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    4. QuarkStars binaries

    All of the presented models are described in Wiktorowicz et al. 2017. Total simulated stellar mass is 2.9e8 solar masses.

    Files are named in the following way: zZZZ_mMM_dD.dat

    ZZZ represents a mantissa of metallicity (e.g. 02 refers to metallicity equal 0.02)
    MM is the deconfinement mass multiplied by 10, e.g. 15 means deconfinement mass of 1.5 Msun (see Wiktorowicz et al. 2017 for details).
    D is the data type: 0 - NS/QS in binaries; 1 - QS formation.
    For example, if you wish to see QS formation information for solar metallicity (Z=0.02) and lower value of deconfinement mass 1.5 Msun you should choose z02_m15_d1.dat file.

    Each line of the files for which D equals 0 contains information about one evolutionary timestep of a binary with NS/QS component. The format is as follows:

    QSn,mt,t,dt,Ma,Mb,a,e,Ka,Kb,Mzamsa,Mzamsb,a0,e0,idum,iidd,evroute

    [Units are in square brackets]

    • QSn: 0 - only NSs are present in the system; 1 - priamry is QS; 2 - secondary is a QS; 3 - double QS
    • mt is 0/1 when mass transfer is off/on
    • t is the age of the system (i.e. time since ZAMS) [Myr]
    • dt is the length of the timestep [Myr]
    • Ma/Mb is a mass of the priamry/secondary [Msun]
    • a is a semi-major axis [Rsun]
    • a is the semi-major axis of the system [Rsun]
    • e is an eccentricity
    • Ka is a type of the primary (see below)
    • Kb is a type of the secondary (see below)
    • Mzamsa is the initial (at ZAMS) mass of the primary component [Msun]
    • Mzamsb is the initial (at ZAMS) mass of the secondary component [Msun]
    • a0 is the initial (at ZAMS) separation (semi-major axis) of the components [Rsun]
    • e0 is the initial (at ZAMS) eccentricity of the binary.
    • idum, iidd are identifiers of a system (i.e. all lines with identical idum and iidd refer to the same binary)
    • evroute is a symbolical description of binary evolution (see below)


    Each line of the files for which D equals 1 contains information for the deconfinement process. The format of the files is as follows:

    QSf,inbin,t,Maold,Ma,Mbold,Mb,Ka,Kb,a,e,aold,eold,Mzamsa,Mzamsb,a0,e0,idum,iidd,evroute

    [Units are in square brackets]
    • QSf shows which star has became a QS (1 - primary, 2 - secondary)
    • inbin indicates if stars are still bound
    • t is the age of the system (i.e. time since ZAMS) [Myr]
    • Maold/Ma is the mass of the primary prior/after the deconfinement [Msun]
    • Mbold/Mb is the mass of the secondary prior/after the deconfinement [Msun]
    • Ka is a type of the primary (see below)
    • Kb is a type of the secondary (see below)
    • aold,a is the semi-major axis of the system prior/after the deconfinement [Rsun]
    • eold,e is the eccentricity of the system prior/after the deconfinement
    • Mzamsa is the initial (at ZAMS) mass of the primary component [Msun]
    • Mzamsb is the initial (at ZAMS) mass of the secondary component [Msun]
    • a0 is the initial (at ZAMS) separation (semi-major axis) of the components [Rsun]
    • e0 is the initial (at ZAMS) eccentricity of the binary.
    • idum, iidd - identifiers of a system (i.e. all lines with identical idum and iidd refer to the same binary)
    • evroute is a symbolical description of binary evolution (see below)

    The list of phases used to describe evolutionary history (evroute):
    MTx - stands for non-conservative mass transfer through Roche lobe overflow. "x" indicates the donor: 1-primary, 2-secondary.
    SNx - stands for a supernovae explosion.
    CEx(a0-b0:a1-b1) - stands for a common envelope events. "x" indicates the donor star: 1-primary, 2-secondary or 12-both components are donors.
    "a0-b0" are integer numbers indicating stellar types (explained below) of the primary-secondary components, respectively, at the start of the CE.
    Analogously "a1-b1" indicate stellar types at the outcome of the CE. For example "CE2(14-2:14-7)" means that a CE was initiated by the secondary component ("CE2"), which was a Hertzsprung gap star ("-2:"), onto the primary, which was a black hole ("14-").
    In the outcome, the secondary ejected its hydrogen envelope and became a Wolf-Rayet star ("-7"), while the primary remained a black hole (":14-").
    AICtypex indicates an accretion induced core collapse.
    "type" describes the compact object to which the progenitor has collapsed and "x" - the relevant component: 1-primary, 2-secondary. For example "AICQS1" means that the accreting primary star ("1") has collapsed into a quark star ("QS").

    List of stellar types:

    • 0 - main sequence star with M<=0.7 M☉ (deeply or fully convective)
    • 1 - main sequence star with M>0.7 M☉
    • 2 - Hertzsprung gap star
    • 3 - first giant branch star
    • 4 - core helium burning star
    • 5 - early asymptotic giant branch star
    • 6 - thermally pulsing asymptotic giant branch star
    • 7 - main sequence naked helium star (Wolf-Rayet star)
    • 8 - Hertzsprung gap naked helium star
    • 9 - giant branch naked helium star
    • 10 - helium white dwarf
    • 11 - carbon/oxygen white dwarf
    • 12 - oxygen/neon white dwarf
    • 13 - neutron star/quark star
    • 14 - black hole


    List of QuarkStars files