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The new code for ESA meteoroid model.
Alexey Mints1 Valery Dikarev1 Gerhard Drolshagen2
1University of Bielefeld, Germany
2European Space Agency, Noordwijk, The Netherlands
18.07.2010
Problem
Outline
1 Problem
2 Code
3 GUI
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 2 / 22
Problem
Requirements
Input: Target trajectory and geometry, output contentspecification;
Output: Estimated dust flux, number density and averagevelocity. Dust distributions in mass, incidencedirection and velocity.
GUI: A tool to set input parameters and view output.
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 3 / 22
Problem
Orbital elements
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 4 / 22
Problem
Model (as of now)
5 populations, for each:
• Rectangular 3D grid in orbital space. Dimensions:pericenter distance (0.05-6 a.u., 50 log-scale bins),eccentricity (0-1, 100 bins) and inclination (0-180, 180bins);
• Mass spectra (200 log-scale bins from 10−18 to 105
grams), independent of orbital elements;
Current model file size ∼28 Mbytes.
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 5 / 22
Problem
Grids
Figure: Possible grids: regular (left), irregular (right)
Old IMEMRegular (orthogonal) grid inorbital elements.
New IMEMRegular (spherical) grid inincidence velocity.
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 6 / 22
Problem
Old and new approaches
Old IMEM
/ Jacobian diverges, tricks areneeded;
/ Incidence direction has to becalculated: have to run overthe whole model range;
, Symmetries can be used;
New IMEM
/ Symmetries cannot be used;
, No Jacobian needed;
, Incidence direction emergesnaturally from the grid;
, Reduced calculations forsensitivity;
, Various scans can be easilyimplemented;
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 7 / 22
Problem
Thresholds
C1 < mαV β < C2
• α = 1; β = 0 — mass threshold;
• α = 1; β = 1 — momentum threshold;
• α = 1; β = 2 — kinetic energy threshold;
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 8 / 22
Problem
Calculation grid
V ∗dust = V grid
dust + V ∗target
Geometrical sensitivity can be calculated from ϕ;Knowing V grid
dust we can calculate mass densities as∫ C2/V β
C1/V β mα dm;
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 9 / 22
Code
Outline
1 Problem
2 Code
3 GUI
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 10 / 22
Code
Application layout
Java Fortran
Model
CoreI/O routines
Data module
Inputdatafiles
Outputdatafiles
Task data
Globalsettings
Resultsdata
Interface
Userdata
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 11 / 22
Code
Application composition
• Calculation engine — FORTRAN-95 program (∼4000lines);
• GUI — Java graphical interface (∼11000 lines) developed
with NetBeans ;
• User documentation;
• Model file;
• Sample task and trajectory files;
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 12 / 22
Code
Engine input files
• Task file — over 30 parameters, defining task propertiesand output content and format;
• Trajectory file — contains orbital parameters orpoint-by-point trajectory;
• Sensitivity file — optional file containing sensitivityfunction;
• Model file — dust orbital distribution model (binary file);
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 13 / 22
Code
Task file
De s c r i p t i o n=Popu l a t i o n s=∗Meteoro id mode l=T r a j e c t o r y f i l e=x . t r jS e n s i t i v i t y f i l e=t . t s k s e n sP l o t s e t t i n g s=t . t s k p l o tRe s u l t=t . t s k r e sS e n s i t i v i t y p r e s e t =0P o p u l a t i o n s s t y l e=1P o i n t s s t y l e=1C o o r d i n a t e s s t y l e=1Ea r t h c o o r d i n a t e s=0Scan mode=0Phy s un i t s=0F lux=1Number dens i ty=0A v e r a g e v e l o c i t y=1Thre sho l d s=m, 1 .00 e−18, 1 .00 e+02I n c i d e n c e r a n g e =0.00 :180 .000000V e l o c i t y r a n g e =0.000000:100000.000000Ta rge t t yp e=0Ta r g e t o r i e n t a t i o n=0O r b i t k i n d=1O r b i t s o l a r=0O r b i t e c l i p t i c a l =0
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 14 / 22
Code
Engine output
#IMEM2 output f i l e#Created=20/ 5/2010 20 : 2 7 : 3 5 . 1 60#Phy s un i t s=F#Scan mode=0#S c a n r e s o l u t i o n= 20#P o p u l a t i o n s s t y l e=1#P o i n t s s t y l e=1#Th r e s h o l d s i n c o l umn s=F#C o o r d i n a t e s s t y l e=1#Ea r t h c o o r d i n a t e s=F#Number dens i ty=F#Flux=T#Av e r a g e v e l o c i t y=T#Targe t t yp e=0#Ta r g e t o r i e n t a t i o n=0#S e n s i t i v i t y p r e s e t =0#T r a j e c t o r y t y p e=0#T r a j e c t o r y t y p e= 0 . : 180 .#M i s s i o n d u r a t i o n= 3 .0#Mi s s i o n l a un ch= 0 .0#Po in t Thr | Time | a s t e r o i d s c o l l i s i o n s | . . .# | | F lux | AvgV | . . .# 1 | 2 | 3 | 4 | 5 | . . .
1 1 0.00000000E+00 0.0000000E+000 0.0000000E+000 . . .2 1 0.10000000E+01 0.0000000E+000 0.0000000E+000 . . .3 1 0.20000000E+01 0.0000000E+000 0.0000000E+000 . . .4 1 0.30000000E+01 0.0000000E+000 0.0000000E+000 . . .. . . .. . . .A. Mints, 18.07.2010 The new code for ESA meteoroid model. 15 / 22
GUI
Outline
1 Problem
2 Code
3 GUI
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 16 / 22
GUI
Main window
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 17 / 22
GUI
Output properties window
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 18 / 22
GUI
Progress window
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 19 / 22
GUI
Plots
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 20 / 22
GUI
Maps
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 21 / 22
GUI
Future plans
• Final release – September 2010;
• OpenMP and MPI extensions;
• Web-interface;
• More Engine features (for example, meteor flux for agiven location on Earth);
A. Mints, 18.07.2010 The new code for ESA meteoroid model. 22 / 22