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Physics of Type Ia Supernovae Ginger Bryngelson Clemson University, [email protected]

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Physics of Type Ia Supernovae Ginger Bryngelson Clemson University, Gbrynge@Clemson.Edu Clemson University TigerPrints All Theses Theses 12-2008 Physics of Type Ia Supernovae Ginger Bryngelson Clemson University, [email protected] Follow this and additional works at: https://tigerprints.clemson.edu/all_theses Part of the Astrophysics and Astronomy Commons Recommended Citation Bryngelson, Ginger, "Physics of Type Ia Supernovae" (2008). All Theses. 514. https://tigerprints.clemson.edu/all_theses/514 This Thesis is brought to you for free and open access by the Theses at TigerPrints. It has been accepted for inclusion in All Theses by an authorized administrator of TigerPrints. For more information, please contact [email protected]. PHYSICS OF TYPE IA SUPERNOVAE A Thesis Presented to the Graduate School of Clemson University In Partial Fulfillment of the Requirements for the Degree Master of Science Physics by Ginger Bryngelson December 2008 Accepted by: Dr. Mark D. Leising, Committee Chair Dr. Jeremy King Dr. Bradley Meyer ABSTRACT Type Ia supernovae (SNe Ia), the thermonuclear explosion of a white dwarf, were once considered standard candles. However, increased observations reveal inhomogeneities in chemical composition and luminosity behavior, roughly dividing SNe Ia into three lu- minosity classes; super-luminous, sub-luminous, and normally-luminous. After introducing the problem in the context of previous observations and modeling, this thesis explores the physical processes occurring in a SN Ia after explosion, and discusses observations of SN light curves. A simple model of the expanding ejecta calculates the energy deposition from the decay of radioactive 56Ni as well as photon diffusion. It produces light curves that match early bolometric observations of normal SNe Ia. Variable chemical composition of the ejecta allows for testing a number of explosion scenarios. It becomes apparent that the shape of the light curve is sensitive to the amount and location of synthesized 56Ni. Monitoring gamma ray transport through Compton scattering indicates that gamma rays escape at late times. At this epoch an assumption of instantaneous deposition of energy is inaccurate. It is unclear whether positrons escape the ejecta or are trapped at even later times. The photometry of SN2007ax proved it to be the dimmest and reddest SN Ia ob- served. SN2008D was serendipitously observed in X-rays before it was even visible in optical light, revealing that an early x-ray outburst may accompany every core collapse SN. Subse- quent observations resulted in a well-sampled, multi-band early light curve. Observations of SN2006D, another SN Ia, in B, V, R, I up to ∼ 500 days after maximum light are also presented. The light curve may answer questions about the physics of SNe at late times, if more observations can be included. Future modifications of the simple model and strategies for useful observations are discussed. ii DEDICATION This thesis is dedicated to my parents and brother. Your unconditional love and support carry me through any trial I choose to face. And sharing the joy of my successes with you makes it worth the journey. I love you so much. iii ACKNOWLEDGEMENTS I would like to express my gratitude first and foremost to my advisor, Dr. Mark Leising. Your guidance and patience have helped me to understand the intricacies of SNe Ia, and also enhanced my general curiosity. I appreciate your tireless willingness to answer my questions. I also want to thank my committee, Dr. Jeremy King and Dr. Brad Meyer (and also Dr. Dieter Hartmann who might as well have been on my committee), for their continual guidance and interest in my graduate career. I want to thank Dr. Peter Milne for his invaluable help in observations and photometry, and for the chance to work with data from Super-LOTIS. I also want to thank the many graduate students whose help and witty banter was instrumental in either my use of linux/photometry/idl, or my understanding of the physics of the cosmos. These include Roggie Boone, Eric Bubar, Blake Miller, Matt Troutman, Bethany Johns, Adria Updike, Keith Davis, Allen Parker, Mark Theiling, Brian Donehew, Joe Liskowsky, and Yu Chen. A special thanks to Yu, Joe, and Tatsiana. Your friendship has brightened my life in Clemson, and kept me sane, happy, and cheerful. iv TABLE OF CONTENTS Page TITLE PAGE . i ABSTRACT . ii DEDICATION . iii ACKNOWLEDGMENTS . iv LIST OF FIGURES . vii 1. INTRODUCTION . 1 1.1 Core Collapse Supernovae . 3 1.2 Type Ia Supernovae . 4 1.2.1 Light Curve . 5 1.2.2 Optical Spectra . 9 1.3 Superluminous SNe Ia . 13 1.3.1 Superluminous Light Curves . 13 1.3.2 Superluminous Spectra . 15 1.3.3 Possible Super-luminous Explosion Scenarios . 18 1.4 Subluminous SNe Ia . 19 1.4.1 Subluminous Light Curve . 19 1.4.2 Subluminous Spectra . 20 1.4.3 Possible Sub-luminous Explosion Scenarios . 20 1.5 Width-Luminosity Relation . 22 1.6 Late Times . 24 1.6.1 Positron Deposition and Escape . 24 1.6.2 The Importance of the Infrared . 28 1.6.3 Previous Late Infrared Observations . 28 1.7 Unanswered Questions . 29 2. MODELING . 31 2.1 Nuclear Energy . 31 2.2 Decay . 32 2.3 Expansion . 34 2.4 Early Times . 36 2.4.1 Diffusion Time . 36 2.4.2 Opacity . 37 2.4.3 Energy . 38 2.4.4 Results . 39 2.4.5 Assumptions . 42 2.5 Late Times . 44 2.5.1 Gamma Ray Transport & Deposition . 44 v 2.5.2 Positron Transport & Deposition . 47 3. OBSERVATIONS . 48 3.1 Telescopes and Instruments . 48 3.1.1 Super-LOTIS . 48 3.1.2 Kuiper Telescope . 48 3.1.3 Mayall . 48 3.2 Observational Analysis Techniques . 49 3.2.1 Reductions . 49 3.2.2 Photometry . 51 3.3 SN2007ax . 54 3.4 SN2008D . 57 3.5 SN2006D . 57 3.5.1 Early Times . 61 3.5.2 Late Times . 62 4. CONCLUSIONS . 65 4.1 Models and Observations . 65 4.2 Future Work . 66 APPENDICES . 68 A. COSMOLOGICAL IMPLICATIONS . 69 B. WHITE DWARF . 73 C. SN 2007ax: AN EXTREMELY FAINT TYPE Ia SUPERNOVA . 74 D. AN EXTREMELY LUMINOUS X-RAY OUTBURST AT THE BIRTH OF A SUPERNOVA . 79 BIBLIOGRAPHY . 87 vi LIST OF FIGURES Figure Page 1.1 Optical Spectrum of Types of Supernovae . 2 1.2 Composite Normal SN Ia Light Curve in BVRI ................. 6 1.3 Decay Scheme of 56Ni → 56Co → 56Fe ...................... 8 1.4 SN Ia Light Curves in U,B,V,R,I,J,H,K ..................... 10 1.5 Early Spectra of SNe Ia . 11 1.6 Progression of SNe Ia Spectrum . 12 1.7 Light Curves of Superluminous SN Ia 1991T . 14 1.8 Early Spectrum of Superluminous SN Ia 1991T . 15 1.9 1 Week Spectrum of Superluminous SN Ia 1991T . 16 1.10 20 Day and 50 Day Spectra of Superluminous SN Ia 1991T . 17 1.11 Bolometric Light Curve of Subluminous SN Ia 1991bg . 20 1.12 Spectra of Subluminous SN Ia 1991bg . 21 1.13 Sequence and Stretch-fitting of Light Curves of all SNe Lumi- nosity Classes . 23 1.14 Light Curves of Different Deposition Assumptions . 25 1.15 SNe Ia V -band Light Curves with Models of Positron Escape . 27 1.16 UVOIR Light Curve of SN2000cx with Models of Positron Escape . 29 2.1 Number of 56Ni, 56Co, and 56Fe Nuclei . 33 2.2 Energy released from 56Ni and 56Co Decay . 34 2.3 Division of the Ejecta into Spherical Shells . 35 2.4 Power Deposited in and Escaping from SNe Ia Ejecta . 39 2.5 Model-Generated Light Curve and Observed Bolometric Light Curves of SNe Ia . 40 2.6 The Effect of 56Ni Placement on SNe Light Curves . 41 56 2.7 Light Curve of SN with 1 M of Ni....................... 42 56 2.8 Light Curve of SN with 0.07 M of Ni..................... 43 vii List of Figures (Continued) Figure Page 2.9 Schematic of a Compton Scattering . 44 2.10 Optical Depth of a SN Ia for a 1 MeV Gamma Ray . 46 3.1 Schematic of Aperture and Annulus used in Photometry . 52 3.2 Multi-band Light Curve of SN2007ax . 55 3.3 Multi-band Light Curve of SN2007ax . 56 3.4 Discovery Image of SN2008D in X-ray and UV . 58 3.5 Composite Light Curve of SN2008D . 59 3.6 SN2006D in the galaxy MCG-01-33-034 . 60 3.7 SN2006D Early Light Curve . 61 3.8 SN2006D Late Light Curve . 63 A.1 Hubble Composite Normal SN Ia Light Curve in BVRI ............ 69 A.2 SNe Ia Hubble Plot . 72 viii CHAPTER 1 INTRODUCTION A supernova is the explosive end to a massive star’s life, or, for a low mass star, is a fiery alternative to an otherwise dismal smoldering existence. These explosions can produce 100 times as much energy as the sun produces in its entire lifetime, and can temporarily rival the brightness of an entire galaxy. They enrich.
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