SNR Modelling Program - version 1.1, January 2019
===================================================
Developed by Dr. Denis Leahy, Bryson Lawton and Jacqueline Williams
Description: A GUI program used to model supernova remnants.
Also attached are a set of animations of hydrodynamic simulations of supernova remnants (animations.zip) and
an animation (dEMdTvsT_n6_12.avi) of the Emission Measures and Temperatures for the shocked ISM and for the shocked ejecta.
These calculations for these animations are described in the astroph arXiv preprint 1902.08284.
Python requirements
-------------------
Note: Users are encouraged to use the provided executable file for Windows if
an appropriate version of Python is not already installed.
Python version >= 3.6
Required libraries:
- NumPy
- SciPy
- Matplotlib
The Anaconda distribution of Python (https://www.continuum.io/downloads) comes
with these libraries; however some distributions have a broken version of
Matplotlib. If the program does not run, try uninstalling Matplotlib and
replacing it using pip.
How to run
----------
Assuming Python has been added to the PATH, run from the
command line using "python snr.py"
Required files (must remain in the same folder):
- snr.py
- snr_calc.py
- snr_gui.py
- snr_plot.py
- data directory (should contain 30 files)
Program usage details
---------------------
Program takes supernova remnant (SNR) properties as user inputs and produces
the following outputs:
- Values at user-specified time: SNR radius, velocity, electron temperature
- SNR phase transition times
- Plots of SNR radius and velocity as functions of time
For some models, an additional set of outputs are produced by clicking the
"Emissivity" button. These outputs include:
- Emission measure
- Emission weighted temperature
- Total luminosity over a user-specified energy range
- Plots:
- Temperature as a function of radius
- Density as a function of radius
- Specific intensity as a function of impact parameter
- Luminosity as a function of energy
Abbreviations used:
- RS: reverse shock
- ED: ejecta-dominated
- ST: Sedov-Taylor
- PDS: pressure-driven snowplow
- MCS: momentum-conserving shell
- CISM: Cloudy ISM phase, starts at t_ST (defined in TM99)
Version 1.1 Changes
-----------------------------------
- Time when the reverse shock reaches the core's edge now displayed under transition times
- Time when the reverse shock reaches the center now displayed under transition times
- s=0 case now expanded to address the n=1,9,11,13 cases
- s=0 case constants replaced with more accurate ones
- s=2 case now expanded to address the n= 6,8,9,10,11,12,13,14 cases
- s=2 case had n=0,1,2,4 cases removed while solutions are improved
- Various fixes with the emissivity button for various models
- Fractional Energy Loss model input fixed
- Standard model data files updated with more accurate structure models from the Chevalier & Parker solutions
- Cloudy ISM model data files updated with more accurate structure models from White & Long solutions
- 5th model type "Sedov-Taylor" with zero ejecta mass added
- Various smaller bug fixes
-----------------------------------
See 2017 and 2019 arXiv papers (astrop-ph 1701.05942 and 1902.08284 ) for details of models used and associated
calculations.
This program is open source and is licensed under The 3-Clause BSD License.