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PRODID:UW-Madison-Physics-Events
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SEQUENCE:2
UID:UW-Physics-Event-6355
DTSTART:20210304T213000Z
DTEND:20210304T230000Z
DTSTAMP:20260415T010821Z
LAST-MODIFIED:20210305T140627Z
LOCATION:Zoom meeting(see Abstract ) Coffee and tea 3:30pm\, Talk 3:45
 pm
SUMMARY:What Sets the Efficiency of Radial Migration is Spiral Galaxie
 s?\, Astronomy Colloquium\, Kate Daniel\, Bryn Mawr
DESCRIPTION:After an initial epoch of assembly\, spiral galaxies like 
 the Milky Way evolve primarily under the influence of slow\, internal 
 processes.  This secular evolution rearranges the orbital angular mome
 ntum and energy of a galaxy’s disk\, thus altering its kinematics\, 
 morphology\, and chemical distribution.  Central to our understanding 
 of secular evolution is how transient spiral arms cause stars to migra
 te large radial distances from their birth radii.  Radial migration is
  often associated with increased orbital eccentricity\, thus kinematic
 ally heating the disk.  However\, a particularly important type of rad
 ial migration\, called churning or cold torquing\, can change the size
 s of stellar orbits in the disk without significantly altering their e
 ccentricities.  The relative importance of cold or heating radial migr
 ation significantly impacts how disks evolve. In this talk\, I will de
 mystify the physics that governs various forms of radial migration and
  discuss their observational signatures.  I will then present scaling 
 relations for the efficiency of cold torquing. Finally\, I will argue 
 that in some limits cold torquing can\, in fact\, kinematically heat t
 he disk.  First steps have been taken\, but there is an ongoing need t
 o further develop this theoretical framework for the interpretation of
  data from high resolution simulations and large\, high precision obse
 rvational surveys of the Milky Way.<br>
\n<br>
\nZoom Link<br>
\nhttps
 ://uwmadison.zoom.us/j/88513896776?pwd=Y1JtRE1KZllxWkFTamJBSGtGdm9yQT0
 9
\n
URL:https://www.physics.wisc.edu/events/?id=6355
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