[mesa-users] mesa-users Digest, Vol 74, Issue 1

[Conny Aerts]

Hi Dave and Jan-Torge,

count us in at Leuven. This is totally in line with a new grant achieved here. Even though I’ll only be hiring personnel in the 2016/7 time frame for this topic, we already have lots of information in terms of asteroseismic interior structure profiles, to make tests based on your new implementation for various types of stars and evolutionary phases.

Good luck! Conny

> Message: 1
> Date: Wed, 30 Sep 2015 10:13:55 -0700
> From: David Arnett <wdarnett at gmail.com>
> Subject: [mesa-users] Solberg-Hoiland stability
> To: MESA users group <mesa-users at lists.sourceforge.net>
> Message-ID:
> 	<CAGpgfQE3CnYDkhBLvnHhL-M-0ynddpMOYX+QHsfKa2k8bXKS8g at mail.gmail.com>
> Content-Type: text/plain; charset="utf-8"
> 
> J.-T. Schindler and I are planning to visit Kavli in November (the week
> before Thanksgiving) to work with Bill to implement a new option for
> convection in MESA: 321D (Arnett, et al., ApJ, 2015). Because 321D uses an
> acceleration equation, it automatically determines  boundaries (that is,
> where velocity is negligible). It is based on 3D simulations of turbulent
> convection and fluid experiments.
> 
> We crawl before we walk, so the first version ignores rotation, but it
> seems obvious how to start to generalize to rotating systems. For slow
> rotation, something like the shellular approximation of Maeder and Meynet
> is valid.
> 
> We welcome collaborators in this effort. Anyone interested?
> Dave
> 
> ps. All the usual stability criteria (e.g., Schwarzschild, Ledoux,
> Richardson, Solberg-Hoiland,  etc.), as well as boundary physics
> (overshoot, semiconvection, wave generation, etc.) are contained in the
> general formulation of 321D simply because acceleration is what gives
> motion.
> 
> -- 
> David Arnett
> Regents Professor
> Steward Observatory
> University of Arizona
> 
> Facts are stubborn, but statistics are more pliable.  Mark Twain
> Facts do not cease to exist because they are ignored.  Aldous Huxley
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