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PRODID:UW-Madison-Physics-Events
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SEQUENCE:1
UID:UW-Physics-Event-6200
DTSTART:20201123T180000Z
DTEND:20201123T190000Z
DTSTAMP:20260408T231312Z
LAST-MODIFIED:20201116T200242Z
LOCATION:Zoom: https://us02web.zoom.us/j/81509597155
SUMMARY:Monday Science Seminar\, Goni Halevi (Princeton) and Theron Ca
 rmichael (Harvard CfA)
DESCRIPTION:Goni Halevi:<br>
\nI’ll be talking about the interplay o
 f MHD turbulence and nuclear burning in accretion disks formed by disr
 upted white dwarfs. This has relevance to binary systems that may cont
 ribute to optical transients and future gravitational waves sources.<b
 r>
\n<br>
\nTheron Carmichael:<br>
\nTitle: The search for transiting 
 brown dwarfs with NASA's TESS mission<br>
\nTraditionally\, astronomer
 s have separated giant planets from brown dwarfs based on the object's
  mass. Objects more massive than 13 Jupiter masses but less massive th
 an 80 Jupiter masses are considered to be brown dwarfs. However\, in d
 etail\, the lower mass threshold is 11 to 16 Jupiter masses depending 
 on the metallicity of the object. This betrays how arbitrary a purely 
 mass-based distinction between planets and brown dwarfs is. Instead\, 
 we take a critical look at the population of brown dwarfs for which we
  have the most fundamental information: transiting brown dwarfs. Trans
 iting brown dwarfs provide us their mass\, radius\, and sometimes age\
 , which makes them useful for directly testing substellar evolutionary
  models. Through a better understanding of how well these models descr
 ibe the population of transiting brown dwarfs\, we will develop a bett
 er definition of what makes a brown dwarf different from a giant plane
 t: its formation mechanism. It is certainly true that in the mass rang
 e spanning between giant planets and low-mass stars that the dominant 
 formation mechanism must change significantly. If we can determine whi
 ch mass or distribution of masses that this change occurs at\, then we
  will have a more physical way to distinguish planets from brown dwarf
 s. In this talk\, we will review how the TESS mission has contributed 
 to the transiting brown dwarf population so far\, and we will examine 
 a few specific examples of transiting brown dwarfs whose masses\, radi
 i\, and ages have served as useful tests to substellar isochrones.
URL:https://www.physics.wisc.edu/events/?id=6200
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