Computer Science – Learning
Scientific paper
Feb 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997taea....1.1008g&link_type=abstract
NASA University Research Centers Technical Advances in Education, Aeronautics, Space, Autonomy, Earth and Environment, vol. 1, p
Computer Science
Learning
Planetary Nebulae, Research, Ions, Interstellar Matter, Image Processing, Electron Density (Concentration), Workstations, Telescopes, Enrichment, Cosmic Rays, Correction, Charge Coupled Devices, Calibrating, A Stars
Scientific paper
An examination is made of the planetary nebula M57. also known as the Ring Nebula. The presentation will begin with an overview of planetary nebulae including their role in the evolution of the Interstellar Medium (ISM). Since planetary nebulae are formed during the final stages in the life of a star, these are important objects to study. They are good laboratories for learning about how stars interact with the ISM, including how a star will enrich the surrounding medium with elements heavier than H and He. There will also be a brief discussion of the various atomic processes which are important to the nebula. The planetary nebula M57 will be discussed next. This well known object has been the subject of many studies. What is significant about this work is that we have derived temperature and density maps of the nebula using the ions O(sup ++), N(sup +) and S(sup +). For the first time, point-by-point variations in the electron temperature (Te) from both the O(sup ++) ion and the N+ion can be compared. Cospatial maps of electron density (Ne) derived from S+are also presented. These quantities are important in order to calculate the chemical abundances of this object and to better understand how the ISM will evolve over time. These maps were generated using CCD images taken at the 2.12 meter telescope at San Pedro Matir in Baja, Mexico. The images were calibrated on a SPARC 20 workstation using the well known image processing software, IRAF. The standard reduction steps were followed, including bias and dark subtraction, flat field corrections and cosmic ray removal. These steps will be discussed briefly.
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