Examples of protoplanetary

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Delivery rates are more efficient to protoplanetary discs, as the solid grains effectively sputter the incoming material in hypervelocity collisions.
The reason for this revisitation lies in the fact that complex organic matter resembling a petroleum fraction may exist in certain protoplanetary nebulae.
Derived core masses and observed short lifetimes of protoplanetary disks strongly constrain conditions for forming gas giant planets.
A disc of scattered protoplanetary and planetesimal material is building up in external orbits.
The structure and chemistry of protoplanetary disks depend strongly on the nature of the central star around which they have formed.
The resulting spectrum is able to match the emission spectrum of a protoplanetary nebula.
A gravitationally unstable protoplanetary disk forms giant gaseous protoplanets within about 1000 years, while dust grains coagulate and sediment to their centers, forming solid cores.
These include the 21 and 30 mm emission features, and the extended red emission observed in protoplanetary nebulae and planetary nebulae.
The grains from which meteorites initially aggregated were interstellar silicates, processed through a molecular cloud prior to accretion in the protoplanetary disc.
In the following protoplanetary nebulae stage, emission features corresponding to stretching and bending modes of aliphatic compounds are detected.
The global modelling of dust and gas evolution in protoplanetary discs should follow.
In this introduction, we have started from the observation that petroleum fractions may exist in certain protoplanetary nebulae.
The protoplanet evolves under the gravitational interaction of the central star and the protoplanetary disc.
Thus, these petroleum fractions can be used as model for the matter present in the interstellar medium or in the protoplanetary nebulae.
Dusty plasmas, perhaps the fastest growing area in plasma physics, might also be of extreme importance for the theory of protoplanetary discs.
In other words, it appears that the organic and carbonaceous matter present in the protoplanetary nebulae should be closer in composition to that found in carbonaceous chondrites.
The main aim of our work was to investigate the evolution of the planet's orbit due to the torque exerted on it by the truncated protoplanetary disc.
We have also addressed our discussion to the possible formation of petroleum fractions or petroleum-like organic matter, which could exist both in the interstellar medium and in the protoplanetary nebulae.

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