Chemical Composition of High-Excitation Planetaries

Details Chemical Composition of High-Excitation Planetaries Chemical Composition of High-Excitation Planetaries

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981pnas...78.5266a&link_type=abstract

Proceedings of the National Academy of Sciences of the United States of America, Volume 78, Issue 9, pp. 5266-5270

Physics

11

Scientific paper

Nebular spectral line intensities measured mostly in the optical region, but also in the IR and satellite UV (where possible), are used to derive plasma diagnostics and ionic concentrations n (Xi)/n(H+). Then, we use theoretical nebular models to represent as closely as possible certain excitation-sensitive line ratios of HeII/HeI, [OIII]/[OII], and [NeIII]/[NeV]. Also, we try to reproduce the line intensities themselves. These models are used as devices to allow for unobserved ionization stages. Although He, C, and N show significant variations among different nebulae, heavier elements such as O, and probably Ne, S, Cl, and Ar are more nearly constant, suggesting that progenitor stars underwent nuclear transformations in their interiors that affected C and N but not heavier elements.

Affiliated with

Also associated with

No associations

Rating

Chemical Composition of High-Excitation Planetaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Chemical Composition of High-Excitation Planetaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Chemical Composition of High-Excitation Planetaries will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1516393