X-ray binaries
All of the presented models are described in Wiktorowicz et al. 2017. Total simulated stellar mass was 2.9e9 solar masses.
Files are named in the following way: zZZZ_adAD_bh/ns.dat
ZZZ represents a mantissa of metallicity (e.g. 02 refers to metallicity equal
0.02)
AD is the accretion model (see Wiktorowicz et al. 2017 for details)
bh/ns for black hole and neutron star accretors, respectively.
For example, if you wish to see X-ray binaries with black holes for
metallicity 0.002 and logarithmic accretion model choose: z002_ad1_bh.dat
Each line contains information for one time-step for one system. The format of the files is as follows:
idum iidd t dt Ma Mb Ka a e Ra dMedd dMgain Lxmt dMdonor Lxdonor mttype tran Mzamsa Mzamsb a0 e0 evroute
[Units are in square brackets]
- idum, iidd - identifiers of a system (i.e. all lines with identical idum
and iidd refer to the same binary)
- t is the age of the system (i.e. time since ZAMS) [Myr]
- dt is the length of the actual time-step [Myr]
- Ma is the mass of the donor [Msun]
- Mb is the mass of the accretor [Msun]
- Ka is a type of the donor (see below)
- Kb is a type of the accretor (see below)
- a is the semi-major axis of the system [Rsun]
- e is the eccentricity of the system
- Ra is the radius of the donor [Rsun]
- dMedd is the Eddington limit for mass accretion
- dMgain is the mass accretion rate
- Lxmt is the isotropic X-ray luminosity
- dMdonor is the mass transfer rate
- Lxdonor is the maximal possible isotropic X-ray luminosity for actual mass
transfer rate
- mttype is the timescale of mass transfer (1 - nuclear, 4 - thermal, 5 -
mass transfer from white dwarf)
- tran is a flag telling if the system is transient or not
- 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.
- 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 "AICNS1" means that the accreting primary star ("1") has collapsed into a neutron star ("NS").
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
- 14 - black hole
- 17 - hybrid white dwarf
List of X-ray files
(English)
(Polski)