Starting with his first publication in 1974 as a graduate student, TChM has been working on the formulation of a theory of star formation, specifically accounting for the role of cosmic magnetic fields in the process. This is within the realm of nonideal, multifluid magnetohydrodynamics and involves the understanding of physical processes that lead from the mean density of the interstellar medium (about 1 cm-3) to the mean density of stars, such as the Sun (about 1024 cm-3). His calculations thus far have elucidated the physics of star formation up to densities of about 1015 cm-3. The most difficult part of the task is done. What is left is, by comparison to the already completed work, is straightforward but computationally intensive. Nevertheless, at all stages of the calculations in the past, the magnetic field never ceased to spring up surprises in the form of new, unexpected physical effects. No doubt, therefore, that many more surprises will be in store by the time the calculations produce a model protostar turning on its nuclear reactions—at which stage the long-term goal of this project will have been achieved. What has been encouraging in this long journey is that dozens of TChM's predictions have been confirmed by observations and, more importantly, no observation has contradicted a single one of his predictions. By contrast, several competing ideas have come and gone.