We have shown that for reasonable assumptions regarding the proto-planetary nebula, magnetic reconnection in a dusty plasma can result in localized heating of dust particles.
The reason for this revisitation lies in the fact that complex organic matter resembling a petroleum fraction may exist in certain protoplanetary nebulae.
These objects probably retained the prebiotic material present in the pre-solar nebula and deposited it on our planet.
More realistically, the nebula would be evolving under the influence of internal viscous forces and the tidal forces of embedded giant planets.
Among several sources, gas-grain reactions operating in the solar nebula have been well recognized to play an important role in nebular chemistry.
In any event, the physical aspects of the moon, the planets, the nebulae will be able to be studied and charted under favourable conditions.
The resulting spectrum is able to match the emission spectrum of a protoplanetary nebula.
These include the 21 and 30 mm emission features, and the extended red emission observed in protoplanetary nebulae and planetary nebulae.
