Stern-Gerlach-Type Separations of Structural and Chiral Isomers by Interstellar Magnets

White dwarfs, with masses just above the Chandrasekhar limit (1.4 solar masses), can violently collapse into small (104 km radius) and very dense (rho = 10(17) kg/m(3)) magnetars that can produce B-fields up to 10(12) Tesla (T) with gradients potentially exceeding one-thousandth of the total field. Such strong gradiated fields pull on paramagnetic molecules with a force proportional to the magnetic moment of the radical (mu(r)) dotted into (dB/dz)(z) over cap, which falls off by the distance cubed. The magnetic force is sufficiently strong to accelerate radicals to velocities of many thousands of meters per second. Radical magnetic moments are strongly dependent on conjugation (dispersion of spin density). As a result, radical isomers, with different mu(r) values, are separated when in the vicinity of a magnetar. The effect is fundamentally due to the radical's g-value, which, in turn, is embedded in its magnetic moment. Fundamental mathematical protocols were developed to quantify the degrees of large-B-field-enforced isomeric (including chiral isomers) separations. D and L enantiomers have different g-values because of spin orbit coupling effects mediated by the weak force. The alanine enantiomeric radicals falling into or escaping from a nearby magnetar become physically separated in space by many kilometers and may end up in spatially separated molecular clouds. The chiral excess in the Murchison meteorite, and perhaps on Earth, might be a result of this scenario.