Hello Roland,<div><br></div><div>thanks for the quick reply...</div><div><br></div><div>when i did the collapse (with less refinement levels and resolution due to RAM restrictions on my iMac) the code crashes as well after the Bh has been formed...when using AHfinderDirect, the simulation stops upon the following error:</div>
<div><br></div><div><div>[1mWARNING level 0 in thorn AHFinderDirect processor 0 host <a href="http://permeability.daa.uv.es" target="_blank">permeability.daa.uv.es</a></div><div> (line 78 of /Users/vass/programs/Cactus/arrangements/EinsteinAnalysis/AHFinderDirect/src/jtutil/error_exit.cc): </div>
<div> -> [0m ***** row_sparse_Jacobian__UMFPACK::solve_linear_system():</div><div> error return status=1 from umfpack_numeric() routine</div><div><br></div><div>and when running without the AHFinderdirect, the run produces meaningless results (the density maximum and minimum as well as the lapse min and max get set to <span style="background-color:rgb(255,255,255);font-family:arial,sans-serif;font-size:13px">1.797693e+308 and -1.797693e+308</span>) however, there are no NaNs caught by the NaNChecker...</div>
<div><br></div><div>thanks for pointing out the trigger thorn, is it triggering more refinement levels once the density has reached a certain threshold?</div><div><br></div><div>what about the general stability of simulations after a BH has been formed? is it yet possible to evolve the system for a long time after the formation of a BH, using the current tools available in the ET? i am asking this because we are interested in gravitational collapse of NS triggered by winds past the NS and it would be desirable to observe the long term evolution of the NS-wind and later BH-wind system...</div>
<div><br></div><div>best wishes,</div><div><br></div><div>Vassili</div>
<div><br><div class="gmail_quote">On Mon, Jul 23, 2012 at 7:31 PM, Roland Haas <span dir="ltr"><<a href="mailto:roland.haas@physics.gatech.edu" target="_blank">roland.haas@physics.gatech.edu</a>></span> wrote:<br><blockquote class="gmail_quote" style="margin:0 0 0 .8ex;border-left:1px #ccc solid;padding-left:1ex">
Hello Vassilios,<br>
<div><br>
> the plot shows the evolution up to a time of roughly 180 (in M_sun)...my<br>
> first question is: for how long in total was the simulation running? for<br>
> how much longer is the evolution stable AFTER the BH has been formed? does<br>
> the code eventually crash or was there only interest in showing<br>
> the successful collapse and then stop the simulation manually after that<br>
> point?<br>
</div>I ran the NS collapse run for the paper.<br>
Mostly there was only interest in getting the collapse. The code fails<br>
shortly after that though (with NaNs inside the AH I think is what it was).<br>
<div><br>
> furthermore, in the tov_collapse_vc_l3.par file for the collapse for the<br>
</div>> paper there the following parameters for a thorn *corecollapsecontrol* the<br>
> following section:<br>
These have to go. I'll put up a replacement that uses public thorns<br>
(CoreCollapseControl is not yet public [though there are no objections<br>
to making it public from the author]).<br>
<br>
> what is this *corecollpasecontrol* thorn doing? and where can it be<br>
<div>> obtained if it is necessary for successful simulations of NS to BH collapse?<br>
</div>It does many things but we only really need functionality to steer some<br>
grid functions.<br>
<br>
I attach an updated parameter file which uses Frank Loeffler's Trigger<br>
thorn (<a href="https://docs.einsteintoolkit.org/et-docs/Thorns_we_know_of" target="_blank">https://docs.einsteintoolkit.org/et-docs/Thorns_we_know_of</a>).<br>
Please let me know if this solves your problem (I only tested that I can<br>
start it), then I can (barring protests from the other authors), update<br>
the parameter file in the repository.<br>
<br>
Yours,<br>
Roland<br>
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<br></blockquote></div><br></div></div>