A collection of modules for computing neutron star structure and evolution.
The code has been updated to use
mesa version 10398.
This required (finally) getting rid of tabs, explicity specifying
dp in a few places, and changing
INTENT() on a few interfaces.
A tutorial on crust cooling
Look in the
examples/INT-16-2b-demo directory for a demonstration of using this code that was presented in a talk given at the INT workshop 16-2b, "Phases of Dense Matter". See the
README.md file in that directory for instructions.
Total mass, radius are now reported
profile datafiles now list the total mass (solar units) and radius (kilometers) in the header. By total, I mean the value at the top of the domain, not the photosphere.
Multiple accretion epochs can be specified
You can now specify a run with a number of accretion "epochs": distinct periods of time with a different accretion rate. For example, suppose you wish to accrete at 1.5e17 g/s for 1000 d (starting at t = 0 d) and then cool for 5000 d (that is, from t = 1000 d to t = 6000 d). In the inlist, you would set the following flags.
number_epochs = 2 epoch_Mdots = 1.5e17,0.0 epoch_boundaries = 0.0,1000.0,6000.0
You can also use this to specify times at which you want the surface effective temperature recorded. For example, suppose we want the surface effective temperature 50 d, 100 d, 500 d, 1000 d, 2000 d, and 5000 d after the end of the outburst in the above example. We would then put the following in the inlist.
number_epochs = 7 epoch_Mdots = 1.5e17,6*0.0 epoch_boundaries = 0.0,1000.0,1050.0,1100.0,1500.0,2000.0,3000.0,6000.0
We can make this even more convenient by setting the end of the outburst at t = 0 d.
number_epochs = 7 epoch_Mdots = 1.5e17,6*0.0 epoch_boundaries = -1000.0,0.0,50.0,100.0,500.0,1000.0,2000.0,5000.0
Time, observed effective temperature are stored
The structure pointer now contains arrays
Teff_monitor that contain the epoch end times (in days) and the observer-frame effective temperature (in K) at the end of each epoch. This facilitates comparison with observations.
Command line options
Check out the examples
custom_Tc_Qimp to see how to add command line options to your run.
Tools for reading output
tools/reader.py. This contains a python class for reading the output history and profile data files. The quantities are stored as class members for easy access when analyzing results.
dStarmakes use of the
MESAnumerical, utility, and equation of state libraries.
- MESA SDK: the compilation of both
dStarhas been tested using a specific build environment.
This version of
dStar has been tested with
MESA version 10398 and the 2018 January 27 (or later) version of the
How to install
- Follow the instructions on the MESA website to build a working version of
MESA, and ensure that the environment variable
MESA_DIRpoints to that directory.
- After forking or cloning the dStar repository, go into the top-level directory and type
./install. If you had compiled it previously, you should do a
./cleanfirst to force a clean install.
What the installation does
For each module, the install script
- Downloads, verifies, and installs to the
datadirectory the necessary data files. Note that the
md5utility is used first for checking data integrity. This may be an issue on linux systems which prefer
md5sum. If so, edit the
- Compiles each module as a library.
- Performs a test of each module and compares the output against a sample. A deviation from allowed tolerances results in a install failure.
- Installs the library and module files into the top-level
How to use
For each module, look in the
test directory for an example of how to run the module. The primary module is
For a basic example of how to run a neutron star model over an accretion/quiescent cycle, copy
examples/basic_run and follow the instruction in the
README.md file in that directory.
How to cite
If you do use
dStar, we'd appreciate a citation!
dStar is listed in the Astrophysics Source Code Library ascl:1505.034 and can be cited as, e.g.,
Brown, E. F. 2015, Astrophysics Source Code Library, ascl:1505.034
A bibliographic entry can be obtained from ADS.
- add load/save options for models
- ability to generate an atmosphere model with an arbitrary composition.
- Add environment variable pointer to root directory and allow cache directories to be in a user-specified location.