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INVESTIGATIONS OF LONG-PERIOD DQ HERCULIS STARS. Item Type text; Dissertation-Reproduction (electronic) Authors PENNING, WILLIAM ROY. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 23/09/2021 13:28:45 Link to Item http://hdl.handle.net/10150/188161 INFORMATION TO USERS This reproduction was made from a copy of a manuscript sent to us for publication and microfilming. While the most advanced technology has been used to pho tograph and reproduce this manuscript. the quality of the reproduction is heavily dependent upon the quality of the material submitted. Pages in any manuscript may have indistinct print. In all cases the best available copy has been filmed. 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Other_______________________________________ _ University Microfilms International INVESTIGATIONS OF LONG-PERIOD DQ HERCULIS STARS by William Roy Penning A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY in the Graduate College THE UNIVERSITY OF ARIZONA 1 986 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Final Examination Committee, we certify that we have read the dissertation prepared by ___W~i~l~l~i~a~rn~~R~O~y~P~e~n~n~i~n~gL- _________________ enti tIed __...:I::.:n .... v..=->=e""'s'-'t::..::i:::.;g~a=t=i~o~n~s~o=f-=L!!:O::.:ln.!..:g::l---=-P~e:.:::r:..::i;.::o~d~=:D.:.:O:..-;H~e""r;..c=u~l..=i~s::-!S~t.=.:=a-=r..:::s~ _____ and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of __~D~o~c~t~o~r=-~o~f~P~h~i~l~o~s~o~p~h~y _______________________ ___ Date Date I tI Date J).-h!!~ ::--~------'(i...--.f-"------------ Dat.e ))",/1 1 IlS- Date i Final approval and acceptance of this dissertation is contingent upon the candidate's submission of the final copy of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommend that it be accepted as fulfilling the dissertation requirement. Date STATEMENT BY AUTHOR This dissertation has been ~ubmitted in partial fulfillment of requirements for an advanced degree at The University of Arizona and is deposited in the University· Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permission, provided that accurate acknowledgement of source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major depar.tment or the Dean of the Graduate College when in his or her judgmen t the proposed use is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. ACKNOWLEDGEMENTS I would first like to thank my graduate advisor, Dr. James Liebert, for his constant support of my work which eventually led to this dissertation. His Glrive and dedication to the field of Astronomy often served to encourage me when my own enthusiasm flagged. I am also indebted to Dr. Gary Schmidt f?r his work with the polarimetric part of this research, which provided a very important contribution in this particular subfield of astronomical science. I am also grateful to Alan Koski, Dave Skillman, and the rest of the Steward Computer group for their maintenance of the Eclipse, and later the MV 10000, compu terse without these machines the modeling aspect of this work would not have been possible. I also thank the mountain staffs of Steward Observatory at Kitt Peak and the Multiple Mirror Telescope Observatory for their work in maintaining those facilities and thus allowing for much fruitful data gathering. I am also thankful to Dr. Craig Foltz of MMTO, formerly of Steward Observatory, for implementing the Steward Interactive Reduction System, an IRS we can all live with, which made possible the rapid reduction of hundreds of iii iv spectra taken at both the MMT and the SOKP 2.3m facilities. Dr. H. S. "Pete" Stockman of Space Telescope Science Institure, also formerly of Steward, and graduate student Steve West, contributed much work toward bringing the Octopol polarimeter into operation, without which much of this research would have been impossible. Above all, I would like to thank God for getting me through nine straight years of college. TABLE OF CONTENTS Page LIST OF ILLUSTRATIONS • vii LIST OF TABLES xi ABSTRACT • xii CHAPTER I. BACKGROUND 1 A. Introduction • • • • • 1 Cataclysmic Variables • 1 Magne tic Binaries • • • • .• 6 B. History of Objects 12 AO Psc 12 V1223 Sgr • • • • • • 13 H2215-086 and 3A0729+103 ••••• 14 C. Motivation for Research • 15 II. SPECTROSCOPIC INVESTIGATIONS • 19 A. Introduction 19 B. Observations •••••• 21 C. The Orbital Modulation 30 D. Rotational Modulations 36 Coherent Periodicities 36 A Rotation-Illumination Model. 43 E. System Parameters • • • • • 48 F. Conclusions • • • • • • 51 III. POLARIMETRIC INVESTIGATIONS 55 A. Introduction 55 B. Observations 57 C. Discussion 65 Analysis 65 In terpreta tion 76 D. Conclusions • • • 82 v vi IV. MODELING AND CALCULATIONS 84 A. Introduction •••••• • • • • 84 B. The Rotation-Illumination Model 86 The X-Ray Distribution •• • • 86 Asymmetries in Emission Lines • • • 101 The Modeling Program • • • •• • • • • • 103 The Shape of the X-Ray Distribution • • • 107 The Cosine Distribution Model • • • • • • 112 Comparison with Observations • • • • 115 C. Emission of Polarized Radiation • • • • 131 Polarized Radiation from a Plasma Slab ••• 131 The Modeling Program • 147 Results. • • • • • • • • • • • • • 154 D. Conclusion ••••••• • 159 The Rotation-Illumination Model ••••• 159 Emission of Polarized Radiation ••••• 161 Overall Implications •• 162 V. SUMMARY 164 A. Observational Data . • 164 Spectroscopy • • • • • 164 Polarimetry • • • • 164 B. Interpreta~ion • • • • • 165 The Accretion Disk . • . 165 The Accretion Funnel • • 167 C. Conclusions • • • • 168 REFERENCES • • • • • • 171 LIST OF ILLUSTRATIONS Figure Page 1. Diagram illustrating effects of illuminating a flared disk with an X-ray source 11 2. Composite spectra of objects studied. a) V1223 Sgr, b) H22l5-086, c) 3A729+l03, d) AO Psc • • • • 23 3. Wavelength data for V1223 Sgr. Top to bottom: HS, Hy, He II A4686. Curves represent orbital fit ••••• • • • • • • • • 25 4. Wavelength data for H2215-086. Top to bottom: H S, Hy, He II A4686 • • • • • • • • • 26 5. Wavelength data for 3A0729+103. Top to bottom: HS, Hy, He II A4686. Curves represent orbital fit •••• ••• • • • 27 6. Wavelength data for AO Psc. Top to bottom: HS, Hy, He II A4686 • • • • • • • • • • 28 7. Equivalent width of absorption vs. orbital phase for 3A0729+103 ••••• • • • • 31 8. Diagram showing center-of-mass placement vs. offset location between H and He motion vectors • • • • • • . • . • • 35 9. Power spectrum for the wavelength data for V1223 Sgr. Top to bottom; HS, Hy, He II A4686 • • • • • • • • • • • • • • • • • 38 10. Power spectrum for the wavelength data for H2215-086. Top to bottom; HS, Hy, He II A4686 • • • • • • • • • • • • • • • • • 39 11. Power spectrum for the wavelength data for 3A0729+103. TOp to bottom; HS, Hy, He II A4686 • • • • • • • • • • • • • • • • • • 40 vii viii 12. Power spectrum for the wavelength data for AO Psc. Top to bottom: HS, Hy, He II ~4686 • ~ • • • • • • • • • • 41 13. Diagram illustrating effects of a rotating source of X-rays illuminating different parts of .an accretion disk •• • • • • • • • 4S 14. Circular polarization data for H221S-086, plotted vs. time ••••••• • • • • 63 IS. Circular polarization data for 3A0729+103, plotted vs.

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