Diffusion Reacceleration and Advection of Galactic cosmic rays: an Open New code
DRAGON adopts a second-order Cranck-Nicholson scheme with Operator Splitting and time overrelaxation to solve the diffusion equation. This provides fast a solution that is enough accurate for the average user. Occasionally, users may want to have very accurate solutions to their problem. To enable this feature, users may get close to the accurate solution by using the fast method, and then switch to a more accurate solution scheme, featuring the Alternating-Direction-Implicit (ADI) Cranck-Nicholson scheme.
Some parts of DRAGON are built following GALPROP, v50p. The first reason is that it is a waste of time to reimplement standard parts, like energy losses, in which nothing new has to be found. The second reason is that it is essential to be able to compare our predictions with that of the Galprop code, and this can be done only by following the details of its implementation. Therefore, we kept in the code some features and models used in Galprop, like nuclear cross-sections, the gas distribution, the convergence technique. However, each of these models is accompanied by other models, which can be selected by setting the appropriate switch. This is done very easily using the well known C++ structure of abstract/derived classes. The code is then very flexible and easy to manage and to modify or update.
The code was built having in mind a few motivations:
- in order to find good propagation models one needs to run the code thousand times. Therefore we wrote the code aiming at performances and with an efficient memory management.
- we wanted to propagate DM originated cosmic rays. Therefore we wrote DRAGON as a library that can be coupled to, e.g., DarkSUSY.
- from the physics point of view, we wanted to have a position dependent diffusion model, which requires a substantial modification of the discretization scheme.
Get the latest version of the code here and untar it.
To install DRAGON you need to download and install the GSL libraries and CFITSIO library first.
It also optionally requires DarkSUSY, if user wants to propagate DM originated cosmic rays.
Before installing the code launch the script to initialize installation tools:
./start.sh
Configure the code, a typical command line is:
./configure --with-cfitsio=$CFITSIO_DIR --with-numcpu=2
where $CFITSIO_DIR is the path of your cfitsio library and NUMCPU is the machine core number.
The default installation path is in the same folder as the source code is (the program automatically creates the bin/ and lib/ subfolders). It can be set via --prefix=<NEW_INSTALLATION_PATH>
Finally create the executable:
make
Run the example models in the examples/ directory:
./DRAGON examples/run_2D.xml
or
./DRAGON examples/run_3D.xml
A detailed description of the input XML file and some examples can be found here.
Please let us know for any problem with installation!
We acknowledge here the use of external routines/table:
- dmspec.F Routines for calculating the annihilation spectrum from DarkSUSY package, to be cited as Gondolo et al., 2004
- MilkyWay_DR0.5_DZ0.1_DPHI10_RMAX20_ZMAX5_galprop_format.fits.gz The ISRF model used for the energy losses, to be downloaded from the GALPROP package (v54) and to be cited as Porter and Strong, 2008
- webber_xsec.dat Tabulated spallation cross sections, to be cited as Webber et al., 2003
- webber_xsec_total.dat Tabulated inelastic cross sections, to be cited as Webber et al., 2003
- cparamlib Library for secondary production in pp interactions from the cparamlib repository, to be cited as Kamae, et al., 2007
- tinyxml A C++ XML parser, from here
We include the routines and data tables taken from the public version of GALPROP. In more detail, the material included in our code contains: 1) the nuclear reaction network, built using the Nuclear Data Sheets; 2) the isotopic cross section database built using the T16 Los Alamos compilation Mashnik et al., 1998 and the CEM2k and LAQGSM codes Mashnik et al., 2004; 3) fits to some particular channels of isotopic production cross section Moskalenko et al., 2001, Moskalenko et al., 2003, Moskalenko et al., 2003b; 4) phenomenological approximations adapted from Webber et al., 1990 and Silberberg et al., 1998; 5) inelastic cross section database adapted from Barashenkov and Polanski, 1994
Specific files from GALPROP are listed below.