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The a Lgol-Type Binary CX Draconis The Algol-type binary CX Draconis: numerical models of ultraviolet observations A thesis submitted for the Degree of Doctor of Philosophy of the University of London by David Wonnacott Department of Physics & Astronomy University College London University of London 1990 ProQuest Number: 10609784 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a com plete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest ProQuest 10609784 Published by ProQuest LLC(2017). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States C ode Microform Edition © ProQuest LLC. ProQuest LLC. 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106- 1346 To the two wonderful people who taught me that if you reach for the heavens, you can have the stars. To my parents. 2 .. .every strong intellect.. .is a guardian of integrity. Dr. Jacob Bronowski — The Ascent of Man 3 Acknowledgements It is my great pleasure to thank the following people, without whom this work would have been immeasurably lessened. I should like to offer my sincerest thanks to Ian Howarth for the supervision he has bestowed upon me in the years since I set out to produce this thesis. It wouldn’t have been the same without him. My grateful thanks also go to Raman Prinja, Ian’s more-than-able stand-in during my third year, and to Professor Sir Robert Wilson who had the foresight to place me under their guidance. Thanks too, go to Ian, Raman, Nicole, Julie, Dave P. and Keith for being such able proof-readers and spotters-of-mistakes, and to my friends and colleagues at U.C.L. and at R.A.L. for their time, sufferance and encouragement, notably Paul (atomic physics) and Mike (spectroscopy). I must not fail to mention the indomitable squaddies from ‘E3’ (lately of ‘A25’). Daily life with Keith, Des and ‘Barry’ was a permanent source of debate, education, fun and sticky buns. I could not have wished for more stimulating companions to pass my time with. I only hope that they remember me with the same fondness. Finally, there are three people for whom I cannot express the full extent of my gratitude in words: Julie, my fiancee, who had (and still has) the soundness of mind to make me work when I really didn’t want to and who was always there when I needed her to be, and my Mother and Father who have contributed to this thesis more than they could ever know and to whom I shall be more grateful than I can ever say. 4 A bstract International Ultraviolet Explorer satellite spectra of the Algol-type interacting binary system CXDra (B2.5 Ve + F?) have been analysed in detail, revealing a new phenomenon, to whit, CXDra possesses a matter stream which at certain orbital phases disappears from the line-of-sight almost entirely. This has been dubbed ‘stream dipping’. Two possible alternative interpretations of these observations have been exam­ ined. Either the stream is undergoing a rapid change in its ionization balance, or the stream is collapsing towards the orbital plane as it gains speed. More complex models involving, for example, variable stellar winds or distortion of the stream trajectory by magnetic forces can be excluded to varying degrees by the velocity structure seen in the resonance lines. Several scale-independent numerical models of interacting binary systems have been generated and applied to CX Dra in order to gain an insight into the geometry which is responsible for this effect. U Cep, with its well-known system parameters, has been used as a benchmark for the models. Those models with inviscid streams have failed to reproduce the observations, but the viscous streams, modelled using a cell-averaging technique, reproduce not only the observed velocity structure but the phase-dependency of the profiles too. Profile fitting then yields the chemical composition of the stream (these results indicate a high degree of CNO-processing), and allows a lower limit to be placed on the inclination of the orbital plane. The density structure of the models has also been used to predict the variations Attention is drawn to the inclusion of an addendum which contains the results of a detailed investigation into the properties and possible failings of the numerical model employed in this work, in particular to the non-conservation of angular mo­ mentum. The results derived from this model are, however, largely insensitive to this flaw. 5 C ontents 1 To Be or not to Be... 12 1.1 Introduction ...................................................................................................... 12 1.2 The present state of p la y ................................................................................ 14 1.2.1 The optical spectrum ..................................................................... 14 1.2.2 The infrared sp e c tru m ..................................................................... 15 1.2.3 The radio frequencies ..................................................................... 16 1.2.4 The ultraviolet spectrum .............................................................. 16 1.2.5 The X-ray s p e c tru m ........................................................................ 17 1.2.6 P olarim etry ......................................................................................... 18 1.2.7 Evolutionary status ........................................................................ 18 1.2.8 The Be Phenomenon as the product of binary star interaction 19 1.3 Summary and a im s .......................................................................................... 20 1.4 C X D raconis ....................................................................................................... 21 1.5 Thesis o u tlin e ................................................................................................... 22 2 IUE observations 24 2.1 Introduction ........................................................ 24 2.2 Reduction of the IUE d a t a ......................................................................... 25 2.3 The velocity-phase variations ...................................................................... 26 2.4 Extraction of the stream profiles ............................................................... 31 2.4.1 The choice of the standard ........................................................... 31 2.5 In terp retatio n ................................................................................................... 34 6 7 3 The Single Particle Model 39 3.1 Introduction .................................................................................................... 39 3.2 The Model ....................................................................................................... 40 3.3 Comparison with the d ata ............................................................................. 44 3.4 Discussion .......................................................................................................... 45 3.5 The conditions for an escaping stream ...................................................... 46 4 The viscous model 50 4.1 Introduction .................................................................................................... 50 4.1.1 Possible stream-supporting mechanisms ...................................... 50 4.1.2 Viscosity ............................................................................................ 53 4.2 The viscous m odel .......................................................................................... 54 4.2.1 Prendergast & Taam viscosity ........................................................ 54 4.2.2 Im plem entation................................................................................... 54 4.3 Tests of the M odel .......................................................................................... 58 4.4 Results................................................................................................................. 63 4.5 Scale-height predictions ............................................................................. 66 5 Ultraviolet line synthesis 69 5.1.....Introduction .................................................................................................... 69 5.2 Profile synthesis: A bsorption ...................................................................... 70 5.2.1 The ‘slab’ m odel ................................................................................ 70 5.2.2 Results ................................................................................................ 74 5.3 Profile synthesis: Scattering ......................................................................... 75 5.3.1 The scattering model ......................................................................... 75 5.3.2 Preliminary analysis ......................................................................... 78 5.3.3 Results ................................................................................................ 81 6 Polarization in Algols 91 6.1 Introduction .................................................................................................... 91 6.1.1 Possible sources of polarization ..................................................... 92 8 6.2 Polarization theory ......................................................................................
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