Gongjie Li, and today my work focus.
On how to bake puffy planets.
Radius inflation with high extensity migration.
So TAVI planets is, is one of the mystery that the tactic that exoplanets brings us was their origin, and many of them can be explained by these Strong's intents deliberation. It received some nice post star, but some of them only receive moderate stellar ration. How do they?
Form how do they get there and what causes these papines?
So here I use words and phrases as an example, which is a satin mass planet with Jupiter radius making houses of Saturn.
It's relatively easy planet, and it also orbits its whole star in around 10 day orbit with residual extrinsity around .3, which is indicating its title hitting history.
So this brings us the question, how does title fitting affect the structure of the tenets and which inter influence the dynamic evolution of this planet?
Actually, there has been previous works highlighting radius inflation with title migration for example and that has shown the formation of what's being successfully explained by helping radios, inflation and high exchange migration and tackle also shows the formation of hat P11B and also they demonstrated that really.
Simulation can save planners from Tetris eruption.
But their works have limitations. Using a very crude.
So you and I only use a simple analytical.
Model that has constant deflation and inflation timescales well.
Instantaneous inflation model.
So it calls for a realistic structure evolution model which will not only enable us to investigate the dynamical origin of the planets more accurately, but also allows for probing into the planet structure evolution.
So here I introduce our model the calculate Mesa with codes.
So it's here we still consider actions to migration as the formation channel, the worms, and so we here include octopod little posi and also short range forces such as J2GR and especially the title forces. In our code we calculate title hitting rate and the standard ER.
Rate.
From the dynamical code and inject the heating into the planets.
To bake the planet and the planning mother was based on Mesa, which is the can also be used for planets and we inject the heating. We use Mesa to build a core and model and we inject the title hitting onto the core and the boundary and the surface.
Hitting the celebration is on to the surface of planet.
As a planet evolves, we will update the planet radius and love number of this planet back to the dynamic code which will in turn influence this dynamic evolution and as a loop goes on, we will finally get our results.
But here, should the possible formation channel was one 7B.
The right panel shoots a tiny evolution of semius axis extensions.
T radius of these planets as a blue line shows the case with reduced inflation and the Orange line shows the case of without REDUS inflation.
We see that with redistribution because.
Suppress at larger prison distances, leading to a longer synchronization time scale, which means that with the evolution of this planet, circular rise very slowly and finally reach our observation value shown in the red dots here.
And in short, we will have a larger final semi access and radius with radius inflation.
So in order to illustrate our results, I have made a 3D movie here.
The lap panel shows the 3D object evolution of the planets to orbit with the radial radius of the planet and the right panel shows semijaxis extensions, T, personal distance, and the radius of this planet with a radius line is a time indicator.
Doesn't take a quick look.
At the first phase, the orphanage oscillates very fast because and then the title hitting triples, radius of the planet.
Leading to stronger ties that suppress kosai.
And after that we see slower precession due to ties in Jr. and also the civilization is much slower.
And that was for only one case.
We have also done a multi colour simulation of many cases.
So here we show the final orbital distribution for the multi cast formulation with reduced inflation, which is shown in blue and without reduced inflation, which is shown in orange. You see that with red inflation the final of the period is generally larger than those without reducing inflation which.
Is due to the larger percentages when suppressing the Kobe.
Similar things happens with eccentricity.
We see a broader eccentricity distribution for those wave.
In compared with those without radius inflation.
So this is due to the longer synchronization time scale.
And for our all previous examples, we all used A20 Earth core math model.
But since we're using unrealistic interior structure model, it enable us to infer the internal structure of this planet.
So we made another example with only five Earth mass core masses for the planets, which is shown in green.
Here we see that with lower chromatography, even larger and leading to a stronger suppression in the of the difficult dye and finally.
Leading to a larger final order period.
She has given us the opportunity to constrain the planet's interior structure and core messages using our observation onto the orbit of the planet.
So to summarize, we have shown that table heating is capable of explaining the radius information of warm, puffy plants.
The mechanism behind the is a suppression of larger pressure distances and also the core mass matters. So and also thanks for the ongoing and the future observations we can expect for more transit and RV observations for pinning down the pyramids of the inner planets.
And also long term RV and also astronomical observations.
To find out the characteristics of the other plans and the most interesting thing is that we can actually try to constrain the planes corresponding to atmospheric chemical abundance using the jwst.
And we are entering an era, an exciting era of investigating orbital evolution with interior structures.
With that, with all that, I'd like to thank you for your attention and I'm happy to take any questions.
We have two minutes for questions, please. Yeah, go ahead.
Hi. Chopping the only Brandy.
University of Kansas. Really interesting work.
Can you say a little bit about the final like density distributions that you end up with some of these planets?
How puffy can you actually make a planet by this method?
Well, so you it depends on the planet and we can inflate the planet at most as three groups of radius for seven mass planet. And that is actually only for a very short period.
But for the most of the period that we can inflate the atmosphere down to around.
.2G per cubic centimeter and you can expect it even less for a a very short period.
So quick questions.
We have two-minute, one minute, very cool result.
I think you did a great job demonstrating that this mechanism is going to be important for hot Jupiters.
I'm curious if you've thought at all about finding the lower mass limit where you expect this radius inflation to kind of protect against tidal evolution.
Is that something you have?
Maybe planned in the future or?
We're pending to do this at in the future and that currently we're only focusing on the Saturns and Jupiter's with more masses.
Thanks. OK. Very quick question. While the other speaker sets up.
Hi. Great talk, Megan howsler. As you, I was just wondering.
So are most of these puffy planets tidally locked?
Like or can they be buffet planets without being tidally lock?
Ed. They have eccentricity.
They actually are causal synchronized. The way the stars so so it doesn't matter.
So actually we if you call them, it's actually not exactly tidally locked, it's pseudo locked.
So we will have them ties because of the extensity.
Thank you very much. OK.
Let's take the chance to thank all the early career science speakers.