[mesa-users] Deuterium burning in PMS stars

Aaron Dotter aaron.dotter at gmail.com
Thu Dec 3 17:44:51 EST 2015

Hi Mike

Try adding one or more of these to you history_columns.list:

   ! the following add all of the isos that are in the current net

   ! add_center_abundances
   ! add_surface_abundances
   ! add_average_abundances
   ! add_log_center_abundances
   ! add_log_surface_abundances
   ! add_log_average_abundances

These will add all the isotopes in the current net to the history file and
you can monitor when h2 begins to be depleted.


On Fri, Dec 4, 2015 at 9:13 AM, Michal Simon <michal.simon at stonybrook.edu>

> Dear colleagues,
> Jayashree Toraskar, a colleague at the American Museum
> of Natural History, and I have been using MESA to calculate
> the evolutionary tracks of low-mass young stars.   For us
> low-mass means mostly 0.1 to 1.5 Msun and young means
> mostly from age 0.1 MY to 10-50 MY.  I don't want to face the
> complicationsof brown dwarfs and leave evolution off the MS sequence to the
> pros.
> I would like to identify the age when deuterium burning starts.
> Here I mean as given by MESA's way of computing age from
> the start of the star's collapse.
> In analogy with a history.list column for
>                             power_h_burn
> I thought that
>                             power_h2_burn
> would provide the information, but sadly that is not an allowed
> parameter.
> If worst comes to worst I could identify the age of D-burning onset
> by monitoring the temperature at the center but there must be
> a more accurate way of doing it.  We would appreciate any
> help you can give us.
> BTW, we have enabled
>                              change_initial_net = true   and
>                              new_network="pp_extra.net"
> and can monitor the Li7 abundance just fine.
> Cheers, Mike Simon
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