Neutron_Star_EOS

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Neutron_Star_EOS

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Neutron star equation of state files, includes TOV solver, unit conversion, and plots

Neutron_Star_EOS 최신버젼 다운로드

최종 버전 다운로드 (.zip)

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# Neutron_Star_EOS

== Table of Content ==

0. Codes and input files that produe the EoSs
1. Correspondence between EoS folders and paper figures
2. Files in the folders
3. Neutron star observation constraints

==== 0. Codes and input files that produe the EoSs ========================================================

To run the code, one requires the folder input_files, the Mathematica code, and a generic folder called output_files and output_files/TW (the generated EoS will be outputed here).  We have also uploaded the EoS folders as well but those are the output of the code and not required to run the code.

We include two different codes here, please cite the following papers: 
PRL_EOS_TOV.nb: Tan, Noronha-Hostler, Yunes, Phys.Rev.Lett. 125 (2020) 26, 261104 
PRD_Twins_TOV.nb: Tan, Dore, Dexheimer, Noronha-Hostler, Yunes to appear

If the SLy crust was used cite: 
E. Chabanat, P. Bonche, P. Haensel, J. Meyer, and R. Schaef-fer. A Skyrme parametrization from subnuclear to neutronstar densities. 2. Nuclei far from stablities.Nucl. Phys. A,635:231–256, 1998. [Erratum: Nucl.Phys.A 643, 441–441(1998)].doi:10.1016/S0375-9474(98)00180-8 
F. Douchin and P. Haensel. Inner edge of neutron star crustwith SLY effective nucleon-nucleon interactions.Phys. Lett.B, 485:107–114, 2000.arXiv:astro-ph/0006135,doi:10.1016/S0370-2693(00)00672-9. 
F. Douchin and P. Haensel. A unified equation of state ofdense matter and neutron star structure.Astron. Astrophys.,380:151, 2001.arXiv:astro-ph/0111092,doi:10.1051/0004-6361:20011402. 
F Douchin, P Haensel, and J Meyer. Nuclear surface andcurvature properties for SLy Skyrme forces and nuclei in theinner neutron-star crust.Nucl. Phys. A, 665:419–446, 2000.

==== 1. Correspondence between EoS folders and paper figures ======================================================== 
The EoS folder contains:

Fig.4 top -> /adjustedwidth 
Fig.4 bottom -> /peaklocation 
Fig.5 -> /endpoint 
Fig.6 -> /2bumpsfat

Fig.7 blue dotted dash -> /crust/QHC-125 
	red dash	 -> /endpoint_maxfull/eos3 
	green solid	 -> /crust/SKA-140 
	blue dash -> /crust/QHC-275 
	red solid -> /endpoint_maxfull/eos1 
	green dash -> /crust/SKA-300

Fig.8 -> /endpoint_maxfull

Fig.9 blue dash -> /peaklocation/eos1 
	pink solid -> /endpoint_maxFull/eos2 
	red dotted-dash -> /endpoint_maxfull/eos3 
	cyan solid -> /slanted_3M/eos1 
	green dash -> /endpoint_3M/eos4 
	megenta solid -> /2bumpsfat/eos1

Fig.11 purple dash -> TW/peakwide_longcs0/eos4 
	brown dotted-dash -> TW/peakwide_longcs0/eos2 
	blue solid -> TW/highhyb/eos1 
	green dash -> TW/peakwidthFIXL/eos1

Fig.12 blue dotted dash -> /TW/Blat_repeat/eos1 
	red solid -> /TW/Blat_repeat/eos3 
	green dash -> /TW/low_n_peak1st/eos2

Fig.13 -> /TW/peakwidthFIXL

Fig.14 purple dash -> /TW/pickFIX_PTwidth/eos1 
	deep green dash -> /TW/pickFIX_PTwidth/eos2 
	light green dash -> /TW/pickFIX_PTwidth/eos3 
	blue dot -> /TW/pickFIX_PTwidth/eos4 
	black solid -> /TW/pickFIX_PTwidth2/eos1 
	brown dotted dash -> /TW/pickFIX_PTwidth2/eos3 
	brown dash -> /TW/pickFIX_PTwidth3/eos4

Fig.15 -> /TW/slantendpoint 
Fig.16 -> /TW/endpoint

==== 2. Files in the folders =================================================================================

In each folder, there should be at least 3 types of files: EoS, mr, all observables

For EoS, the file name is eosX.dat, where X is a number. 
There are five columns in eosX.dat, which are 
baryon density[1/fm^3], pressure[MeV/fm^3], energy density[MeV/fm^3], speed of sound squared[], chemical potential[MeV]

For mr, the file name is mrX.dat, where X is a number. 
There are four columns in mrX.dat; the first three of them are: 
radius of NS[km], mass of NS[solar mass], central energy density[MeV/fm^2]

For files contain all observables, the file name is eosX_CntDens[MeV]_R[km]_M[Msun]_Ibar_Qbar_Love.dat 
There are 6 columns in the files, which are 
center energy density, radius of NS, mass of NS, dimensionless moment of inertia, dimensionless quadrupole moment, dimensionless Love number. 
The units are shown in the filenames, where MeV really means MeV/fm^3 and Msun means solar mass.

==== 3. Neutron Star observation constraints ==================================================================

GW170817: 
	publication: http://arxiv.org/abs/1805.11581 
	repository: https://dcc.ligo.org/LIGO-P1800115/public

GW190814: 
	publication: http://arxiv.org/abs/2006.12611

J0030+0451 Illinois-Maryland: 
	publication: http://arxiv.org/abs/1912.05705 
	repository: https://zenodo.org/record/3473466#.YMDjgTZKidY

J0030+0451 Amsterdam: 
 publication: https://arxiv.org/abs/1912.05702 
 repository: https://zenodo.org/record/3386449#.YMDkDjZKidY

J0740+6620 Illinois-Maryland: 
	publication: https://arxiv.org/abs/2105.06979 
	repository: https://zenodo.org/record/4670689#.YMDmSjZKidY

J0740+6620 Amsterdam: 
 publication: https://arxiv.org/abs/2105.06980 
 repository: https://zenodo.org/record/4697625#.YMDlZjZKidY

V723 Mon: 
	publication: https://arxiv.org/abs/2101.02212

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