This directory has a set of tests for MESA/STAR.

They are run regularly to check revisions of the code.

The tests are also useful as a collection of examples
of how mesa/star works for a variety of cases.

Each test can be run independently, so if you see
one you'd like to try, cd to the directory
and do ./mk and ./rn


sample_zams
   load and check a few prebuilt zams models

brown_dwarf
   evolve 0.02 Msun checking L and Teff at various ages
      1 Myr, 10 Myr, 100 Myr, 1 Gyr, and 10 Gyr.
   use tau=100 non-grey atm model.
   compare to Baraffe 03 results.

pulse
   call the pulse module to get results for a solar model

very_low_mass
   evolve 0.001 Msun from birth to 10 Gyr.

multimass
   give list of masses to be evolved using the same controls
   e.g., produce isochrone by using max_age to determine when to stop.

high_mass
   run a very massive star from zams to central hydrogen depletion

low_z
   run 0.08 Msun, Z = 1e-4 from pre-ms until Teff > 6600

solar
   1 Msun from pre-main-sequence to solar age

rlo
   Roche lobe overflow until donor mass drops to 0.02 Msun

he_core_flash
   from tip of RGB until helium burning reaches center

pre_zahb
   evolve 1 Msun from start of central He burn until center Y < 0.75

hb_2M
   evolve 2 Msun during He burn until create C core of 0.25 Msun

agb
   from early AGB through a few thermal pulses

c13_pocket
   check formation of c13 pocket during AGB pulse

wd
   accrete solar composition onto WD until get ignition

wd2
   accrete solar composition at high enough mdot to reach steady burning

wd3
   accrete pure He onto WD until get ignition

wd_ignite
   accrete C/O onto WD until get ignition at center

wd_cool
   1M after leaving AGB until cool WD

ns_h
   accrete solar composition onto neutron star until get ignition

ns_he
   accrete pure He onto neutron star until get ignition

ns_c
   accrete pure C onto neutron star until get ignition

sswind
   mass loss from supersonic wind

sewind
   mass loss from super-Eddington luminosity wind
      
multiple_stars
   evolve 3 stars simultaneously until all have reached a given age.
      at each step, evolve the youngest star

create_zams

sample_pre_ms
   
create_zahb

make_inert_core

make_metals

make_he_wd

make_co_wd

0.2M_pre_ms_to_zams

agb_to_wd

binary_rlo

neutron_star_envelope

irradiated_planet

check_vlm_models

check_wd_models

limit_max_opacity

0.001M_tau1_atm

semiconvection

15M_dynamo

1M_thermohaline










longer tests ("overnight")

1M_pre_ms_to_wd
   full evolution of M = 1 Msun, Z = 0.02 from pre-ms to cool wd
   
15M_si_burn
   from Si burn to onset of core collapse
   
40M_z1m4_to_si_burn
   from pre-ms to start to create 56Cr at center
   
solar_calibration
