  Jovian electrons serve as an important test-particle distribution in the
inner heliosphere and have been used extensively in the past to study the
(diffusive) transport of cosmic rays in the inner heliosphere. With new limits
on the Jovian source function (i.e. the particle intensity just outside the
Jovian magnetosphere), and a new set of in-situ observations at 1 AU for both
cases of good and poor magnetic connection between the source and observer, we
revisit some of these earlier simulations. We aim to find the optimal numerical
set-up that can be used to simulate the propagation of 6 MeV Jovian electrons
in the inner heliosphere. Using such a set-up, we further aim to study the
residence (propagation) times of these particles for different levels of
magnetic connection between Jupiter and an observer at Earth (1 AU). Using an
advanced Jovian electron propagation model based on the stochastic differential
equation (SDE) approach, we calculate the Jovian electron intensity for
different model parameters. A comparison with observations leads to an optimal
numerical set-up, which is then used to calculate the so-called residence
(propagation) times of these particles. Comparing to in-situ observations, we
are able to derive transport parameters that are appropriate to study the
propagation of 6 MeV Jovian electrons in the inner heliosphere. Moreover, using
these values, we show that the method of calculating the residence time applied
in former literature is not suited to being interpreted as the propagation time
of physical particles. This is due to an incorrect weighting of the probability
distribution. We propose and apply a new method, where the results from each
pseudo-particle are weighted by its resulting phase-space density (i.e. the
number of physical particles that it represents). Thereby we obtain more
reliable estimates for the propagation time.
