  The mode-sum method provides a practical means for calculating the self force
acting on a small particle orbiting a larger black hole. In this method, one
first computes the spherical-harmonic $l$-mode contributions $F^{\mu}_l$ of the
"full force" field $F^{\mu}$, evaluated at the particle's location, and then
sums over $l$ subject to a certain regularization procedure. In the
frequency-domain variant of this scheme the quantities $F^{\mu}_l$ are obtained
by fully decomposing the particle's self field into Fourier-harmonic modes $l m
\omega$, calculating the contribution of each such mode to $F^{\mu}_l$, and
then summing over $\omega$ and $m$ for given $l$. This procedure has the
advantage that one only encounters {\it ordinary} differential equations.
However, for eccentric orbits, the sum over $\omega$ is found to converge badly
at the particle's location. This problem (reminiscent of the familiar Gibbs
phenomenon) results from the discontinuity of the time-domain $F^{\mu}_l$ field
at the particle's worldline. Here we propose a simple and practical method to
resolve this problem. The method utilizes the {\it homogeneous} modes $l m
\omega$ of the self field to construct $F^{\mu}_l$ (rather than the
inhomogeneous modes, as in the standard method), which guarantees an
exponentially-fast convergence to the correct value of $F^{\mu}_l$, even at the
particle's location. We illustrate the application of the method with the
example of the monopole scalar-field perturbation from a scalar charge in an
eccentric orbit around a Schwarzschild black hole. Our method, however, should
be applicable to a wider range of problems, including the calculation of the
gravitational self-force using either Teukolsky's formalism, or a direct
integration of the metric perturbation equations.
