Carbonaceous Grain Formation Report

Review of Carbonaceous Grain Formation

Introduction: Carbon is produced in red giant stars and supernovae because of triple alpha reactions that occur when 3 alpha particles(He-4) fuse together. The rate that this happens is dependent on the temperature and density. When the distance between particles increases the rate of reaction decreases [1]. After a star cools the carbon begins to collect in the photosphere condensing and forming microstructures with graphene cores. The droplets conglomerate into larger dust particles before eventually being ejected from the photosphere.

In this paper I will review the research focusing on carbon dust formation. This is believed to occur primarily in red giant stars and in addition particle condensation happens in supernovae, detonation waves and in the lab using carbon-vapor condensation methods. Understanding carbon condensation and modelling the

Aromatic, alkenes, alkanes and alkynes growth can be simulated using density, number of atoms, and geometries to show reaction rates deduced from combustion chemistry. The condensation and growth has been simulated at various different temperatures and corroborated with laboratory experiments. The energy of carbonaceous clusters is proportional to the distribution throughout the stellar atmosphere [9]. Carbon condensates forming from free carbon atoms ejected from supernovae have been studied in detail. In the supernova gas, Carbon atoms are colliding and releasing energy with high frequency. Complex exothermic reactions result in a large variety of carbon isotopes where some of the carbon will react with oxygen to create carbon monoxide and a lower number isotope of carbon. Over time the carbon dust grains cluster together and form carbon grains. Particles observed in meteorites tend to be large ranging from 0.8 to 20 micrometers