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X-WR-CALNAME;VALUE=TEXT:ITC Special Seminar - Maxwell Moe (Univ of Arizona)
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SUMMARY:ITC Special Seminar - Maxwell Moe (Univ of Arizona)
DESCRIPTION:<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">"The Formation and Evolution of Close Binaries and Planets "</span></span></span></span><div>	 </div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">Abstract: The formation and orbital migration of close binaries and</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">planets remain a mystery. The majority of very close binaries have</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">outer tertiary companions, suggesting Kozai-Lidov oscillations coupled</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">with tidal friction play an important role in their dynamical</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">evolution. However, close pre-main-sequence binaries are ubiquitous,</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">indicating most close binaries migrated within a few Myr while there</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">was still dissipative gas in the primordial disk. I will overview a</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">new population synthesis model that incorporates more realistic</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">initial conditions and a novel tidal mechanism to explain the</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">formation of close binaries and hot Jupiters during the</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">pre-main-sequence phase. The close binary fraction and Jovian planet</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">occurrence rate both increase with stellar mass, providing insights</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">into their respective formation processes. Although planets may favor</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">metal-rich hosts, recent observations demonstrate the close binary</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">fraction dramatically increases toward lower metallicities. I will</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">discuss five different observational techniques that corroborate this</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">metallicity trend and outline a fragmentation model that reproduces</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">the observations. I will also highlight the implications for Type Ia</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">supernovae, mergers of compact remnants, and biases in the inferred</span></span></span></span></div><div>	<span><span style="color:#212121"><span style="Helvetica,Arial,sans-serif"><span style="background-color:#f5f5f5">planet statistics.</span></span></span></span></div>
LOCATION:Pratt
STATUS:CONFIRMED
DTSTART:20180627T173000Z
DTEND:20180627T183000Z
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