All Tables

Table 1: Properties for the donor stars of some of our grid models with Z = 0.01 and $M_{\rm i} = 1.1~M_\odot$ at their period minimum. The first three columns list the orbital period initially (at the ZAMS) in days, at Roche-lobe overflow ( $P_{\rm rlof}$ ) in hours and the minimum period ( $P_{\rm min}$ ) in minutes. The next 11 columns show stellar properties at $P_{\rm min}$ : the age of the donor (since ZAMS), the logarithm of the mass transfer rate (expressed in $M_\odot~ {\rm yr}^{-1}$ ), the mass and luminosity of the donor, the logarithms of the effective temperature, the core temperature (both in K) and the central density (in g cm^-3), and the last four columns show the logarithms of the core and surface mass fractions of hydrogen and helium.
Table 2: Some properties for two of our grid models with Z = 0.01 and $M_{\rm i} = 1.1~M_\odot$ at selected orbital periods. First row: initial (ZAMS) parameters. Rows 2-6: the model with $P_{\rm i} = 0.75$ d and $P_{\rm min} = 39.5$ min. Rows 7-11: the model with $P_{\rm i} = 0.85$ d and $P_{\rm min} = 11.3$ min. $\dot{M}_{\rm tr}$ in Col. 3 is expressed in $M_\odot$ yr^-1 and $T_{\rm eff}$ in Col. 7 in Kelvin. The last five columns give the logarithm of the surface mass fractions of the elements described.
Table 3: Comparison between the orbital periods that lead to periods less than 30 min within a Hubble time and orbital periods that result from tidal capture with a 1.4 $M_\odot$ neutron star, for different secondary masses and Z = 0.01. Column 1: initial secondary mass, Cols. 2 and 3: initial period range that leads to ultra-short periods, Cols. 4 and 5: RLOF-period period range that leads to ultra-short periods, Cols. 6 and 7: ZAMS and TAMS radii, Cols. 8 and 9: orbital periods for a circularised binary with capture distances of $1 \times R_{\rm zams}$ and $3 \times R_{\rm tams}$ . Masses are in $M_\odot$ , radii in $R_\odot$ and periods in days.