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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-1470
DTSTART:20090224T213000Z
DURATION:PT1H0M0S
DTSTAMP:20260506T190735Z
LAST-MODIFIED:20090218T162724Z
LOCATION:6515 Sterling Hall
SUMMARY:Structure and Generation of the Solar Transition Region\, Astr
 onomy Colloquium\, Hakeem Oluseyi\, Florida Institute of Technology
DESCRIPTION:The solar transition region is an important region of the 
 Sun's atmosphere to understand since all the energy that is deposited 
 into the corona must pass through this component. Yet\, after over thr
 ee decades of study\, the morphology\, generation and energy balance o
 f the Sun's transition region atmosphere is poorly understood. Several
  classes of discrete plasma structures have been identified in the tra
 nsition region but their various contributions to the solar luminosity
  and variability have not been determined nor have their relationships
  to the dynamics and interactions of magnetic flux distributions been 
 clearly revealed. The connectivity between the transition region and t
 he corona has been heavily debated but also remains unresolved. The la
 rge-scale structure of the transition region\, including the disappear
 ance of the &amp\;quot\;chromospheric&amp\;quot\; network at temperatu
 res above 1 MK\, also remains unexplained. We have undertaken the task
  of studying several classes of transition region structures to addres
 s the problems introduced above. I describe in this talk studies of di
 screte plasma structures (funnels\, loops\, and bright points) and the
 ir ensembles to determine the partitioning of energy between them. I t
 est a statistical model of the generation\, distribution and propertie
 s of upper transition region bright points as a consequence of the con
 vection-driven recycling of solar magnetic fields. I present a new mod
 el of the upper transition region structure and implications for the p
 hysics of magnetic reconnection in plasmas at upper transition region 
 temperatures and densities. I will also discuss how these results may 
 be extrapolated to explore the detailed magnetohydrodynamic conditions
  on stellar surfaces and a recent technological advancement I have dev
 eloped that may substantially improve the spatial resolution of solar 
 observations.
URL:https://www.physics.wisc.edu/events/?id=1470
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