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ZEEB ROAD, ANN ARBOR, Ml 48106 18 BEDFORD ROW, LONDON WC 1 R 4EJ, ENGLAND 8022334 R i n s l a n d , C u r t i s P h il ip SPECTRA OF LATE-TYPE STARS IN THE ONE TO FOUR MICRON REGION The Ohio State University Ph.D. 1980 University Microfilms International 300 N. Zeeb Road, Ann Arbor, MI 48106 18 Bedford Row, London WC1R 4EJ, England PLEASE NOTE: In all cases this material has been filmed in the best possible way from the available copy. Problems encountered with this document have been identified here with a check mark I, Glossy photographs 2c Colored illustrations 3, Photographs with dark background '4, Illustrations are poor copy ___ 5, Drin t shows through as there is text on both sides of page 6, Indistinct,, broken or small print on several pages ,^ throughout 7, Tightly bound copy with print lost in spii 8, Computer printout pages with indistinct print 9. Page(s) _ _ _ _ _ _ lacking when material received,, and not available from school or author _ _ _ _ _ _ 10. Page(s) _ _ _ _ _ _ seem to be missing in numbering only as text follows _ _ _ _ _ _ 11. Poor carbon copy _______ 12. Not original copy, several pages with blurred type ________ 13. Appendix pages are poor copy 14. Original copy with light type 15. Curling and wrinkled pages 16. Other University MicroTiims international 30C \ 13 = 3 30 4=1 SQ 4 VI! 43'06 '313! 761-4700 SPECTRA OF LATE-TYPE STARS IN THE ONE TO FOUR MICRON REGION DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Curtis Philip Rinsland, B.S., M.S. ***** The Ohio State University 1980 Reading Committee: Approved By Professor Stanley J. Czyzak Professor Geoffrey Keller Professor Robert F. Wing Department of Astronomy ACKNOWLEDGMENTS My deepest gratitude goes to my adviser, Professor Robert F. Wing, for his encouragement and guidance during the course of this research project. His knowledge, insight, enthusiasm, and patience were indispensable in every phase of this work. If I am ever put in the role of advising graduate students, I only hope I can perform a small fraction as well as he has. His influence x^ill be appreciated long after this manuscript has gathered dust. I am particularly grateful to Professor K. Narahari Rao for his assistance and encouragement during my many years as a graduate student. The many beneficial ideas contributed throughout the pursuit of this work are greatly appreciated. His continued financial support has helped to sustain me during these lean times. I am indebted to Dr. Sergio Ghersetti for making available the facilities of the Institute of Organic Chemistry in Venice, Italy. The hospitality extended to the author during his two visits to Venice is greatly appreciated. Special thanks to Dr. Agostino Baldacci who introduced me to the mysteries of acetylene. It has been a pleasure to work with him both at The Ohio State University Infrared Molecular Spectroscopy Laboratory and in Venice, Italy. Without his advice and assistance, the analysis of acetylene reported in this work would not have been possible. I would like to thank Drs. John H. Shaw and Robert J. Nordstrom of the Ohio State University for guidance to the literature of the atmospheric sciences. I would also like to express my sincerest gratitude to the following people, places, and things for their contributions to this experiment and/or my life: Drs. S. Ridgway, D. Hall, and P. Connes (for FTS data), Dr. C. Sneden (for MOOG), Kitt Peak National Observato­ ry (for the observing time), AUDREY (the rather cold and sometimes temperamental InSb detector of KPNO), Dr. R. Joyce (AUDREY'S father), Dr. S. Giorgianni (whose wine cellar is one of the great landmarks of Italy), Dr. Z. Gastone (useful discussions), and Y. Gardner and R. Bowman (great friends and neighbors). Finally, I would like to thank my parents who have always encour­ aged me to do my best, offered understanding and support in all my decisions, and, above all, given me their love. VITA December 5, 1950 . Born - Allentown, Pennsylvania 1972 ................. B.S. in Physics, The Pennsylvania State University, University Park, Pennsylvania 1972-1975............. Research Associate, The Ohio State University Radio Astronomy Observatory, Department of Electrical Engineering, The Ohio State University, Columbus, Ohio 1975 ................. M.Sc. in Astronomy, The Ohio State University, Columbus, Ohio 1975-1978............. Teaching Associate, Department of Astron­ omy, The Ohio State University, Columbus, Ohio 1978-197 9 ............. Teaching Associate, College of Mathemati­ cal and Physical Sciences, The Ohio State University, Columbus, Ohio 1979-198 0............. Research Associate, The Ohio State University Infrared Molecular Spectroscopy Laboratory, Department of Physics, The Ohio State University, Columbus, Ohio PUBLICATIONS "Ohio Survey VII", with R.S. Dixon, M.R. Gearhart, and J.D. Kraus, Astronomical Journal, 79, 1129 (1974). "The Ohio Radio Sky Survey: Supplement 2", M.Sc. thesis, The Ohio State University, Columbus, Ohio (1975). "Ohio Survey Supplement 2", with R.S. Dixon and J.D. Kraus, Astronomical Journal, 80, 759 (1975). "Observations of First-Overtone Silicon Monoxide Bands in Cool Stars", with R.F. Wing and R.R. Joyce, in Symposium on Recent Results in Infrared Astrophysics, ed. P. Dyal, NASA TM-X-73, 190, 23 (1977). iv "Observations of First-Overtone Silicon Monoxide Bands in Cool Stars", with R.F. Wing and R.R. Joyce, in Symposium on Recent Results in Infrared Astrophysics, ed. P. Dyal, NASA TM-X-73, 190, 26 (1977). "Scans of the 4-p SiO Bands in Late-Type Stars", with R.F. Wing, Bulletin American Astronomical Society, 10, 408 (1978). "Atmospheric Extinction and Photometric Reductions near Four Microns", Bulletin American Astronomical Society, 10, 408 (1978) "A Comprehensive Analysis of the Errors Affecting the Measurement of Intensities in Infrared Spectra", with D.W. Chen, K. Narahari Rao, W.C. Braun, and B. Fridovich, Thirty-third Symposium on Molecular Spectroscopy, Columbus, Ohio (1978). "Strengths of 13C 150.? and 12C 1E,0?_ Lines at 4.3-4,5 pm", with W.C. Braun, B. Fridovich, G.R. Smith, E.E. Champion, D.W. Chen, and K. Narahari Rao, Thirty-third Symposium on Molecular Spectroscopy, Columbus, Ohio (1978). "Aspects of Line Strengths and Half Widths for some the the V2 band lines of 12C 150 2 ", with V.M. Devi, P. Das, IC. Narahari Rao, and B. Fridovich, Thirty-fourth Symposium on Molecular Spectroscopy, Columbus, Ohio (1979). "Acetylene Spectra Observed in N-type Stars: A Laboratory Study", with K. Narahari Rao, A. Baldacci, and S. Giorgianni, Thirty-fourth Sympo- ium on Molecular Spectroscopy, Columbus, Ohio (1979). "Measurements of Atmospheric Extinction near 4 pm", with R.F. W.ng, Thirty-fourth Symposium on Molecular Spectroscopy, Columbus, Ohio (1979). "Atmospheric Extinction in the 4 pm Region", with R.F. Wing, Astronomical Journal, 84, 1235 (1979). "Strengths of 13C 1502 Lines at 4.3 pm", with A. Baldacci and K. Narahari Rao, Journal of Molecular Spectroscopy, in press. v TABLE OF CONTENTS Page ACKNOWLEDGMENTS ................................................... ii VITA ............................................................. iv LIST OF T A B L E S ..................................................... viii LIST OF F I G U R E S .......... xiv Chapter I. INTRODUCTION ............................................... 1 1. General Comments ....................................... 1 2. Overview of the Program. ........................ 9 II. SCANNER OBSERVING PROGRAM............. ..................... 14 1. Introduction........... 14 2. Instrumentation and Observing Procedure............... 17 3. Selection of Stars ..................................... 19 4. Data Reduction . ..................................... 28 III. MEASUREMENTS OF ATMOSPHERIC EXTINCTION IN THE 4 ym REGION ............ 34 IV. OBSERVATIONS OF THE FIRST-OVERTONE SiO BANDS NEAR 4 ym . 41 1. Introduction............... 41 2. Description of the Spectral Region .................... 43 3. Observations and Reduction Procedure . ........... 49 4. Derived Quantities................................ .. 52 5.