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In all cases we have filmed the best available copy. University Microfilms international 300 N. ZEEB RD.. ANN ARBOR. Ml 48106 8129048 K u z m a , T h o m a s Jo h n O N SOME ASPECTS OF THE RADIATIVE INTERACTION IN A CLOSE BINARY SYSTEM The O hio S tale University PH.D. 1981 University Microfilms International 300 N. Zeeb Road, Ann Arbor, MI 48106 ON SOME ASPECTS OF THE RADIATIVE INTERACTION IN A CLOSE BINARY SYSTEM DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy In the Graduate School of The Ohio State University By Thomas John Kuzma, B.S. ***** The Ohio State University 1981 Approved By Reading Committee: Geoffrey Keller William M. Protheroe George W. Collins II Department of Astronomy It gives me great pleasure to dedicate this dissertation to Michael Cole and Alonda Crowell for putting up with me while I wrote it, Steven McGuire, Laura Greene, and Patricia Bobal for many years of friendship and support, Snezna Roglej for pushing me into this in the first place, and my parents for giving me my first telescope when I was ten. ii ACKNOWLEDGMENTS First and foremost I would like to express my gratitude to m y adviser, Dr. George W. Collins II, for introducing me to the wonderful world of stellar atmospheres and proving to me that theory can be fun. I would also like to thank Dr. George Sonneborn and Mr. Kenneth Carpenter for setting up the computer storage space necessary to do this problem and for many long helpful discussions concerning metallic line blanketing. Thanks are also due Drs. William M. Protheroe and Paul F. Buerger for providing their model of V Puppis, Mr. Kenneth Rumstay for doing some of the figures for this dissertation, and Ms. Frances Crowell for dilligently typing my illegible manuscript. Finally I would like to thank The Ohio State University for supplying the computer time necessary to complete this project. iii VITA November 17, 1949 .......... Born - Elizabeth, New Jersey 1970-1972 .................. Teaching Assistant, Department of Astronomy, Villanova University, Villanova, Pennsylvania 1972 ...................... B.S., Villanova University, Villanova, Pennsylvania 1973-1974 .................. Graduate Teaching Associate, Department of Astronomy, The Ohio State University, Columbus, Ohio 1974-197 5 .................. Graduate Teaching Associate, Department of Mathematics, The Ohio State University, Columbus, Ohio 1975-1977 .................. Graduate Teaching Associate, Department of Physics, The Ohio State University, Columbus, Ohio 1977-1979 .................. Graduate Teaching Associate, Department of Astronomy, The Ohio State University, Columbus, Ohio 1979-1981 .................. Graduate Teaching Associate, Department of Physics, The Ohio State University, Columbus, Ohio PUBLICATIONS "On Some Aspects of Balmer-Line Formation in Rotating White Dwarfs." Ap. J., 227, 548, 1979. "Effects of Stellar Rotation on Spectral Classification." (with A. Slettebak) I.A.U. Colloq. 47: Spectral Classification of the Future, ed. M.F. McCarthy, A.G.D. Philip, and G.V. Coyne, (Vatican Observatory), p. 87, 1979. iv VITA (continued) "The Effects of Enhanced Helium Abundance on the Visible Spectra of Luminoius F and G Stars." (with G. Sonneborn and G. W. Collins II), Ap. J., 232, 807, 1979. "Effects of Stellar Rotation on Spectral Classification." (with A. Slettebak and G.W. Collins II), Ap. J., 242, 171, 1980. FIELDS OF STUDY Major Field: Theoretical Astrophysics Studies in Stellar Atmospheres and Radiative Transfer. Professor George W. Collins II Studies in Stellar Rotation. Professors Arne Slettebak and George W. Collins II v TABLE OF CONTENTS Page DEDICATION.................................................... ii ACKNOWLDEGMENTS .............................................. ill V IT A .......................................................... iv LIST OF TABLES ................................................ vii LIST OF FIGURES .............................................. viii Chapter I . INTRODUCTION .......................................... I II. GEOMETRICAL CONSIDERATIONS ............................ 12 III. TRANSPORT OF POLARIZED RADIATION ....................... 35 IV. MODEL CALCULATIONS .................................... 48 V. RESULTS AND D I S C U S S I O N ................................ 63 LIST OF REFERENCES............................................ 136 vi LIST OF TABLES Table Page 1. Plane Parallel and Uniform Illumination Incident Terms for the Moment Equations........................ AO 2. Model Parameters for V P u p ............................. 55 3. Effective Temperatures and Gravities for the Grid of Atmospheres on the Illuminating S t a r .................. 57 A. Effective Temperatures and Gravities for the Grid of Atmospheres on the Illuminated S t a r .................. 59 5. Temperatures and Horizontal Fluxes for the Inner Hemisphere of the Illuminated S t a r .................... 6A 6. Theoretical Spectral Types ............................ 129 vii LIST OF FIGURES Figure Page 1. Star centered reference frames for the binary system.................................................... 2. Cross section in the orbital plane of several equipotentials for the Roche model with a mass ratio of % ............... 17 3. The rotated coordinate frame.............................. 23 4. Star centered, and observed coordinates on the illuminating star......................................... 26 5. The projection of £ onto the observed plane of the sky 27 6. Relation between the observed coordinates p,f5 and the incident angles 6,4>....................................... 31 7. Coordinate system to define the emergent angles toward a distant observer........................................ 33 8. Local coordinate frame to define the incident flux........ 44 9. The binary system V Puppis................................ 56 10. Flux distributions for the four models at the sub-stellar point..................................................... 67 11. Flux distributions for the four models at point 2......... 68 12. Flux distributions for the two models at point 3.......... 69 13. The incident and intrinsic (non-illuminated) flux distributions at the sub-stellar point.................... 70 14. He I 4471 and Mg II 4481 residual intensities for the four models at the sub-stellar point...................... 72 15. He I 4471 and Mg II 4481 residual intensities for the four models at point 2.................... 73 viii 16. He I 4471 and Mg II 4481 residual intensities for the two models at point 3 ............................... 74 17. Temperature structure as a function of for the four models at the sub-stellar point...................... 75 18. Temperature structure as a function of xD for the _ , , „ Ross -,r four models at point 2 .................................... /o 19. Temperature structure as a function of t^oss for the two models at point 3..................................... 77 20. Temperature structure as a function of T^Qg for the four models at point 2, indicating the Rossland depth at which the optical depth in the line cores reaches unity for Mg II 4481 (MG), and the permitted (HE) and forbidden component (HE) of He I 4471..................... 79 21. The number of electrons contributed per He atom as a function of t„ for three models at point 2. LB is plane parallel Illumination with line blanketing, NLB is plane parallel illumination without line blanketing, and EN is the enhanced flux model......................... 80 22. Spectral types for the models at the three points, using monochromatic magnitude differences. LB, NLB, and EN are

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