stardis(1)
NAME
stardis  statistical solving of coupled thermal systemsSYNOPSIS
stardis [option] stardis M <file> [option]
DESCRIPTION
stardis solves coupled thermal systems under the linear assumption. Here coupled refers to conductive, convective and radiative transfers, and linear means that each phenomena is represented using a model that is linear with temperature. stardis can deal with complex geometries as well as highfrequency external solicitations over a very long period of time, relative to the characteristic time of the system. The provided system description should comply with the stardisinput(5) format.
stardis can compute a thermal observable, like temperature or flux, at a probe point and date or the mean value of an observable over a given surface, volume, or time range. When a time range t1, t2 is provided, the computed value is the mean value over the time range. To compute the value at a given time, simply provide a single value t. In addition, stardis gives access to the evaluation of the propagator (a.k.a the Green function).
The propagator is of great value for thermicist engineers as it gives some crucial information to analyse heat transfers in the system. It helps engineers answer questions like "Where from does the heat come at this location?". Propagators seamlessly agregate all the provided geometrical and physical information on the system in an unbiased and veryfast statistical model.
stardis(1) also provides two additional functionalities: converting the stardisinput(5) geometry into a VTK file and rendering an infrared image of the submitted system.
Stardis' algorithms are based on stateoftheart MonteCarlo method applied to radiative transfer physics (Delatorre [1]) combined with conduction's statistical formulation (Kac [2] and Muller [3]). Thanks to recent advances in computer graphics technology which has already been a game changer in the cinema industry (FX and animated movies), this theoretical framework can now be practically used on the most geometrically complex systems. While this capability is part of the StarEngine Star3D library, it is internally powered by Intel® Rendering Framework: Embree.
Everytime the linear assumption is relevant, this theoretical framework allows to encompass all the heat transfer mecanisms (conductiveconvectiveradiative) in an unified statistical model. Such systems can be solved by a MonteCarlo approach just by sampling heat paths. This can be seen as an extension of MonteCarlo algorithms that solve radiative transfer by sampling optical paths. A main property of this approach is that the resulting algorithms does not rely on a volume mesh of the system.
[1] Delatorre et al., Monte Carlo advances and concentrated solar applications, Solar Energy, 2014
[2] Kac, On Distributions of Certain Wiener Functionals. The Annals of Mathematical Statistics, 1949.
[3] Muller, Some continuous MonteCarlo Methods for the Dirichlet Problem, Transactions of the American Mathematical Society, 1956.
MANDATORY OPTIONS
M file
 Read a text file containing a possibly partial description of the system. Can include both media enclosures and boundary conditions, in any order. Can be used more than once if the description is split across different files.
EXCLUSIVE OPTIONS
p x,y,z[,timerange]
 Compute the temperature at the given probe at a given time. By default the compute time range is INF, INF. The probe must be in a medium. The probe coordinates must be in the same system as the geometry.
P x,y,z[,timerange]
 Compute the temperature at the given probe on an interface at a given time. By default the compute time range is INF, INF. The probe is supposed to be on an interface and is moved to the closest point of the closest interface before the computation start. The probe coordinates must be in the same system as the geometry.
m medium_name[,timerange]
 Compute the mean temperature in a given medium at a given time. The medium name must be part of the system description. By default the compute time range is INF, INF. The medium does not need to be connex.
s file[,timerange]
 Compute the mean temperature on a given 2D region at a given time, the region being defined as the front sides of the triangles in the provided STL file. By default the compute time range is INF, INF. These triangles are not added to the geometry, but must be part of it. The region does not need to be connex.
S file[,timerange]
 Compute the bytriangle mean temperature on a given 2D region at a given time, the region being defined as the front sides of the triangles in the provided VTK file. These triangles are not added to the geometry, but must be part of it. By default the compute time range is INF, INF. The region does not need to be connex.
F file[,timerange]
 Compute the mean flux on a given 2D region at a given time, the region being defined as the front sides of the triangles in the provided VTK file. These triangles are not added to the geometry, but must be part of it. Flux is accounted positive when going from the front side to the back side, at a singletriangle level. By default the compute time range is INF, INF. The region does not need to be connex, but it can currently only include geometry appearing in description lines starting with H_BOUNDARY_FOR_SOLID, H_BOUNDARY_FOR_FLUID, F_BOUNDARY_FOR_SOLID or SOLID_FLUID_CONNECTION (see stardisinput(5)).
R [suboption:...]

Render an infrared image of the system through a pinhole camera and write it to
standard output. One can use alldefault suboptions by simply providing the colon character (:) alone as an argument. Please note that the camera position must be outside the geometry or in a fluid. Available suboptions are:
fmt=image_file_format
 Format of the image file in output. Can be VTK or HT. Default image_file_format is HT.
fov=angle
 Horizontal field of view of the camera in [30, 120] degrees. By default angle is 70 degrees.
img=widthxheight
 Definition of the rendered image in pixels. By default the image definition is 640x480.
pos=x,y,z
 Position of the camera. By default it is set to { 1, 1, 1 } or it is automatically computed to ensure that the whole scene is visible, whether tgt is set or not, respectively.
spp=samplescount
 Number of samples per pixel. By default, use 4 samples per pixel.
t=timerange
 Rendering time range. By default timerange is INF, INF.
tgt=x,y,z
 Position targeted by the camera. By default, it is set to { 0, 0, 0 } or it is automatically computed to ensure that the whole scene is visible, whether pos is set or not, respectively.
up=x,y,z
 Up vector of the camera. By default, it is set to { 0, 0, 1 }.
OTHER OPTIONS
a ambient
 Set the ambient radiative temperature for the whole system, in Kelvin. By default ambient is 300.
d

Write the geometry to
standard output
in VTK format along with various properties, including possible errors. If this option is used, no computation occurs.
Using this option in conjunction with an option that specifies a compute region (F, S, s) has the effect to include the region in the output. This option cannot be used in conjunction with other options that write to standard output (g, h, R, v).
D type,files_name_prefix

Write sampled heat paths of the given
type
to files in VTK format, one file per path. Possible values for
type
are
error
(write paths ending in error),
success
(write successful paths), and
all
(write all paths). Actual file names are produced by appending
files_name_prefix
and the path rank starting at index 00000000, and possibly followed by
_err
for failure paths: prefix00000000.vtk, prefix00000001_err.vtk, ...
This option can only be used in conjuction with options that compute a result (F, m, P, p, R, S, s) and cannot be used in conjunction with options g or G.
e
 Use extended format to output MonteCarlo results. Can only be used in conjunction with options that compute a single MonteCarlo (F, m, P, p, or s without options g or G).
g

Compute the Green function at the specified time and write it in ASCII to
standard output.
This option can only be used in conjunction with one these options: p, P, m, s and cannot be used in conjunction with option D.
G file_name[,file_name]

Compute the Green function at the specified time and write it to a binary file. If a second file name is provided, information on heat paths' ends is also written in this second file in ascii csv format.
This option can only be used in conjunction with one these options: p, P, m, s and cannot be used in conjunction with option D.
The resulting file can be further used through the sgreen(1) command to apply different temperature, flux or volumic power values.
h
 Output short help and exit.
n samplescount
 Number of MonteCarlo samples. By default samplescount is set to 10000.
r reference
 Set the reference temperature used for the linearization of the radiative transfer, in Kelvin. By default reference is 300.
t threadscount
 Hint on the number of threads to use. By default use as many threads as CPU cores.
v
 Output version information and exit.
V level
 Set the verbosity level. Possible values are 0 (no message), 1 (error messages only), 2 (error and warning messages), and 3 (error, warning and informative messages). All the messages are written to standard error. Default verbosity level is 1.
EXAMPLES
Preprocess the system as described in scene 5.txt when intending to compute the mean flux on the triangles from the file edge.stl, and write its geometry in the file scene.vtk. Verbosity level is set to 3:

$ stardis M "scene 5.txt" F edge.stl d V 3 > scene.vtk
Compute the temperature at the probe point 0, 0.5, 0 at steady state. The system is read from the file model.txt and the number of samples is set to 1000000:

$ stardis M model.txt p 0,0.5,0 n 1000000
Compute the mean temperature in the medium med05 at t=100 s. The system is read from the file model.txt and the result is output with extended format:

$ stardis M model.txt m med05,100 e
Compute the temperature at the probe point 0, 0, 0 at t=2500. The system is read from the 2 files media.txt and bounds.txt and the number of samples is set to 1000000:

$ stardis M media.txt M bounds.txt p 0,0,0,2500 n 1000000
Compute the mean temperature at the probe point 1, 2.5, 0 over the 50, 5000 time range. The system is read from the file model.txt:

$ stardis M model.txt p 1,2.5,0,50,5000
Render the system as described in scene.txt with default settings:

$ stardis M scene.txt R :
Render the system as described in scn.txt at t=100, spp=2, img=800x600, with output format fmt=ht and all other settings set to their default values. The output is redirected to the img.ht file. If the computation encounters erroneous heat paths, they will be dumped to VTK files named err_path_00000000.vtk, err_path_00000001.vtk, etc. The image file is then postprocessed using htpp(1) with default settings to obtain a png file.

$ stardis M scn.txt R t=100:spp=2:img=800x600:fmt=ht \ D error,err_path_ > img.ht $ htpp o img.pgn v m default img.ht
Compute the Green fonction that computes the temperature at the probe point 0, 0, 0 at steady state. The system is read from the file model.txt and the Green function is written to the probe.green file and the heat paths' ends are written to the probe_ends.csv file:

$ stardis M model.txt p 0,0,0 G probe.green,probe_ends.csv
COPYRIGHT
Copyright © 20182020 MesoStar>. License GPLv3+: GNU GPL version 3 or later http://gnu.org/licenses/gpl.html. This is free software. You are free to change and redistribute it. There is NO WARRANTY, to the extent permitted by law.
SEE ALSO
stardisinput(5), stardisoutput(5), sgreen(1), htpp(1)