Collisions between asteroids containing such solutions during aqueous alteration can disperse microorganisms in solar nebulae and transport them to planets and to other solar systems.
These include the 21 and 30 mm emission features, and the extended red emission observed in protoplanetary nebulae and planetary nebulae.
Star-forming regions within the nebulae encountered may thus be seeded by significant numbers of microorganisms.
Much of the interstellar gas as well as gaseous nebulae are plasmas.
Thus, these petroleum fractions can be used as model for the matter present in the interstellar medium or in the protoplanetary nebulae.
In this introduction, we have started from the observation that petroleum fractions may exist in certain protoplanetary nebulae.
Sections six to eleven lead us on a hop around some constellations, to illustrate a handful of stars and nebulae.
Nucleosynthesis in stars determines the elemental and isotopic composition of protostellar nebulae, which probably develop with systematic relationships between nominally reducing and oxidizing components and between stable and radioactive nuclides.
