The Orion Complex: A Case Study of Interstellar Matter
This work deals with some of the most typical complexes of interstellar matter and is intended to serve both as a reference book for the specialist and as an introduction for the newcomer to the field. It is hoped to meet the first aim by presenting a holistic view of the well studied complexes in Orion, built on information derived from various branches of modern Astrophysics. The wealth of published data is presented in the form of photographs, contour maps, diagrams and numerous heavily annotated tables. The second aim is pursued by providing an outline of the complexes, the physical problems associated with them, the empirical models describing their be haviour and, in addition, by including an extended Appendix section summarizing the numerous methods employed to derive the physical parameters of an H II region and the dust and molecular cloud physically associated with it. The book consists of five chapters and four Appendix sections. Chapter 1, which is concerned with the large scale view of the Orion region, outlines the morphology of the area and examines in particular the nature of Barnard's Loop and the associated filamentary structure in addition to the origin of the I Orion OB association. Chapter 2 focuses on the ionized gas of the Orion H II/molecular complex i. e.
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Large Scale View of the Orion Region
The H ii Regions M42 and M43
The Orion Complex M42OMC1 M43OMC2
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absorption abundance according angular resolution associated Beam brightness centre Chaisson Churchwell cluster complex component concerning contained contour map core density derived detected diameter distance distribution dust electron emission emitted energy envelope estimated excitation expressed extended frequency front given grains H n region hydrogen included indicating infrared intensity ionized ionized gas KL Nebula light lines luminosity lying maser mass measurements method Mezger molecular cloud molecules Munch narrow neutral Note object observed occurs optical originating Orion Nebula peak photograph physical parameters polarization position presented presented in Table probably profiles radial velocity radiation radio continuum range ratio recombination lines relation Remarks References Remarks to Table respectively ridge shell shown in Figure shows similar spectrum stars stellar stellar winds structure taken temperature tion Trapezium various velocity features wavelength width Wilson Zuckerman