SPH Simulations

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Information about SPH Simulations
Science-Technology

Published on September 27, 2008

Author: ellenolan

Source: authorstream.com

Slide 1: by Eleanor Nolan MSc. in Astronomy National University of Ireland, Galway Florida Institute of Technology, Melbourne, Florida Numerical Simulations of Superhumps in Cataclysmic Variables Slide 2: Introduction –What is a CV? Binary System with White Dwarf Roche Lobe filling Secondary Mass Transfer Accretion Stream Accretion Disk Bright Spot Slide 3: Systems with 0.02 ≥ q ≤ 0.25 Constant High Mass Transfer Rates High Viscosity AM CVns and nova-likes Superhumps SPH Code : Lagrangian Fluid Method: Viscosity Mass Ratio Particle Size Disk Temperature Disk Inclination Ray Trace: No. of Particles SPH Code Slide 5: Numerical Simulations of an Accretion Disk CV reference library Emission Line Profiles Trailed Spectrograms Light Curves Results : Results Emission Line Profiles Light Curve Trailed Spectrograms : Trailed Spectrograms Results : SW Sex Star : Results : SW Sex Star Florida Antics : Florida Antics Acknowledgements : Science Faculty Funding FAS Professor Mike Redfern, NUIG Dr. Matt Wood, FIT Acknowledgements

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