Journal
ASTROPHYSICAL JOURNAL
Volume 773, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/773/2/169
Keywords
planets and satellites: atmospheres; stars: interiors; Sun: interior
Categories
Funding
- TAC fellowship
- CITA postdoctoral fellowship
- Hertz Foundation Fellowship
- National Science Foundation Graduate Research Fellowship [DGE 1106400]
- NSF [0847477, NSF-0933759, AST 09-02004, PHY 08-21899]
- Center for Momentum Transport and Flow Organization (CMTFO)
- US Department of Energy-Office of Fusion Energy Sciences
- American Recovery and Reinvestment Act
- STFC [ST/K000853/1] Funding Source: UKRI
- Direct For Mathematical & Physical Scien [847477] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [847477] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0902004] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [821899] Funding Source: National Science Foundation
- Science and Technology Facilities Council [ST/K000853/1] Funding Source: researchfish
Ask authors/readers for more resources
The speed of sound greatly exceeds typical flow velocities in many stellar and planetary interiors. To follow the slow evolution of subsonic motions, various sound-proof models attempt to remove fast acoustic waves while retaining stratified convection and buoyancy dynamics. In astrophysics, anelastic models typically receive the most attention in the class of sound-filtered stratified models. Generally, anelastic models remain valid in nearly adiabatically stratified regions like stellar convection zones, but may break down in strongly sub-adiabatic, stably stratified layers common in stellar radiative zones. However, studying stellar rotation, circulation, and dynamos requires understanding the complex coupling between convection and radiative zones, and this requires robust equations valid in both regimes. Here we extend the analysis of equation sets begun in Brown et al., which studied anelastic models, to two types of pseudo-incompressible models. This class of models has received attention in atmospheric applications, and more recently in studies of white-dwarf supernova progenitors. We demonstrate that one model conserves energy but the other does not. We use Lagrangian variational methods to extend the energy conserving model to a general equation of state, and dub the resulting equation set the generalized pseudo-incompressible (GPI) model. We show that the GPI equations suitably capture low-frequency phenomena in both convection and radiative zones in stars and other stratified systems, and we provide recommendations for converting low-Mach number codes to this equation set.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available