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LORENE is a public C++ software developed to solve partial differential equations in numerical relativity by means of multi-domain spectral methods. The code is developed by Eric Gourgoulhon, Philippe Grandclément, Jean-Alain Marck, Jérôme Novak and Keisuke Taniguchi, at the Meudon Section of Paris Observatory, at LUTH laboratory. For more details about LORENE history and a complete list of contributors, click here. The main references are:

  • E. Gourgoulhon, P. Grandclément, K. Taniguchi, J.-A. Marck, S. Bonazzola, Phys. Rev. D 63, 064029 (2001)
  • K. Taniguchi, E. Gourgoulhon, S. Bonazzola, Phys. Rev. D  64, 064012 (2001)
  • K. Taniguchi, E. Gourgoulhon, Phys. Rev. D 65, 044027 (2002)
  • K. Taniguchi, E. Gourgoulhon, Phys. Rev. D 66, 104019 (2002)
  • K. Taniguchi, E. Gourgoulhon, Phys. Rev. D 68, 124025 (2003) 
  • M. Bejger, D. Gondek-Rosinska, E. Gourgoulhon, P. Haensel, K. Taniguchi, J.L. Zdunik, Astron. Astrophys. 431, 297 (2005)

Summary   of   initial   data   files   for   Lorene: 
 * These   data   files   are   uniform   throughout   all   of   our   EOS   folders 
 The   Initial   data   library   has   these   Equation   Of   State’s   :   AP3,   AP4,   MS1,   MS1b,   Sly, 
 WFF1,   and   MPA   1   with   the   following   configurations 
M1  M2 
1.4  1.4 
1.6  1.4 
1.8  1.4 
 2    1.4 
● calcul.d.DISTANCE: Contains   all   of   the   initial   information   for   the   coalescence 
 (coal)   sequence.   It   describes   the   physical   parameters   of   each   isolated   star 
 (baryon   mass,   EOS,   enthalpy,   densities,   coordinate   positions,   etc.)   and   the 
 physical   parameters   for   the   stars   in   a   binary   configuration.  

● ini.d: Necessary   to   have   for   the   coal   routine   to   run.  

● logfile_coal_seq_DISTANCE: The   complete   log   of   the   coal   sequencing   routine 
 for   the   distance   steps   specified.  

● logfile_init: The   complete   output   file   for   the   initial   binary   routine,   init_bin.   This 
 contains   information   such   as   the   mass   (gravitational   and   baryon),   radius,   and 
 compact   parameter   for   the   corresponding   enthalpy   value   of   the   star.   It   is   where 
 you   look   to   get   the   input   mass   parameter   for   the   coal   routine.  

● parcoal_seq_massscan.d: Parameter   file   for   the   binary   computation   for   the 
 coal   routine.   This   is   where   you   fix   the   specific   parameters   you   want   for   your 
 system   (i.e   starting   and   ending   masses,   starting   and   ending   separation   distance, 
 the   distance   step,   relaxation   parameters,   etc.) 
● par_eos1/2.d: Separate   equation   of   state   parameter   files   for   each   star   (denoted 
 by   the   labels   1   and   2).   This   is   where   you   specify   the   type   of   EOS   for   the   stars, 
 and   where   the   corresponding   polytropes,   adiabatic   indices,   and   fiducial   density 
 values   are   located.   This   file   is   generated   by   our   TOV   solving   code.   You   just   need 
 to   copy   it   and   rename   it   for   your   respective   stars.  

● par_grid1/2.d: Separate   multi   domain   grid   parameter   files   for   each   star.   You   can 
 specify   the   number   of   domains   and   grid   points   within   each   domain.  

● par_init.d:This   is   where   you   set   the   initial   conditions   for   each   star.   This   is 
 necessary   in   order   to   run   the   init_bin   routine.   You   can   specify   the   enthalpy   values (which   determines   both   mass   and   radius   for   each   star,   and   can   be   found   in   the 
 logfile   for   init_bin),   along   with   relativistic   vs.   newtonian   computations,   and   the 
 star’s   rotational   state. 

 ● res_files_DISTANCE: A   tar   file   containing   all   of   the   output   files   from   the   coal 
 routine.   It   includes   the   files   resconv1/2_DISTANCE,   resdiffm_DISTANCE, 
 resformat_DISTANCE,   resglob_DISTANCE,   resrota_DISTANCE,   and 
 resstar1/2_DISTANCE.   These   all   contain   different   information   about   the   output   of 
 the   stars.  

● resu_DISTANCE.d:  this   file   is   needed   as   an   input   in   the   EinsteinToolkit 
 Dynamical   Evolution   code   for   the   respective   separation   distance   that   you   wish   to 
 NOTE: The   Sly   equation   of   state   has     as   the   lighter   mass   star   and   as    the M1 M2 heavier   mass   star. 

Documentation Link
: Eric Gourgoulhon, Philippe Grandclément,Jérôme Novak.
CCRG Contributors
: Eric Gourgoulhon, Philippe Grandclément, Jérôme Novak.
Short Description
Public numerical relativity software using multi-domain spectral methods