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parameters
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# ####### EOS parameters #######
eos_table_name = "./src/extra_code_and_tables/Hempel_SFHoEOS_rho222_temp180_ye60_version_1.1_20120817.h5"
####### Weak interaction parameters #######
directory = "./src/weakrates/tables/"
ravlic_rates = "ravlicrates.dat"
suzuki_rates = "suzukirates.dat"
lmp_rates = "lmprates.dat"
lmsh_rates = "lmshrates.dat"
oda_rates = "odarates.dat"
ffn_rates = "ffnrates.dat"
## Rate table priority hierarchy ##
isuzuki = 1
ilmp = 2
ioda = 3
iffn = 0
ilmsh = 0
iravlic = 4
iapprox = 5
# 0 indicates the table will not be used
# 1 indicates highest priority, if other tables have rates for a nuclei contained in this table, they will be ignored.
# CITATION NOTICE: By using the ilmp/ilmsh/iffn/ioda/iapprox flags you agree to cite the relevant publications in your work.
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| iffn | Fuller, G. M., Fowler, W. A., & Newman, M. J. (1982). |
| | Stellar weak interaction rates for intermediate-mass nuclei. |
| | II - A = 21 to A = 60. The Astrophysical Journal, 252, 715. |
| | http://doi.org/10.1086/159597 |
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| ioda | Oda, T., Hino, M., Muto, K., Takahara, M., & Sato, K. (1994). |
| | Rate Tables for the Weak Processes of sd-Shell Nuclei in Stellar Matter. |
| | Atomic Data and Nuclear Data Tables, 56(2), 231-403. |
| | http://doi.org/10.1006/adnd.1994.1007 |
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| ilmp | Langanke, K., & Mart\'{i}nez-Pinedo, G. (2000). |
| | Shell-model calculations of stellar weak interaction rates: |
| | II. Weak rates for nuclei in the mass range in supernovae environments. |
| | Nuclear Physics A, 673(1-4), 481-508. |
| | http://doi.org/10.1016/S0375-9474(00)00131-7 |
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| ilmsh | Langanke, K., & Mart\'{i}nez-Pinedo, G. (2003). |
| iapprox | Electron capture rates on nuclei and implications for stellar core collapse. |
| | Physical Review Letters 90, 241102. |
| | http://prl.aps.org/abstract/PRL/v90/i24/e241102 |
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| iftrqrpa| Giraud, S., Zegers, R. G. T., Brown, B. A., Gabler, J.-M., Lesniak, J., |
| | Rebenstock, J., Ney, E. M., Engel, J., Ravlić, A., Paar, N. |
| | Finite-temperature electron-capture rates for neutron-rich nuclei near N = 50|
| | and effects on core-collapse supernova simulation. |
| | https://doi.org/10.1103/PhysRevC.105.055801 |
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