[Users] McLachlan crash

[Vassilios Mewes]

hello Erik,

i have attached a plot of the minimum value of the lapse vs time....

here is the segment of the par file where i set the dissipation:

Dissipation::order = 5
Dissipation::vars = "
        ML_BSSN::ML_log_confac
        ML_BSSN::ML_metric
ML_BSSN::ML_trace_curv
        ML_BSSN::ML_curv
        ML_BSSN::ML_Gamma
        ML_BSSN::ML_lapse
        ML_BSSN::ML_shift
  ML_BSSN::ML_dtlapse
        ML_BSSN::ML_dtshift
"

best wishes,

Vassili


On Wed, Feb 27, 2013 at 4:45 PM, Erik Schnetter <schnetter at cct.lsu.edu>wrote:

> Vassili
>
> In my experience, one needs to "control" the puncture by ensuring that (a)
> things evolve only slowly there (keeping the lapse small) and (b) adding
> sufficient dissipation.
>
> What is the value of the lapse near the puncture?
> How much dissipation are you adding?
> To which variables are you adding dissipation?
>
> -erik
>
>
> On Wed, Feb 27, 2013 at 8:53 AM, Vassilios Mewes <vassilios.mewes at uv.es>wrote:
>
>> Hello all,
>>
>> still no success with the full evolution of BH+torus...
>>
>> i have attached the par file i have been using lately, in which i added
>> two more levels of mesh refinement, as Roland suggested, increased the
>> Dissipation order to 5th and removed the parameter
>> ML_BSSN::dt_lapse_shift_method = "noLapseShiftAdvection"..
>>
>> this has improved things a bit, but the L_inf norm of the hamiltonian
>> constraint still starts growing at around t=200 (after having decreased and
>> then having been rather constant up to that point) and then the simulation
>> will crash later (either due to the shift being nan at the puncture or by
>> detecting nans)
>>
>>
>> in the meantime, i have evolved a single puncture, the bondi accretion
>> onto a puncture and an "inverse cowling" (setting up the spacetime and
>> hydro variables of the BH+torus system but only evolving the spacetime),
>> all using the same parameters, and all of those work...its only the full
>> system of BH+torus when i run into problems...this is using the ET 2012.11.
>> release..
>>
>> do you have any ideas what might go wrong with the spacetime evolution
>> when evolving the full system?
>>
>> best wishes,
>>
>> Vassili
>>
>>
>> On Tue, Feb 12, 2013 at 2:07 AM, Roland Haas <
>> roland.haas at physics.gatech.edu> wrote:
>>
>>> Hello Vassilios,
>>>
>>> > as mentioned earlier in the ET phone call, i have attached the par file
>>> > used in the run...
>>> >
>>> > i tried checking for the nans in the output, but the last hdf5 output
>>> was
>>> > too many iterations earlier and they aren't visible in 1D ascii output
>>> > either
>>> >
>>> > as said, the puncture tracker actually aborted the run, not the nan
>>> > checker...
>>> Thank you for the parameter file. As a unsubstantiated guess, I would
>>> try what happens if you move the outer boundary further out. Right now
>>> it sits at 50M which I would find uncomfortably close if there is any
>>> say "junk" radiation (eg from setting up a BH with spin in flat
>>> background) present. I'd move it to at least 200M (ie two more levels of
>>> mesh refinement). Not sure how likely this explanation is since your
>>> NaNs appear after many (9) light crossing times.
>>>
>>> Yours,
>>> Roland
>>>
>>> --
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>>>
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>>
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>
>
> --
> Erik Schnetter <schnetter at cct.lsu.edu>
> http://www.perimeterinstitute.ca/personal/eschnetter/
>
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