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SUMMARY:Modeling the UV Spectra of Magnetic Massive Stars - Christiana Erb
 a Debbrecht - University of Delaware
DTSTART:20210201T140000Z
DTEND:20210201T150000Z
UID:TALK154636@talks.cam.ac.uk
CONTACT:Cleo Loi
DESCRIPTION:The life cycles of massive stars are ultimately linked to thei
 r capacity (or incapacity) to retain their mass during their evolution. Th
 eir extreme radiation is strong enough to drive mass off their surfaces in
  a stellar wind\, which can be studied using ultraviolet (UV) spectra. Mag
 netic massive stars\, a subset of the OBA-type star population\, have surf
 ace dipolar magnetic fields about a thousand times stronger than that of t
 he Sun. These fields channel the stellar wind into structurally complex ma
 gnetospheres\, creating spectral line profiles with atypical shapes. UV re
 sonance lines reveal the density and velocity structure of the magnetosphe
 re and allow us to study the wind/field interaction. To date\, large-scale
  modeling of this phenomenon has been limited by the computational cost. O
 ur analysis\, the UV-ADM project\, solves this problem by applying a simpl
 e analytic prescription to efficiently calculate synthetic UV spectral lin
 es. Our models can be compared to UV observations of magnetic massive star
 s\, enabling us to make better predictions of stellar wind parameters.
LOCATION:Online
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