- Table 1:
Initial models and their parametrisation:
*A*and are the rotation law parameter (Eq. (12)) and the ratio of rotational to gravitational energy, respectively. Larger values of*A*correspond to more rigidly rotating cores. is the sub-nuclear adiabatic index of our hybrid equation of state (see Sect. 2.2). - Table 2:
Parametrisation of the initial
magnetic fields for the models of series AaBbGg-DdMm by the radius
of the field generating current loop centered at
(parametrized by
*d*= 1, 2, 3, 4, 0) and the field strength in the core's center (parametrized by*m*= 10, 11, 12, 13). For models AaBbGg-D0Mm the field generating current loop is located at infinity yielding a uniform magnetic field throughout the entire core. - Table 3: Initial magnetic energy and typical values of the ratio of magnetic to gravitational energy (the exact values depend also on the hydrodynamic initial model and its gravitational energy) for the models of series AaBbGg-DdM12. The magnetic energy of models with can be obtained by a simple scaling relation, e.g. .
- Table D.1:
Some characteristic model quantities: the first two columns give the model name and the
classification of the GW signal (for the corresponding
non-magnetized model). Columns 3 and 4 give the time of bounce
(in milliseconds) and the maximum density at bounce
(in units of
). An exclamation mark behind the density value signifies that the maximum density of
the model exceeds the bounce density during the later evolution.
(Col. 5) and
(Col. 6) are the maximum GW amplitude (in cm) and
the corresponding magnetic contribution.
(Col. 7) is a
*rough*mean value of the wave amplitude (in cm) at some late epoch; no value is provided when the GW amplitude does not approach a quasi-constant asymptotic value. If the absolute value of this amplitude is large, the presence of an aspheric outflow at late epochs can be inferred. The following columns give the maximum value of the rotational (Col. 8) and the magnetic beta parameter (Col. 9), the time when reaches its maximum (Col. 10), and the corresponding beta of the toroidal field (Col. 11). If the magnetic field is still amplifying at the end of the simulation, an exclamation mark is added behind the table entry, and if the magnetic field is decreasing at this time, we give its final value in parentheses. - Table D.2:
Some characteristic model quantities (name of model given in Col. 1) at time
*t*(in msec; Col. 2) when the core has reached a quasi-equilibrium state. For models which do not reach a quasi-equilibrium state until the end of the simulation (e.g. type-II models with large scale core pulsations) we provide upper (top value) and lower (bottom value) bounds estimated from the values at maximum and minimum contraction. Columns 3 and 4 give the surface radius (in km) and the mass (in solar masses) of the quasi-equilibrium configuration, respectively. Since it is still surrounded by an (expanding) envelope of high density matter, the definition of its surface radius is somewhat uncertain. As the rotation rate (in ms), where is the angular velocity averaged over the angle , as well as the total magnetic field and (the absolute value of) its toroidal component (both in Gauss) vary strongly near the surface and on short time scales, the corresponding values in Cols. 5-7 should be used with care. Negative values of the rotation rate signify counter-rotating cores. Finally, in Cols. 8 and 9 we give the radii of the shock at the polar axis, , and at the equator, (both in cm), respectively. No entry in these columns implies that the shock has already left the computational grid.