Introduction to Code_Saturne - Working with subroutines

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Examples Change the density ρ as a function of the temperature T . ! ! iphas = 1 ivart = isca ( iscalt ( iphas )) ipcrom = ipproc ( irom ( iphas )) vara = -4.0668d -3 varb = -5.0754d -2 varc = 1000.9 d0 ρ = T (aT + b) + c do iel = 1, ncel xrtp = rtp (iel , ivart ) propce (iel , ipcrom ) = xrtp * ( vara * xrtp + varb ) + varc enddo Physical properties (ρ, µ, Cp...) can be changed via the usphyv.f90 subroutine. J. Uribe (University of Manchester) Introduction to Code Saturne 14 / 15
Examples Initialize temperature T at the beginning of the calculation: iphas = 1 ivart = isca ( iscalt ( iphas )) if ( isuite .eq .0) then do iel = 1, ncel rtp (iel , ivart ) = 25. d0 enddo endif ISUITE : Index for calculation restart. ( = 1 , restart.) To initialize velocity as a cosine function: iphas = 1 ivaru = iu( iphas ) xpi = 3.14159 d0 A = 2. d0 if ( isuite .eq .1) then do iel = 1, ncel rtp (iel , ivaru ) = A* cos (2. d0*xpi * ttcabs ) enddo endif TTCABS : Current time (in seconds). J. Uribe (University of Manchester) Introduction to Code Saturne 15 / 15
Page 1 and 2: Introduction to Code Saturne Workin
Page 3 and 4: Introduction Code Saturne provides
Page 5 and 6: Introduction Code Saturne provides
Page 7 and 8: Base module subroutines Most useful
Page 15 and 16: Structure Then, a table with the ex
Page 17 and 18: Local variables and initialisation:
Page 19 and 20: Important points to take into accou
Page 25 and 26: Main Variables Array dimensions (se
Page 33 and 34: Solved variables are stored in two
Page 35 and 36: Solved variables are stored in two
Page 37 and 38: Physical properties Physical proper
Page 39 and 40: Physical properties Physical proper
Page 41: All information is stored in two ma

Introduction to Code_Saturne - Working with subroutines

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