TOV 2

University of Heidelberg

Wicker, M. M. Umar, M.

This is an interactive, numerical, python based solver, designed to solve the Tolman-Oppenheimer-Volkoff equation in the context of the internal structure of a neutron star. In the following you will be able to determine the internal density, mass and pressure profiles for a varity of different physical assumptions. You also will be able to investigate the effect of different equations of state (EoS), total masses and central densities on the other characterizing quantities of a neutron star. In the next section you can modify the intial setup used for the calculations and start the simulation.

Initial Parameters

Please insert your desired initial parameters. The pre-selected options are the default set-up for a 1.5 solar masses neutron star following a polytropic equation of state. Under certain circumstances some of the put in parameters are not needed, if you choose a certain kind of simulation. These parameters can be left at their defaults. For more details on the parameter the user is refered to the documentation of the source code. A short description can also be obtained by placing the cursor over the input fields.

Equation of State (EOS):	LALSimNeutronStar_ALF1 LALSimNeutronStarEOS_ALF2 LALSimNeutronStarEOS_ALF3 LALSimNeutronStarEOS_ALF4 LALSimNeutronStarEOS_AP1 LALSimNeutronStarEOS_AP2 LALSimNeutronStarEOS_AP3 LALSimNeutronStarEOS_AP4 LALSimNeutronStarEOS_APR LALSimNeutronStarEOS_APR4_EPP LALSimNeutronStarEOS_BBB2 LALSimNeutronStarEOS_BGN1H1 LALSimNeutronStarEOS_BHF_BBB2 LALSimNeutronStarEOS_BPAL12 LALSimNeutronStarEOS_BSK19 LALSimNeutronStarEOS_BSK20 LALSimNeutronStarEOS_BSK21 LALSimNeutronStarEOS_ENG LALSimNeutronStarEOS_FPS LALSimNeutronStarEOS_GNH3 LALSimNeutronStarEOS_GS1 LALSimNeutronStarEOS_GS2 LALSimNeutronStarEOS_H1 LALSimNeutronStarEOS_H2 LALSimNeutronStarEOS_H3 LALSimNeutronStarEOS_H4 LALSimNeutronStarEOS_H5 LALSimNeutronStarEOS_H6 LALSimNeutronStarEOS_H7 LALSimNeutronStarEOS_HQC18 LALSimNeutronStarEOS_KDE0V LALSimNeutronStarEOS_KDE0V1 LALSimNeutronStarEOS_MPA1 LALSimNeutronStarEOS_MS1 LALSimNeutronStarEOS_MS1B LALSimNeutronStarEOS_MS1B_PP LALSimNeutronStarEOS_MS1_PP LALSimNeutronStarEOS_MS2 LALSimNeutronStarEOS_PAL6 LALSimNeutronStarEOS_PCL2 LALSimNeutronStarEOS_PS LALSimNeutronStarEOS_QMC700 LALSimNeutronStarEOS_RS LALSimNeutronStarEOS_SK255 LALSimNeutronStarEOS_SK272 LALSimNeutronStarEOS_SKA LALSimNeutronStarEOS_SKB LALSimNeutronStarEOS_SKI2 LALSimNeutronStarEOS_SKI3 LALSimNeutronStarEOS_SKI4 LALSimNeutronStarEOS_SKI5 LALSimNeutronStarEOS_SKI6 LALSimNeutronStarEOS_SKMP LALSimNeutronStarEOS_SKOP LALSimNeutronStarEOS_SLY LALSimNeutronStarEOS_SLY2 LALSimNeutronStarEOS_SLY4 LALSimNeutronStarEOS_SLY9 LALSimNeutronStarEOS_SLY230A LALSimNeutronStarEOS_SQM1 LALSimNeutronStarEOS_SQM2 LALSimNeutronStarEOS_SQM3 LALSimNeutronStarEOS_WFF1 LALSimNeutronStarEOS_WFF2 LALSimNeutronStarEOS_WFF3
SuSu-Core Mass of Neutron Star (wanted) in Solar Masses [Msusu]:
Central Density [Nuclear Densities]:
Central-Density we want to Reach:
Maximum Number of steps:
Step at Outer Radius:
Minimum density where to quit:
Do You Want to Plot the Final Model?:
Do You Want to Save Final Model?:
Path to Save Results (Don't change it):

By clicking on the "Start Simulation" button the set initial conditions are used to solve the TOV equations. If additional costumization is desired, the complete python code can be downloaded and imported as python modules as usual. Examples for usage are included.