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Supernova Explosions 1st ed. 2017 [Kietas viršelis]

  • Formatas: Hardback, 721 pages, aukštis x plotis: 235x155 mm, 148 Illustrations, color; 88 Illustrations, black and white; XIX, 721 p. 236 illus., 148 illus. in color., 1 Hardback
  • Serija: Astronomy and Astrophysics Library
  • Išleidimo metai: 10-Aug-2017
  • Leidėjas: Springer-Verlag Berlin and Heidelberg GmbH & Co. K
  • ISBN-10: 3662550520
  • ISBN-13: 9783662550526
Kitos knygos pagal šią temą:
  • Formatas: Hardback, 721 pages, aukštis x plotis: 235x155 mm, 148 Illustrations, color; 88 Illustrations, black and white; XIX, 721 p. 236 illus., 148 illus. in color., 1 Hardback
  • Serija: Astronomy and Astrophysics Library
  • Išleidimo metai: 10-Aug-2017
  • Leidėjas: Springer-Verlag Berlin and Heidelberg GmbH & Co. K
  • ISBN-10: 3662550520
  • ISBN-13: 9783662550526
Kitos knygos pagal šią temą:
Targeting advanced students of astronomy and physics, as well as astronomers and physicists contemplating research on supernovae or related fields, David Branch and J. Craig Wheeler offer a modern account of the nature, causes and consequences of supernovae, as well as of issues that remain to be resolved.

Owing especially to (1) the appearance of supernova 1987A in the nearby Large Magellanic Cloud, (2) the spectacularly successful use of supernovae as distance indicators for cosmology, (3) the association of some supernovae with the enigmatic cosmic gamma-ray bursts, and (4) the discovery of a class of superluminous supernovae, the pace of supernova research has been increasing sharply. This monograph serves as a broad survey of modern supernova research and a guide to the current literature.

The books emphasis is on the explosive phases of supernovae. Part 1 is devoted to a survey of the kinds of observations that inform us about supernovae, some basic interpretations of such data, and an overview of the evolution of stars that brings them to an explosive endpoint. Part 2 goes into more detail on core-collapse and superluminous events: which kinds of stars produce them, and how do they do it? Part 3 is concerned with the stellar progenitors and explosion mechanisms of thermonuclear (Type Ia) supernovae. Part 4 is about consequences of supernovae and some applications to astrophysics and cosmology. References are provided in sufficient number to help the reader enter the literature.

Recenzijos

The authors received the Chambliss Astronomical Writing Award for 2019 from the American Astronomical Society (AAS)



This book aims to be a resource for those working in the field of supernovae the text covers all the basics in fairly good depth, providing ample citations for readers wishing to delve deeper. Summing Up: Recommended. Graduate students, researchers, faculty, and professionals. (D. J. Van Domelen, Choice, Vol. 55 (10), June, 2018)

Part I Observational Overview and General Interpretations
1 Overview
3(20)
1.1 Introduction
3(1)
1.2 Discovery
4(2)
1.3 Spectral Classification
6(2)
1.4 Photometry
8(4)
1.5 Spectral Evolution
12(2)
1.6 Explosion Mechanisms
14(2)
1.7 Asymmetries and Polarization
16(1)
1.8 Sites, Environments, and Rates
16(2)
1.9 Circumstellar Interaction
18(1)
1.10 Supernova Remnants
19(1)
1.11 Gamma-Ray Bursts
20(1)
1.12 Summary
21(2)
2 Search and Discovery
23(10)
2.1 Introduction
23(2)
2.2 Nearby Supernovae
25(2)
2.3 Hubble-Flow Supernovae
27(2)
2.4 High-Redshift Supernovae
29(2)
2.5 Summary
31(2)
3 Environments and Rates of Supernovae
33(14)
3.1 Introduction
33(1)
3.2 Direct Detection of Progenitors and Companion Stars
33(3)
3.3 Environments in the Local Universe
36(2)
3.4 Rates in the Local Universe
38(2)
3.5 The Galactic Rate
40(1)
3.6 Inferences from Rates About Progenitors of Core-Collapse Supernovae
41(1)
3.7 Rates Versus Redshift
42(1)
3.8 The SN Ia Delay-Time Distribution
43(2)
3.9 Summary
45(2)
4 Spectra
47(28)
4.1 Introduction
47(1)
4.2 Elements of Line Formation in the Photospheric Phase
48(8)
4.2.1 The Velocity Law
49(1)
4.2.2 Resonant-Scattering Line Profile: Qualitative Overview
49(2)
4.2.3 Resonant-Scattering Line Profile: More Quantitative
51(3)
4.2.4 Multiple Scattering: Line Blending
54(2)
4.3 Lines To Be Considered
56(1)
4.4 Synthetic Spectra for the Photospheric Phase
57(7)
4.4.1 SYNOW
57(2)
4.4.2 Elementary Monte Carlo
59(1)
4.4.3 Detailed Calculations
59(5)
4.5 The Nebular Phase
64(3)
4.6 Spectropolarimetry
67(6)
4.7 Summary
73(2)
5 Light Curves
75(26)
5.1 Introduction
75(1)
5.2 Physical Conditions
75(2)
5.3 Understanding Basic Properties of Supernova Light Curves
77(4)
5.4 Energy Sources
81(11)
5.4.1 Shock Energy: Breakout, Fireball, and Plateau
81(1)
5.4.2 Radioactive Decay of 56Ni and 56Co
82(8)
5.4.3 Gamma-Ray Light Curves
90(1)
5.4.4 Buried Pulsar/Magnetar
91(1)
5.5 Application to Supernova Types
92(7)
5.5.1 SN Ia
92(3)
5.5.2 SN Ib/c
95(1)
5.5.3 SN IIB
96(1)
5.5.4 SN IIP
96(2)
5.5.5 SN 1987A
98(1)
5.5.6 Light-Curve Extremes
98(1)
5.6 Detailed Calculations
99(1)
5.7 Summary
99(2)
6 Circumstellar Interaction
101(14)
6.1 Introduction
101(1)
6.2 Hydrodynamic Interaction
102(2)
6.3 Optical, UV, and X-ray Emission from the Shocked Regions
104(1)
6.4 Optical, UV, and X-ray Emission from the Unshocked Regions
105(1)
6.5 Radio Emission
105(3)
6.6 Dust and Infrared Emission
108(1)
6.7 Clumps
109(1)
6.8 Shells
110(1)
6.9 Optically-Thick CSM
110(2)
6.10 Core-Collapse Supernovae
112(1)
6.11 Type la Supernovae
112(1)
6.12 Summary
113(2)
7 Supernova Remnants
115(20)
7.1 Introduction
115(1)
7.2 SNR Populations
116(2)
7.2.1 Galactic SNRs
116(1)
7.2.2 Extragalactic SNRs
117(1)
7.3 Evolution of Shell SNRs
118(1)
7.3.1 Classical Theory
118(1)
7.3.2 Presupernova Shells
118(1)
7.4 Young SNRs
119(14)
7.4.1 Cassiopeia A
120(3)
7.4.2 SN 1054 and the Crab Nebula
123(3)
7.4.3 SN 1181 and SNR 3C58
126(1)
7.4.4 SN 1572 and the Tycho SNR
127(2)
7.4.5 SN 1604 and the Kepler SNR
129(1)
7.4.6 SN 1006 and SNR G327.6+14.6
130(1)
7.4.7 SN 185 and SNR RCW 86
131(1)
7.4.8 G1.9+0.3: The Youngest Known Galactic SNR
132(1)
7.4.9 SN 1885A and Its SNR in the Andromeda Galaxy
133(1)
7.5 Summary
133(2)
8 Evolution to Catastrophe
135(38)
8.1 Introduction
135(4)
8.2 Making White Dwarfs
139(3)
8.3 Red Giants and Red Supergiants
142(6)
8.3.1 Dredge-Up
143(2)
8.3.2 AGB Stars, SAGB Stars, Thermal Pulses
145(2)
8.3.3 C, S, and M Stars
147(1)
8.4 Mass Loss
148(4)
8.4.1 Radiation-Driven Mass Loss in Massive Stars
149(1)
8.4.2 AGB Mass Loss
150(2)
8.4.3 Mass Loss by Luminous Blue Variables
152(1)
8.5 Presupernova Evolution
152(7)
8.5.1 Helium Flash
152(1)
8.5.2 Evolution to Degenerate Carbon Ignition
153(1)
8.5.3 Degenerate Oxygen-Neon-Magnesium Cores
154(1)
8.5.4 Off-center Oxygen and Neon Ignition
155(1)
8.5.5 Iron-Core Evolution
156(3)
8.6 Dynamic Instability
159(3)
8.7 Evolution with Rotation
162(2)
8.8 Binary-Star Evolution
164(4)
8.9 Summary
168(5)
Part II Massive-Star Supernovae
9 Core Collapse
173(38)
9.1 Introduction
173(1)
9.2 History of the Collapse Problem
174(4)
9.3 Collapse Physics
178(7)
9.3.1 Entropy
178(2)
9.3.2 The Equation of State
180(1)
9.3.3 Weak Interactions
181(2)
9.3.4 Neutrino Transport
183(2)
9.4 Collapse Dynamics
185(13)
9.4.1 Initial Iron-Core Collapse
185(3)
9.4.2 Electron Capture and Accretion-Induced Collapse
188(1)
9.4.3 Post-Bounce Dynamics
189(1)
9.4.4 Standing Shock Phase
190(2)
9.4.5 Explosion Phase
192(2)
9.4.6 Fluid Instabilities
194(2)
9.4.7 The Standing Accretion Shock Instability: SASI
196(2)
9.5 Rotation and Magnetic Fields
198(8)
9.5.1 Basic Magnetorotational Physics: Length and Time Scales
199(2)
9.5.2 Magnetic-Field Compression and Wrapping
201(1)
9.5.3 The Magnetorotational Instability: MRI
202(3)
9.5.4 Other MHD Processes
205(1)
9.5.5 Non-Axisymmetric Instabilities: NAXI
205(1)
9.6 Black Hole Formation
206(2)
9.7 Quark and Strange Stars
208(1)
9.8 Summary
208(3)
10 Pair-Instability Supernova Models
211(8)
10.1 Introduction
211(1)
10.2 Pre-Explosion Evolution
211(2)
10.3 Dynamics of Pair Instability
213(1)
10.4 Nucleosynthesis
214(1)
10.5 Predicted Observational Properties
214(2)
10.6 Upper Limit to PISN: Collapse to Black Holes
216(1)
10.7 Pulsational Pair Instability: PPISN
217(1)
10.8 Summary
218(1)
11 Supernova 1987A
219(26)
11.1 Introduction
219(1)
11.2 The Progenitor Star and the Triple-Ring System
219(4)
11.3 Neutrinos and the Compact Remnant
223(3)
11.4 Ejecta
226(11)
11.4.1 Breakout and Fireball
226(1)
11.4.2 Radioactivity
227(3)
11.4.3 Molecules and Dust
230(1)
11.4.4 Asymmetries and Mixing
231(6)
11.5 Nucleosynthesis
237(3)
11.6 Circumstellar Interaction
240(2)
11.7 Related Progenitor Stars and Supernovae
242(1)
11.8 Summary
243(2)
12 Type IIP Supernovae
245(22)
12.1 Introduction
245(1)
12.2 Case Study: SN 1999em
246(3)
12.3 Expected Progenitor Structures
249(2)
12.4 Breakout, Fireball, and Rise-Time
251(1)
12.5 The Plateau Phase
252(6)
12.5.1 Typical SN IIP
253(1)
12.5.2 Weak SN IIP
254(2)
12.5.3 Continuity and Correlations
256(1)
12.5.4 Estimating Masses and the Red Supergiant Problem
256(2)
12.6 The Nebular Phase
258(2)
12.7 Circumstellar Interaction
260(1)
12.8 Dust
261(1)
12.9 Polarization and Asymmetry
262(2)
12.10 Summary
264(3)
13 Type IIL Supernovae
267(14)
13.1 Introduction
267(1)
13.2 Case Studies
268(7)
13.2.1 SN 1979C
268(4)
13.2.2 SN 1980K
272(3)
13.3 Synthesis of SN IIL Characteristics
275(4)
13.4 Summary
279(2)
14 Type IIL Supernovae
281(38)
14.1 Introduction
281(1)
14.2 Case Studies
282(11)
14.2.1 SN 1988Z
282(3)
14.2.2 SN 1998S
285(4)
14.2.3 SN 2010jI
289(4)
14.3 Synthesis of SN IIn Characteristics
293(14)
14.3.1 Light-Curve Subtypes
293(5)
14.3.2 Spectra
298(2)
14.3.3 Mass Loss and Circumstellar Medium
300(2)
14.3.4 Infrared Observations and Dust
302(1)
14.3.5 Polarization and Asymmetry
302(5)
14.3.6 Statistics
307(1)
14.4 Impostors
307(6)
14.5 SN1994W-Likes
313(3)
14.6 Summary
316(3)
15 Type IIb Supernovae
319(26)
15.1 Introduction
319(1)
15.2 Case Study: SN 1993J
320(13)
15.2.1 Light Curve
320(2)
15.2.2 Spectra
322(1)
15.2.3 Polarization and Asymmetry
323(3)
15.2.4 Circumstellar Interaction
326(1)
15.2.5 Evolutionary Models
327(1)
15.2.6 Model Light Curves
328(1)
15.2.7 Models of Photospheric Spectra
329(3)
15.2.8 Models of Nebular Spectra
332(1)
15.3 Synthesis of SN IIb Characteristics
333(5)
15.3.1 SN IIb Subtypes
333(1)
15.3.2 Light Curves
333(1)
15.3.3 Spectra
334(2)
15.3.4 Circumstellar Interaction
336(1)
15.3.5 Polarization and Asymmetry
336(2)
15.4 Models of SN IIb
338(5)
15.4.1 Evolutionary Models
338(3)
15.4.2 Model Light Curves
341(1)
15.4.3 Models of Photospheric Spectra
342(1)
15.4.4 Models of Nebular Spectra
343(1)
15.5 Summary
343(2)
16 Type Ib Supernovae
345(34)
16.1 Introduction
345(1)
16.2 Case Studies
346(6)
16.2.1 SN 1983N
346(4)
16.2.2 SN 2008D
350(2)
16.3 Synthesis of SN Ib Characteristics
352(14)
16.3.1 Light Curves
353(3)
16.3.2 Spectra
356(4)
16.3.3 Polarization and Asymmetry
360(5)
16.3.4 Circumstellar Interaction
365(1)
16.4 Models of SN Ib
366(4)
16.4.1 Evolutionary Models
366(1)
16.4.2 Model Light Curves
367(1)
16.4.3 Models of Photospheric Spectra
368(2)
16.4.4 Models of Nebular-Phase Spectra
370(1)
16.5 SN Ibn
370(5)
16.5.1 Case Study: SN 2006jc
371(2)
16.5.2 Synthesis of SN Ibn Characteristics
373(2)
16.6 Summary
375(4)
17 Type Ic Supernovae
379(34)
17.1 Introduction
379(1)
17.2 Case Study: SN 19941
380(5)
17.3 Synthesis of SN Ic Characteristics
385(8)
17.3.1 Light Curves
385(3)
17.3.2 Spectra
388(3)
17.3.3 Polarization and Asymmetry
391(1)
17.3.4 Circumstellar Interaction
392(1)
17.4 SN Ic-bl
393(9)
17.4.1 Case Study: SN 2002ap
393(4)
17.4.2 Synthesis of Properties of SN Ic-bl
397(2)
17.4.3 The Connection Between SN Ic-bl and Gamma-Ray Bursts
399(3)
17.5 Models of SN Ic and SN Ic-bl
402(9)
17.5.1 Evolutionary Models
403(1)
17.5.2 Models of Light Curves
404(4)
17.5.3 Models of Photospheric Spectra
408(2)
17.5.4 Models of Nebular Spectra
410(1)
17.6 Summary
411(2)
18 Superluminous Supernovae
413(24)
18.1 Introduction
413(3)
18.2 SLSN-II
416(6)
18.2.1 Case Study: SN 2006gy
416(3)
18.2.2 Synthesis of SLSN-II Characteristics
419(3)
18.3 SLSN-I
422(8)
18.3.1 Case Study: SN 2010gx
422(1)
18.3.2 Synthesis of SLSN-I Characteristics
423(7)
18.4 Superluminous PISN?
430(2)
18.5 Summary
432(5)
Part III Type Ia Supernovae
19 Degenerate Carbon Burning
437(46)
19.1 Introduction
437(1)
19.2 Single Degenerate: The Smoldering Phase
437(3)
19.3 Convective Urea Process
440(1)
19.4 Dynamical Degenerate Carbon Burning
441(7)
19.4.1 General Considerations
441(2)
19.4.2 The Basics of Supersonic and Subsonic Combustion
443(5)
19.5 Astrophysical Deflagration: Subsonic Burning and Combustion
448(5)
19.5.1 Laminar Flames
449(3)
19.5.2 Rayleigh-Taylor Instability
452(1)
19.6 Interaction of Buoyancy, Turbulence and Flames
453(9)
19.6.1 Landau-Darrieus Instability
453(2)
19.6.2 Buoyancy-Driven Flames
455(1)
19.6.3 The Gibson Scale
455(3)
19.6.4 Turbulent Flames
458(2)
19.6.5 Distributed Flames?
460(2)
19.7 Ignition Kernels
462(1)
19.8 Early Runaway: Hot Spots and Bubbles
463(3)
19.9 Astrophysical Detonation: Supersonic Burning
466(1)
19.10 Detonation Instability
467(5)
19.11 Deflagration-to-Detonation Transition
472(8)
19.11.1 The Zel'dovich Gradient Mechanism
473(2)
19.11.2 Turbulent Flame-Brush Instability
475(3)
19.11.3 DDT Due To Turbulent Flame-Brush Instability
478(2)
19.12 Summary
480(3)
20 Observational Properties
483(36)
20.1 Introduction
483(1)
20.2 Case Studies
484(12)
20.2.1 SN 2011fe
484(5)
20.2.2 SN 2014J
489(7)
20.3 Homogeneity
496(5)
20.4 Diversity and Correlations
501(6)
20.5 Multiparameter Subclassification
507(4)
20.6 Colors and Extinction
511(1)
20.7 Substantially Super-Chandrasekhar SN Ia
512(1)
20.8 Outliers
513(1)
20.9 Correlations Between Properties of SN Ia and Host Galaxies
514(2)
20.10 Variations with Redshift
516(1)
20.11 Summary
516(3)
21 Progenitors
519(36)
21.1 Introduction
519(4)
21.2 Single Degenerates
523(13)
21.2.1 Canonical SD Model: C/O White Dwarfs Accreting to the Chandrasekhar Mass
524(4)
21.2.2 Canonical SD Model: Binary Evolution and Population Synthesis
528(3)
21.2.3 Distribution Predictions
531(2)
21.2.4 M-Dwarf Donors?
533(1)
21.2.5 Super-Chandrasekhar Single Degenerates
534(1)
21.2.6 Sub-Chandrasekhar Single Degenerates
535(1)
21.3 Double Degenerates
536(5)
21.3.1 Canonical Super-Chandrasekhar DD Model
536(1)
21.3.2 Canonical DD Model: Binary Evolution and Population Synthesis
537(2)
21.3.3 Noncanonical and Sub-Chandrasekhar Possibilities
539(2)
21.4 Core Degenerates
541(1)
21.5 Observed Candidate Progenitor Systems
542(2)
21.5.1 Recurrent Novae
542(1)
21.5.2 Other Possibilities
543(1)
21.6 Other Evidence Constraining Progenitor Systems
544(8)
21.6.1 Archival Observations at Supernova Sites
544(1)
21.6.2 Statistics of Supersoft X-Ray Sources
545(1)
21.6.3 Breakout and Interaction with an Accretion Disk
546(1)
21.6.4 Interaction with a Donor Star
546(2)
21.6.5 Circumstellar Interaction
548(2)
21.6.6 Supernova Remnants
550(1)
21.6.7 White Dwarf Populations
551(1)
21.6.8 Abundance Constraints
552(1)
21.7 Summary
552(3)
22 Explosion Models
555(26)
22.1 Introduction
555(2)
22.2 Dark Time
557(2)
22.3 Single-Degenerate Chandrasekhar-Mass Models
559(16)
22.3.1 Central Detonation
559(1)
22.3.2 Model W7
559(1)
22.3.3 3D Deflagrations
560(1)
22.3.4 Delayed Detonations
561(8)
22.3.5 Pulsation-Driven Detonations
569(1)
22.3.6 Gravitationally-Confined Detonations
570(2)
22.3.7 Single-Degenerate Super-Chandrasekhar Models
572(1)
22.3.8 Single-Degenerate Sub-Chandrasekhar Models
573(2)
22.4 Double-Degenerate Models
575(3)
22.4.1 The Canonical Double-Degenerate Model
575(1)
22.4.2 Other Double-Degenerate Possibilities
576(2)
22.5 Summary
578(3)
23 Related Explosions
581(16)
23.1 Introduction
581(1)
23.2 SN 2002ic-Likes: SN Ia-CSM
581(4)
23.3 SN 2002cx-Likes: SN Iax
585(5)
23.4 SN 2002bj-Likes: SN Ia?
590(2)
23.5 SN 2005E-Likes: Calcium-Rich Transients
592(2)
23.6 Summary
594(3)
Part IV Consequences, Applications, and Summary
24 Consequences of Supernovae
597(28)
24.1 Introduction
597(1)
24.2 Compact Remnants
597(7)
24.2.1 Neutron Stars
598(3)
24.2.2 Black Holes
601(3)
24.3 Surviving Companion Stars
604(1)
24.4 Neutrinos and Gravitational Waves
605(2)
24.5 Nucleosynthesis
607(5)
24.6 Dust
612(1)
24.7 Mechanical and Radiative Feedback
613(4)
24.7.1 Current Epoch
614(2)
24.7.2 Early Universe
616(1)
24.8 Chemical Enrichment
617(3)
24.8.1 The Galaxy
618(1)
24.8.2 Damped Lyman-α Clouds
619(1)
24.9 Cosmic Rays
620(1)
24.10 Gamma Rays
621(1)
24.11 Effects on the Solar System?
622(1)
24.12 Life
622(2)
24.13 Summary
624(1)
25 Applications of Supernovae to Other Areas of Astrophysics and Physics
625(12)
25.1 Introduction
625(1)
25.2 Distances to Type Ia Supernovae
625(4)
25.2.1 Accelerating Cosmic Expansion and Dark Energy
625(2)
25.2.2 Flows, Peculiar Velocities, and Anisotropy
627(1)
25.2.3 Cosmic Opacity
628(1)
25.2.4 The Hubble Constant
628(1)
25.3 Distances to Core-Collapse Supernovae
629(1)
25.4 Astrophysics
630(4)
25.4.1 Interstellar Medium
630(2)
25.4.2 Supernovae from the First Stars
632(1)
25.4.3 Lensing
632(2)
25.4.4 Time Dilation
634(1)
25.4.5 Finding Dwarf Galaxies and Intracluster Populations
634(1)
25.5 Physics
634(1)
25.5.1 Constraints from Core Collapse
634(1)
25.5.2 Constraints from SN Ia
635(1)
25.6 Summary
635(2)
26 Summary and Prospects
637(6)
26.1 Introduction
637(1)
26.2 Massive-Star Supernovae
637(1)
26.3 Type Ia Supernovae
638(1)
26.4 Prospects
639(3)
26.4.1 Observations
639(2)
26.4.2 Modeling
641(1)
26.5 Conclusion
642(1)
Appendix: Abbreviations 643(4)
References 647(52)
Index 699
David Branch received his Ph.D. in astronomy from the University of Maryland in 1969.  He then served as Postdoctoral Research Fellow at the Goddard Space Flight Center (1969), the California Institute of Technology (1969-70), and the Royal Greenwich Observatory, England, (1970-73).  During those years he worked on the spectroscopic determination of the relative abundances of the chemical elements in the Sun and stars, and began to work on the interpretation of the spectra of supernovae.  In 1973 he joined the faculty of the University of Oklahoma as Assistant Professor and became Full Professor in 1981.  From 1985 to 1990 he served as Chair of the Department of Physics and Astronomy.  In 1987 he received the career appointment of George Lynn Cross Research Professor.  During his tenure at Oklahoma he also held Visiting-Professor appointments at the University of Texas (1979-80), Oxford University (1980), the University of California, Santa Cruz (1984), and the University of Munich (1987), as well as Visiting Senior Scientist appointments at the Lawrence Berkeley National Laboratory (1991) and the International School of Advanced Studies, Trieste, Italy (1997).  He is a member of the American Astronomical Society and the International Astronomical Union.  He received the Senior United States Scientist Award of the Alexander Humboldt Foundation, Germany (1988) and the Distinguished Alumnus Award of the Department of Astronomy, University of Maryland (2004).  He has published more than 300 refereed scientific papers.  At the University of Oklahoma, his research has concentrated on advancing our understanding of the physics of supernova explosions, with emphasis on the interpretation of the spectra of supernovae.  He was an early and persistent advocate of using supernovae to determine the history of the expansion rate of the universe. J. Craig Wheeler received his PhD in physics from the University of Colorado, Boulder, in 1969. He was a Postdoctoral Fellow at the California Institute of Technology from 1969 to 1971 and Assistant Professor of Astronomy at Harvard from 1971 to 1974. In 1974, he joined the University of Texas at Austin as Associate Professor of Astronomy. He became Full Professor in 1980, was appointed the Samuel T. and Fern Yanagisawa Regents Professor of Astronomy in 1985 and was Chair of the Department from 1986 to 1990. He has won a number of teaching awards, was appointed to the Academy of Distinguished Teachers in 2002, and received the state-wide Regents Award for Outstanding Teaching in 2010. He has published over 350 refereed scientific papers, a popular book on supernovae and gamma-ray bursts (Cosmic Catastrophes), two novels, and has edited six books. He was a Visiting Fellow at the Joint Institute for Laboratory Astrophysics (JILA) in 1979 and the Japan Society for the Promotion of Science in 1983, AURA/NOAO Visiting Professor in 1990, and a Fulbright Fellow in Italy in 1991. He is a long-time member of the Aspen Center for Physics and has done stints as Trustee there. He was a member of the Executive Committee of the Texas Symposium on Relativistic Astrophysics for twenty years. He has served on a number of agency advisory committees, including those for the National Science Foundation for which he chaired the Committee of Visitors of the Astronomy Division in 2005, the National Aeronautics and Space Administration for which he chaired the Senior Review of Operating Missions in 2010, and the National Research Council where he was Co-Chair of the Committee on the Origin and Evolution of Life from 2002 to 2005, a member of the Space Sciences Board from 2002 to 2006, a member of the Committee on Astronomy and Astrophysics from 2012 to 2015, and a member of the Committee on A Strategy to Optimize the U.S. Optical and Infrared System in the Era of the Large Synoptic Survey Telescope from 2014 to 2015. He has held many positions in the American Astronomical Society and was President of the Society from 2006 to 2008.  His research interests span all aspects of supernovae, both theory and observations, thermonuclear and core collapse.  He has also worked on closely related areas including late phases of stellar evolution, accretion disks, black holes, and astrobiology.