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VERSION:2.0
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PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-1906
DTSTART:20100909T203000Z
DTEND:20100909T220000Z
DTSTAMP:20260506T161507Z
LAST-MODIFIED:20100901T172700Z
LOCATION:4421 Sterling Hall  Same Location
SUMMARY:3-D Dust Radiation Transfer: What can it do for you?\, Astrono
 my Colloquium\, Barbara Whitney\, UW SAL Department
DESCRIPTION:I will introduce myself to the department by describing so
 me applications of our radiation transfer codes to the study of star f
 ormation on size scales small and large. The codes calculate dust ther
 mal and non-thermal emission\, scattering\, and polarization in arbitr
 ary 3-D geometries. I will discuss how we can map the structure of the
  inner disks of T Tauri stars by modeling their optical and infrared v
 ariability\; our models of Young Stellar Objects (protostars and their
  circumstellar disks and envelopes) and star forming regions\; compari
 son of a Galactic population synthesis model of YSOs to GLIMPSE catalo
 gs to determine the star formation rate of our Galaxy\; determining th
 e star formation rate of the Large Magellanic by counting and modeling
  YSOs\; and galaxy models incorporating stars\, YSOs\, and interstella
 r dust\, including PAHs. As I dip my toes into the field of extragalac
 tic research\, I will be interested to get feedback on whether these c
 odes\, which are publicly available\, can be useful to you in your res
 earch\, and what additional development is most desirable (e.g.\, line
  emission).<br>
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URL:https://www.physics.wisc.edu/events/?id=1906
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