Changes between Version 70 and Version 71 of u/erica/2DShockedClumpsSNR

Timestamp:

01/31/18 12:46:00 (7 years ago)

Author:

Erica Kaminski

Comment:

—

u/erica/2DShockedClumpsSNR

@@ -142 +142 @@
 === Unresolved thoughts: ===
 
-Q - reflected BC differences - due to pressure/density protection, or position of clump wrt to grid?
+Q - Reflected BC differences - in only simulating the upper half of the domain, asymmetries formed in the shocked clump layer similar to those shown above in the AMR and PPM cases. Would be interesting to investigate this further -- e.g. what are numerical instabilities that occur along the symmetry axis in jet models when reflecting BC's are used, and could those be applicable here?  
 
-Q - size scales needing to resolve (i.e. instabilities and their wavelengths)?
+Q - Size scales needing to resolve (i.e. instabilities and their wavelengths) for supernovae remnants and their embedded shocked clumps?
 
-Q - examine cooling cases (cooling lengths/timescales, temperature ranges for various cooling tables in astrobear, modifying the abundances statically as well as dynamically, what options for tracking ionizations, etc., radiative shock physics -- shock structures in steady state solutions, additional instabilities that arise when cooling is possible)
+Q - Examine cooling cases (cooling lengths/timescales, temperature ranges for various cooling tables available in astrobear, modifying the abundances upon initialization, as well as dynamically throughout the simulation, what options are there for tracking ionization fractions, what additional instabilities can arise with cooling turned on.
+
+Q - Examine radiative shock structures in steady state solutions
 
 
 === Reference Papers === 
+
+See my supernova remnant library on ads here.