BEGIN:VCALENDAR
PRODID:-//Microsoft Corporation//Outlook MIMEDIR//EN
VERSION:1.0
BEGIN:VEVENT
DTSTART:20121115T223000Z
DTEND:20121115T231500Z
LOCATION:Ballroom-EFGH
DESCRIPTION;ENCODING=QUOTED-PRINTABLE:ABSTRACT: A number of astrophysical phenomena are characterized by low Mach number flows. Examples include the convective phase of a white dwarf prior to ignition as=0Aa Type Ia supernova, X-ray bursts, and convection in massive stars. Low Mach number models analytically remove acoustic wave propagation while retaining compressibility effects resulting from nuclear reactions and ambient stratification. This enables time steps controlled by advective time scales, resulting in significant reduction in computational costs.  We will discuss the derivation and implementation of low Mach number models for astrophysical applications, particularly in the context of structured grid AMR, and will present computational results from three-dimensional adaptive mesh simulations.
SUMMARY:Low Mach Number Models in Computational Astrophysics
PRIORITY:3
END:VEVENT
END:VCALENDAR