[Mesa-users] New Public Release 10398

[Earl Bellinger]

Great! Good work everybody!

Where can we find the release? I don't see it in
    https://sourceforge.net/projects/mesa/files/releases/
but maybe I am just being impatient...

Best regards,
Earl


---
earlbellinger.com
Earl Bellinger, Ph.D. Candidate
Stellar Ages & Galactic Evolution Group
Max Planck Institute for Solar System Research

On Wed, Mar 21, 2018 at 10:47 PM, Evan Bauer <ebauer at physics.ucsb.edu>
wrote:

> Dear MESA Users,
>
> We’re happy to announce a new public release of MESA: version
> 10398. Release notes below.
>
> Cheers,
> Evan (on behalf of the MESA developer team)
>
>
>
>
> MESA 10398 Release Notes
>
>
> Equation of State: PTEH, DT2, and ELM (Bill)
>
> Several new options for the mesa/eos have been added, all aiming for more
> accurate partials for the Newton solver.  All of these new eos options use
> bicubic spline interpolation in tables of lnPgas, lnS, and lnE as a way to
> get numerically accurate 1st and 2nd partial derivatives with respect to
> lnRho and lnT.  The partials are directly calculated from the interpolating
> bicubic polynomials to give numerical accuracy, but this comes at a cost in
> thermodynamic consistency since the actual thermodynamic relations can only
> be approximated by bicubic splines.
>
> The new eos options are called “PTEH”, “DT2”, and “ELM”.  The PTEH tables
> are created using the approach of Pols, Tout, Eggleton, and Han (1995) as
> implemented by Paxton (2004) in a program derived from Eggleton’s stellar
> evolution code (1973).  PTEH extends the mesa/eos coverage to lower
> densities than allowed by OPAL (down to 10^-18 g cm^-3) and higher
> metallicity than covered (OPAL stops at Z = 0.04 while PTEH covers all Z).
>   When PTEH is enabled, it is used for low densities and for high Z in
> cases that for lower Z would be handled using data from OPAL/SCVH tables.
> In the old MESA EOS we fell back to HELM to provide approximate results for
> the cases now covered by PTEH.
>
> The mesa/star default controls enable PTEH for both low densities and high
> Z.
>
>       use_eosPTEH_for_low_density = .true.
>       use_eosPTEH_for_high_Z = .true.
>       Z_for_all_PTEH = 0.040d0
>       Z_for_any_PTEH = 0.039d0
>
> The two remaining new eos options, DT2 and ELM, provide high resolution
> tables in logRho and logT for values from mesa/eos for OPAL/SCVH values and
> for HELM respectively.  These cover a subset of the standard eos domain
> with standard eos results for logPgas, logS, and logE in a form suitable
> for bicubic spline interpolation in order to give 1st and 2nd partials with
> high numerical accuracy. However, since use of DT2 and ELM will give
> decreased thermodynamic consistency that might not be compensated for by
> better residuals, these are both disabled by default in mesa/star.
>
>       use_eosDT2 = .false.
>       use_eosELM = .false.
>
>
> Opacities (Josiah, Aaron)
>
> The opacity module (kap) underwent some internal restructuring.  The kap
> module now exposes only a single kap_get interface instead of separate
> kap_get_Type1 and kap_get_Type2 subroutines.  This has two user-visible
> consequences.
> * The control kappa_type2_logT_lower_bdy was removed.  That control was no
> longer needed, as the existing control kappa_blend_logT_lower_bdy now also
> applies to Type2 opacities.  All other related opacity controls (e.g.,
> use_Type2_opacities) remain unchanged in name and behavior.
> * Previously, there were separate "other" hooks for Type1 and Type2
> opacities.  Now, there is only one hook, other_kap_get.  It has the call
> signature of the previous Type2 hook, which is a super-set of the arguments
> to the Type1 hook (see star/other/other_kap.f90).
>
> In previous versions opacities where clipped to the edge values of the
> tables when logR=logRho-3logT+18<-8. This has been replaced for a blend to
> Compton opacities between logR=-7.5 and logR=-8.
>
>
> Element Diffusion (Evan)
>
> Fixed a bug in the ionization treatment for diffusion in the pressure
> ionization routine. This was due to a typo in the original paper that
> presented the ionization scheme. Restored the missing factor of rho^1/3
> thanks to a later presentation of this same scheme (Dupuis et al. 1992) and
> a note here: http://www1.astrophysik.uni-kiel.de/~koester/
> astrophysics/astrophysics.html.
>
> Added a user control (D_mix_ignore_diffusion) for when to ignore element
> diffusion in surface or core mixing regions. Previously, diffusion would be
> turned off for surface mixing regions of ANY strength, even very weak
> mixing where diffusion might still be relevant. Now this control is set to
> a D_mix of 10^5 (cm^2/s), so that mixing that will obviously overwhelm
> diffusion (like convection) will turn it off, but weaker mixing won’t.
>
>
> Gravity Darkening (Aaron)
>
> Added options to include gravity darkening, in the form of projected
> (surface-averaged) luminosities and effective temperatures of the star
> viewed along the equator and pole, to the history file.  Assumes the star
> is an oblate spheroid; see https://github.com/aarondotter/GDit for more
> info.
>       grav_dark_L_polar !Lsun
>       grav_dark_Teff_polar !K
>       grav_dark_L_equatorial !Lsun
>       grav_dark_Teff_equatorial !K
>
>
> Isomers (Frank, Josiah, Bill)
>
> The isomers of 26Al can now be added to a reaction network. To use them,
> include the isomers in your network specification file. Two examples
> include
>
> add_isos_and_reactions(
>    neut
>     h  1  1     ! hydrogen
>    he  4  4    ! helium
>    mg 25 25 ! magnesium
>    al26-1      ! ground state
>    al26-2      ! meta-stable excited state
>    )
>
> and
>
> include 'mesa_45.net'
> add_isos_and_reactions(
>   al26-1
>   al26-2
> )
> remove_iso(al26)
>
> One may use either al26 or al26-1 and al26-2. Reaction rates for the 26Al
> isomers with other isotopes are picked up from the JINA reaclib file.
> Reaction rates for al26-1 <-> al26-2 are from Gupta & Meyer (2001) [
> http://adsabs.harvard.edu/abs/2001PhRvC..64b5805G] and located in
> data/rates_data/rate_tables along with the new default rate_list.txt file.
>
> User-Beware:
> if you want a local rate_tables directory, http://mesa.
> sourceforge.net/star_job_defaults.html#rate_tables_dir,  and you want the
> 26Al isomers, then the two al26-1 <-> al26-2 rate files must be copied from
> their default location to your local rate_tables directory and your local
> rate_list.txt modified to include these two rates.
>
>
> Installation Debugging (Rob, Josiah)
> There is a new command, $MESA_DIR/help which outputs system information we
> need when debugging installation issues and/or MESA crashes. ./install will
> now also log its output to a file $MESA_DIR/build.log, if you have an
> installation issue please include this file when reporting an issue to
> mesa-users.
>
>
> Miscellaneous improvements (Rob, Josiah):
>
> You can now use the MESA_INLIST environment variable to set the name of
> the main inlist file when using MESA binary.
>
> The output cadence of MESA binary has been tweaked to that its behavior is
> the same as MESA star.  (If you use the same options, you should get output
> at the same steps.)
>
> There is now a flag b% need_to_update_binary_history_now, which if set
> forces binary history output to occur at the current step.
>
>
> Run_star_extras (Aaron)
>
> Put calls to extra_header_items back into standard_run_star_extras and
> provided working examples of how to call all of them.  These are useful for
> adding extra information to the history and profile headers beyond what is
> provided by default, such as including mixing_length_alpha in the history
> file header.
>
>
> Building with Other Compilers
>
> MESA currently does not compile with ifort.
> Other non-SDK compilers that are known to work (at the bit-for-bit level):
> Gfortran 7.3.1 (fedora 27)
>
>
> _______________________________________________
> mesa-users at lists.mesastar.org
> https://lists.mesastar.org/mailman/listinfo/mesa-users
>
>
>
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