In four pages this paper discusses nebular emission in an informational overview. Three sources are cited in the bibliography.
Name of Research Paper File: JR7_RAnebula.rtf
Unformatted Sample Text from the Research Paper:
the creation of space, and the evolution of space. One author notes that, "Within the last decade or so new atomic data has become available for most atomic systems of
interest in astrophysics. Recent progress in atomic processes relevant to spectral formation" generally assumes some involvement with nebular emission lines (Pradhan; Peng, 1995). Bearing that in mind the following paper
briefly examines some of the important issues relating to nebular emission in todays study of space. Nebular Emission In an article which discusses the first stars Schneider (2002) states
that, "Recent modeling of the evolution and nucleosynthesis of very massive metal-free stars has enabled to predict their spectrum, emission lines due to recombinations in the nebular gas surrounding the
stars as well as specific nucleosynthetic signatures." What this tells us is that research concerning the development, the nature, and the evolution of stars involves a great deal of research
involving the emissions of stars themselves. By measuring and evaluating nebular emission line one can better understand the inherent structure and nature of nebula. But, it should also be understood
that this particular topic is incredibly intricate and diverse, illustrating that when speaking of nebular emission one is often speaking of something else to which nebular emission is associated.
In further examination of this conditions we note that in a "simulation of the collision of a fast wind with a slowly expanding shell...developing Rayleigh-Taylor instabilities are traced by density
contours...The concentration into high density knots is even more pronounced when time-dependent cooling is included in the calculations" (Vacca et al., 2003). Any localized density enhancements "would be observed as
knots. The formation of high density knots is even more pronounced if the time dependence of the cooling is taken into account, as this leads to further compression and enhancement"