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The stability of massive main-sequence stars as a function of metallicity

"The stability of massive main-sequence stars as a function of metallicity" by Joshua H. Shiode, Eliot Quataert, & Phil Arras (2012). Pulished in MNRAS, vol. 423, p. 3397-3404 This folder contains inlists and pre-MS models used to create models of 120 -- 1000 solar mass, Population III, non-rotating stellar models evolved from ZAMS to center hydrogen mass fraction of 0.4 (stopped before TAMS due to difficulties evolving the highly radiation-dominated stellar envelope).

Inlist for evolving Pop III stars along Main Sequence

To run masses other than 120, simply modify "saved_model_name = '###z0_prems.mod'" to point to the pre-MS model with the relevant mass.

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Pre-MS models

Archive with all pre-MS models used for MS evolution of Pop III stars. Also includes pre-MS model for 120 solar mass, solar metallicity model. To reproduce metallicity study at 120 solar masses, read in either 120 solar mass pre-MS model and use the following lines in &star_job: load_saved_model = .true. saved_model_name = '120z0_prems.mod' relax_Z = .true. new_Z = [some new metallicity] set_initial_model_number = .true. initial_model_number = 0 save_model_number = 1 save_model_filename = '120z[new metallicity]_prems.mod' and then restart by reading in the new save_model_filename and commenting out these additional lines.

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