[mesa-users] negative age and rotation values in "OSC" file

[Martin C.]

I notice you have
    overshoot_f_above_burn_h_core = 0.01
    overshoot_f0_above_burn_h_core = 0.21
Shouldn't f> f0?

Martin


On Thu, Feb 16, 2017 at 11:46 AM, Juan Carlos Suárez <jcsuarez at iaa.es>
wrote:

> Hi!
> Well, at some point, some years ago, it seemed that glob(14) was the Teff
> but maybe it changed since.
> But I am really not sure about the source of this…
>
> OK so MESA in principle does not provide this information, so that we have
> to infer it from the
> photometric radius. If I understood correctly glob(2) is the photometric
> radius, right?
>
> JC
>
>
> On 16 Feb 2017, at 16:57, RICHARD H D TOWNSEND <townsend at astro.wisc.edu>
> wrote:
>
> Hi Juan Carlos —
>
> The OSC output routines are based on the description of the OSC file
> format given in the ESTA project:
>
> https://www.astro.up.pt/corot/ntools/docs/CoRoT_ESTA_Files.pdf
>
> According to this document, fields 14 and onwards of glob are not used. Do
> you have an updated description of the OSC file format which indicates
> glob(14) should contain Teff?
>
> cheers,
>
> Rich
>
> On Feb 16, 2017, at 9:54 AM, Juan Carlos Suárez <jcsuarez at iaa.es> wrote:
>
> Dear Richard and all,
>
> Thank you very much for your valuable help.
> Now we are able to construct a complete evolutionary track from PMS to
> TAMS (we are indeed interested in
> keeping the PMS models), with around 4K for the number of shells, and
> using the Eddington atmosphere.
> Taking a look to the OSC files, it seems that now everything is OK except
> for the effective temperature (corresponding
> to glob(14) which is now 0.00000 for all the models in the track).
>
> We have used the inlist attached to this email.
>
> JC
>
> On 11 Feb 2017, at 23:17, RICHARD H D TOWNSEND <townsend at astro.wisc.edu>
> wrote:
>
> Hi Juan Carlos —
>
> In your email below, I can spot quite a few different problems you’re
> running into. In each case I’ll try to explain what’s going on
>
> On Feb 10, 2017, at 12:26 PM, Juan Carlos Suárez <jcsuarez at iaa.es> wrote:
>
> Dear Richard,
>
> We have modified a little bit the previous “inlist” in order to include
> some atmosphere (the default simple atmosphere)
> since we are interested in working with the photosphere radius. So we
> decided to include the following options in the
> inlist (attached)
> ! if true, write atmosphere to pulse files
>
> add_atmosphere_to_pulse_info = .TRUE.
>
>
> Although it’s not the main cause of your problems below, I should mention
> that In MESA 8845 (and previous releases) there is a bug in the atmosphere
> writing routine. The code should output the same atmosphere as selected by
> the ‘which_atm_option’ parameter; however, in many cases (including the
> default ‘simple_photosphere’ atmosphere), the atmosphere written out is
> actually the ‘Paczynski_grey’ atmosphere. This bug is fixed in the
> development version of MESA, but only for a restricted set of atmosphere
> choices:
>
> Eddington_grey
> Paczynski_grey
> solar_Hopf_grey
> Krishna_Swamy
> grey_and_kap
>
> For other atmosphere options the code now halts — because there is
> insufficient information to construct the atmosphere structure.
>
> ! if true, add point for r=0 to pulse files
>
> add_center_point_to_pulse_info = .FALSE.
>
>
> In fact, it’s setting this flag to .FALSE. that ‘fixed’ the problem with
> age and rotation rate being overwritten (as discussed in the previous
> email) — the central second derivative data only gets calculated when
> add_center_point_to_pulse_info = .TRUE. (which itself is a bug — again,
> fixed in the development version)
>
> ! if true, add k=1 cell to pulse files
>
> keep_surface_point_for_pulse_info = .false.
> ! add double points at discontinuities
>
> add_double_points_to_pulse_info = .TRUE.
>
>
> This is what’s causing the (approximate) doubling of the number of points
> in the OSC files. This flag causes MESA to write out a double points when
> it detects a density discontinuity. The threshold for recognizing density
> discontinuities is set by the threshold_dlnrho_for_double_point flag.
> Since this flag defaults to zero, *every* pair of adjacent cells in the
> model is producing a double point!
>
> The fix is to set add_double_points_to_pulse_info = .FALSE., or to
> specify a non-zero value for threshold_dlnrho_for_double_point — e.g., 10.
>
>
> Curiously, it seems that now the problem of the negative ages and rotation
> values is solved, but we
> do not know why.
>
>
> See above!
>
> On the other hand unfortunately the computation halted with an error
>
> failed to open LOGS/profile686.data
> star_finish_step ierr          28
> after_step_loop ierr          28
>
> That is, it halted at model 686, while without the above options MESA
> reached the 905 models with no errors.
>
>
> I imagine the program halted because it ran out of disk space. You are
> writing out a profile *and* an OSC file after each timestep. Each profile
> file is ~15MB, and each OSC file is ~5MB. After 686 models, you have used
> up well over 10 GB of disk space.
>
> To get around this issue, you should consider the following approaches:
>
> *) Don’t set mesh_delta_coeff so small — you use 0.15, which results in
> very high resolution models (some might say over-resolved). 0.5 might be a
> better choice for this parameter.
>
> *) Only write out every N’th profile/OSC file, rather than all of them. To
> do this, set profile_interval = N
>
> *) Don’t bother writing out the pre-MS models, if you don’t need them.
> This can be achieved by doing two separate runs — an initial run with no
> profile/OSC file output, which terminates at the ZAMS. Then, do a restart
> and write out profiles/OSC files as necessary.
>
> In addition to this, with the above options it seems that MESA has doubled
> the number
> of mesh points (from 4K to 8K). Is that what we should expect? The 4K
> additional
> points are located at the atmosphere?
>
>
> No, as I mentioned above, every single model point is being written as a
> double point — not what you want!
>
> So, to sum up:
>
> *) Upgrade to the development version of MESA.
>
> *) Set add_atmosphere_to_pulse_data = .FALSE., or set which_atm_option to
> one of the atmosphere choices listed above.
>
> *) Set add_double_points_to_pulse_data = .FALSE., or specify a non-zero
> value for threshold_dlnrho_for_double_point.
>
> *) Adjust mesh_delta_coeff, set_profile_interval to reduce size of files,
> or run the pre-MS and MS parts separately.
>
> (Note also that some of the parameter names have changed, with the phrase
> ‘pulse_info’ changed to ‘pulse_data’)
>
> Hope that helps!
>
> cheers,
>
> Rich
>
>
> Thanks!
> JC
>
>
> On 9 Feb 2017, at 20:38, Juan Carlos Suárez <jcsuarez at iaa.es> wrote:
>
> Yes here it is!
> JC
>
> On 9 Feb 2017, at 20:05, RICHARD H D TOWNSEND <townsend at astro.wisc.edu>
> wrote:
>
> Hi Juan —
>
> Can you post the inlist file(s) that you’re using?
>
> Many thanks,
>
> Rich
>
> On Feb 9, 2017, at 12:43 PM, Juan Carlos Suárez <jcsuarez at iaa.es> wrote:
>
> Dear colleagues
>
> I am trying to compute a 1.5 Msun evolutionary model (with solar
> metallicity) from PMS to TAMS approx.
> We have set the options to obtain the .OSC files to be read by our
> oscillation codes.
>
> We found that for all the models the age provided has negative values.
>
> Moreover, although no option for rotation was included in the inlist (i.e.
> rotation should be zero)
> we obtain some models with rotation 0 but others with negative non-zero
> values
>
> Any idea?
>
> Thanks in advance!
>
>
> ------------------------------------------------------------
> --------------------------------------------------------
> Dr. Juan Carlos Suárez
>   Ramon y Cajal fellow at Física Teórica y del Cosmos Dept. University of
> Granada
>   Facultad de Ciencias. 18071. Granada. Spain
> jcsuarez at ugr.es | +34 958249056 <+34%20958%2024%2090%2056> |
> www.ugr.es/~fqm292/
>   Associate researcher at Stellar Physics Dept. IAA-CSIC
> Glorieta de la Astronomia s/n. 18008. Granada. Spain
> jcsuarez at iaa.es | +34 958230619 <+34%20958%2023%2006%2019> | www.iaa.es
> ------------------------------------------------------------
> --------------------------------------------------------
>
>
>
> <inlist_project>
>
>
>
> ------------------------------------------------------------
> --------------------------------------------------------
> Dr. Juan Carlos Suárez
>    Ramon y Cajal fellow at Física Teórica y del Cosmos Dept. University of
> Granada
>    Facultad de Ciencias. 18071. Granada. Spain
>  jcsuarez at ugr.es | +34 958249056 <+34%20958%2024%2090%2056> |
> www.ugr.es/~fqm292/
>    Associate researcher at Stellar Physics Dept. IAA-CSIC
>  Glorieta de la Astronomia s/n. 18008. Granada. Spain
>  jcsuarez at iaa.es | +34 958230619 <+34%20958%2023%2006%2019> | www.iaa.es
> ------------------------------------------------------------
> --------------------------------------------------------
> <inlist_project>
>
>
>
> ------------------------------------------------------------
> --------------------------------------------------------
> Dr. Juan Carlos Suárez
>     Ramon y Cajal fellow at Física Teórica y del Cosmos Dept. University
> of Granada
>     Facultad de Ciencias. 18071. Granada. Spain
>   jcsuarez at ugr.es | +34 958249056 <+34%20958%2024%2090%2056> |
> www.ugr.es/~fqm292/
>     Associate researcher at Stellar Physics Dept. IAA-CSIC
>   Glorieta de la Astronomia s/n. 18008. Granada. Spain
>   jcsuarez at iaa.es | +34 958230619 <+34%20958%2023%2006%2019> | www.iaa.es
> ------------------------------------------------------------
> --------------------------------------------------------
>
>
> ------------------------------------------------------------
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-- 
Martin C.
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