- One of the main binary parameter - a, semimajor axis or orbital period
of the system, P. You can choose in what units to input and output these
parameters.
M1- mass of the primary (initially more massive companion).
In solar units.
M2 or q. You can determine M2- secondary mass in solar units
(initially less massive companion),
or mass ratio, q=M2/M1 (always less or equial than unity).
E-orbital eccentricity.
T- time of the evolution of the system (in years). Calculations will
stop at the moment T.
B1 or Mu1. Initial magnetic field of the first compact star, B1, in gauss.
Or magnetic moment, Mu1, in Gauss*cm^3 (Mu1=B1*R^3, R- radius of the star).
B1 or Mu2. Initial magnetic field of the second compact star, B2, in gauss.
Or magnetic moment, Mu2, in gauss*cm^3.
Kick velocity. Additional velocity, the compact object
achieve after the supernova
explosion due to anysotropy of the collapse. The user can determine the
direction of the velocity: random direction or exactly determine by the
user. Kick velocity is determined separately for every star.
Maximum accretion rate into common envelope (CE). The user can choose
between two opportunities: Eddington luminosity and no limit.
Matter acception. How the normal star accept matter during the
Roche lobe overflow by its companion.
Common envelope efficiency. The efficiency of the angular momentum
loss during the CE stage.
Collapse mass fraction. During collapse not all matter
convert into the BH. Some fraction is lost. Here the user determine
the fraction which is NOT lost.
Oppenheimer-Volkov limit. The upper limit of the NS's mass.
Initial spin period of the NS and WD. The periods can be determined by the
user, or one can use momentum conservation condition, in that case
normal star rotation period will be used to calculate initial period of
the compact object.
Last modified: Mon Sep 13 06:45:09 MSD 2004