All Tables

Table 1: Sample of PCEBs with orbital periods $P\protect\la~2$ days, $\mbox{$M_{\rm 1}$ }>\mbox{$M_{\rm sec}$ }$ and a main-sequence secondary star.
Table 2: The properties of the PCEBs calculated in Sects. 5-7. If there is no reference given in the table, the distance is obtained from the references listed in Table 1. The time until the mass transfer is expected to start ( $\mbox{$t_{\rm sd}$ }$ ) is calculated using Eqs. (8), (9) (CMB) and Eq. (10) (RMB). The total time until the system becomes semi-detached, $t_{{\rm tot}}$ is given by the sum of the present cooling age, $t_{{\rm cool}}$ , the estimated MS lifetime of the primary, $t_{{\rm evol}}$ , and $\mbox{$t_{\rm sd}$ }$ . PCEBs with $t_{{\rm tot}}$ less than a Hubble time are marked in bold. For the systems RR Cae, EG UMa, EC 13471-1258, BPM 71214 and V471 Tau we find the properties of the progenitor of the PCEB (orbital period $P_{{\rm CE}}$ , primary mass $M_{1,{\rm pCE}}$ and, $t_{{\rm evol}}$ ) depending on the assumed AML (see text). In these cases, the second line gives the results assuming reduced magnetic braking (RMB) whereas the first line corresponds to the classical magnetic braking assumption (CMB). $f_{{\rm PCEB}}$ gives the mean fractional PCEB life time that the system has already passed through. The orbital period at which the PCEB starts mass transfer $\mbox{$P_{\rm sd}$ }$ is independent on the assumed angular momentum loss.