\begin{table}%t2
   \caption{Characteristic frequencies of the expected spectral energy distributions. \label{freq}}
   \small%\centerline
{
  \begin{tabular}{@{}lrrrrrr@{}}
\hline\hline
\ls & \multicolumn{3}{c}{Periastron $d_{\rm s}=0.1$~AU}	& \multicolumn{3}{c}{Apastron $d_{\rm s}=0.2$~AU} \\
\hline\noalign{\smallskip}
& $2\times 10^{11}$~cm & 100~keV & 0.4 TeV & $4\times 10^{11}$~cm & 200~keV & 0.4~TeV\\
& \\
\lsi & \multicolumn{3}{c}{Periastron $d_{\rm s}=0.1$~AU}	& \multicolumn{3}{c}{Apastron $d_{\rm s}=0.7$~AU} \\
\hline\noalign{\smallskip}
polar	& $8\times 10^{11}$~cm & 100~keV & 0.8 TeV & $4\times  10^{12}$~cm & 15~keV & 0.5~TeV \\
equatorial	& $5\times 10^{10}$~cm & 6~keV & 0.05~TeV & $2\times 10^{12}$~cm & 5~keV & 0.3~TeV\\
&\\
\psrb	& \multicolumn{3}{c}{Periastron $d_{\rm s}=0.7$~AU}	& \multicolumn{3}{c}{Apastron $d_{\rm s}=10$~AU} \\
\hline\noalign{\smallskip}
polar 	& $3\times 10^{12}$~cm & 12~keV & 0.5~TeV & $4\times 10^{13}$~cm & 1~keV & 0.5~TeV \\
equatorial	& $10^{12}$~cm & 4~keV & 0.2~TeV & \multicolumn{3}{c}{not applicable}\\
\hline 
\end{tabular}}
\smallskip
 The standoff distance (first number) is calculated at periastron and apastron using Eq.~(\ref{standoff}) and the stellar wind parameters in Sect.~6. Both a polar and an equatorial wind are considered for the Be stars. The break frequencies in the synchrotron and Compton spectra are then calculated using Eqs.~(\ref{syncs}) and~(\ref{comps}) in Sect.~\ref{spectral}. The pulsar wind parameters are the same for all the objects: $\dot{E}=10^{36}$~erg~s$^{-1}$, $\sigma=0.01$, and $\gamma_{\rm p}=10^5$. The star temperatures are such that inverse Compton interactions are in the Klein-Nishina regime.  
\end{table}