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Hello planeteers!
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<div>We’re excited to host Roberto Tejada Arevalo from Princeton for this week’s planetary seminar. He will be joining us tomorrow to discuss the evolution of gas giant planets as constrained by solar system observations and how these models might inform our
understanding of gas giant exoplanets. Please join us on Tuesday (10/21) at 12:30pm in 54-517 or on Zoom. Lunch will be provided and we encourage you to arrive a bit early to get food.</div>
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<div>Roberto is available on Tuesday and for some of Wednesday morning for one-one-one meetings. You can sign up for a meeting <a href="https://docs.google.com/spreadsheets/d/1z16a3wqja10ozVbR69HT_yd-uy6fsSyZnPTIDwu-zgY/edit?usp=sharing">here</a>.</div>
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<div>Talk details and Zoom information are below. We hope to see you there!</div>
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<div>-John</div>
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<div><i>The Evolution of Gas Giant Planets</i></div>
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<div><b>Abstract: </b>Over the past decade, the Juno and Cassini spacecraft have revealed the existence of inhomogeneous interior structures in Jupiter and Saturn. Similarly, measurements of Uranus's gravitational field have been more consistent with an inhomogeneous
interior for many decades. More recently, formation models of the gas giants suggest that these planets may not have started fully convective, as past interior structure models assumed. Inhomogeneous evolution is required to explain the lower-order gravitational
field, helium abundances, effective temperatures, and radii of Jupiter and Saturn via fuzzy cores and helium rain. Our Saturn evolution models align with the recent Kronoseismology results from Cassini.</div>
<div>Similarly, inhomogeneous interior evolution is required to explain the gravitational harmonics, radius, atmospheric abundances, and the long-standing luminosity dichotomy of Uranus and Neptune. Provided that all of our Solar System gas giants likely harbor
extended regions that are stable to convection, this has implications for how we model giant exoplanet evolution generally. Throughout this work, I present new evolution models of the Solar System gas giants, guided by formation models and their gravitational
harmonic measurements. I will also present new evolutionary models of gas giant exoplanets with fuzzy cores to interpret new observations in the era of JWST and beyond.</div>
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<div>Zoom link: <a href="https://mit.zoom.us/j/97275591700">https://mit.zoom.us/j/97275591700</a></div>
<div>PW: 54100</div>
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