Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp13b..01c&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SP13B-01
Astronomy and Astrophysics
Astrophysics
7509 Corona, 7549 Ultraviolet Emissions
Scientific paper
In this work, physical characteristics of the solar corona in the Extreme Ultra-Violet (EUV) regime of the electromagnetic spectrum are investigated. Regions of heightened coronal activity are generally found near the locations of sunspots. These regions are commonly called Active Regions and are the focus of the project. Multiple space based observing platforms have been deployed in the last decade and it is possible to use several of these observatories in combination to develop a more complete picture of the solar corona. Joint Observing Program 146 was created to collect spectroscopic intensities using the Coronal Diagnostic Spectrometer (CDS) on Solar and Heliospheric Observatory (SoHO) and EUV images using NASA's Transition Region and Coronal Explorer (TRACE). The emission line intensities are used to develop an understanding of the temperature and density of the active region coronal plasma. However, the performance of the CDS instrument in the spatial and temporal domains is limited and to compensate for these limitations data collected by the TRACE instrument provide a high spatial and temporal resolution set of observations. The combination of the information contained in the data from these two instruments is used to determine the temperature, density and dynamics of the solar coronal active regions. One of the most exciting unsolved problems in solar astrophysics is to understand why the corona maintains a temperature roughly two orders of magnitude higher than the underlying material. An detailed investigation of the coronal emission has provided constraints on models of the heating mechanism, since the temperature, density and evolution of emission rates for multiple ionic species are indicative of the mechanism(s) working to heat the corona. The observed corona appears to consist of multiple unresolved structures as well as resolved active region structures, called coronal loops. The purpose of the present work is to determine the characteristics of the unresolved background corona. This has two important applicatons. Any model of the corona must account for the emission comprising the unresolved background, and the study of coronal loops can be improved by subtracting the emission along the line-of-sight due to the background contribution to the total intensity. Using the characterizations of the coronal unresolved background, results for loops after background subtraction are also presented. This work demostrates the magnitude of the unresolved coronal emission with respect to the total emission along the line of sight, and how this compares to that of the resolved loops. It is apparent from this analyis that the unresolved corona is the dominant source of radiation in the active region corona.
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