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Common envelope evolution (CEE) physics plays a fundamental role in theformation of binary systems, such as mergering stellar gravitational wavesources, pulsar binaries and type Ia supernovae. A precisely constrained CEEhas become more important in the age of large surveys and gravitational wavedetectors. We use an adiabatic mass loss model to explore how the total energyof the donor changes as a function of the remnant mass. This provides a moreself-consistent way to calculate the binding energy of the donor. Forcomparison, we also calculate the binding energy through integrating the totalenergy from the core to the surface. The outcome of CEE is constrained by totalenergy conservation at the point at which both component's radii shrink backwithin their Roche lobes. We apply our results to 142 hot subdwarf binaries.For shorter orbital period sdBs, the binding energy is highly consistent. Forlonger orbital period sdBs in our samples, the binding energy can differ by upto a factor of 2. The CE efficiency parameter $\beta_\mathrm{CE}$ becomessmaller than $\alpha_\mathrm{CE}$ for the final orbital period $\log_{10}P_{\mathrm{orb}}/\mathrm{d} > -0.5$. We also find the mass ratios $\log_{10} q$and CE efficiency parameters $\log_{10} \alpha_{\mathrm{CE}}$ and $\log_{10}\beta_{\mathrm{CE}}$ linearly correlate in sdBs, similarly to De Marco et al.(2010) for post-AGB binaries.

The Common Envelope Evolution Outcome -- A Case Study on Hot Subdwarf B Stars