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SUMMARY:Exploring Convective Boundary Mixing Through Stellar Pulsations
DTSTART;VALUE=DATE-TIME:20261028T174500Z
DTEND;VALUE=DATE-TIME:20261028T175500Z
DTSTAMP;VALUE=DATE-TIME:20261101T123120Z
UID:indico-contribution-3627@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Serena Davis (Mount Allison University)\nConvective 
 boundary mixing occurs at the boundaries between convection and radiation 
 zones in stars\, where the material in the convection zone crosses the con
 vective boundary. This can change the location of the convective boundary 
 and bring more hydrogen into the core of the star\, which has many effects
  on its evolution\, including an extended main sequence lifetime. We use 1
 D stellar evolution code MESA (Modules for Experiments in Stellar Astrophy
 sics) to make models of stars with various convective boundary mixing proc
 esses\, and calculate pulsation frequencies for the models with the GYRE s
 tellar oscillation code. We then use the pulsation frequencies of the mode
 ls to compare the effects of these different processes\, and their impleme
 ntations in MESA\, on the star. Our goal is to find some difference caused
  by the different convective boundary mixing processes that could potentia
 lly be observed in real stars. This will help us understand how these proc
 esses occur in stars\, enabling more accurate predictions of stellar evolu
 tion.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributions/3627/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3627/
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