We use fluctuating magnetic helicity to investigate the polarisation properties of Alfvenic fluctuations at ion-kinetic scales in the solar wind as a function of $beta_p$, the ratio of proton thermal pressure to magnetic pressure, and $theta_{vB}$, the angle between the proton flow and local mean magnetic field, $mathbf{B}_0$. Using almost 15 years of textit{Wind} observations, we separate the contributions to helicity from fluctuations with wave-vectors, $textbf{k}$, quasi-parallel and oblique to $mathbf{B}_0$, finding that the helicity of Alfvenic fluctuations is consistent with predictions from linear Vlasov theory. This result suggests that the non-linear turbulent fluctuations at these scales share at least some polarisation properties with Alfven waves. We also investigate the dependence of proton temperature in the $beta_p$-$theta_{vB}$ plane to probe for possible signatures of turbulent dissipation, finding that it correlates with $theta_{vB}$. The proton temperature parallel to $mathbf{B}_0$ is higher in the parameter space where we measure the helicity of right-handed Alfvenic fluctuations, and the temperature perpendicular to $mathbf{B}_0$ is higher where we measure left-handed fluctuations. This finding is inconsistent with the general assumption that by sampling different $theta_{vB}$ in the solar wind we can analyse the dependence of the turbulence distribution on $theta_{kB}$, the angle between $textbf{k}$ and $mathbf{B}_0$. After ruling out both instrumental and expansion effects, we conclude that our results provide new evidence for the importance of local kinetic processes that depend on $theta_{vB}$ in determining proton temperature in the solar wind.
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