Chapter
10. Microquasars in our Galaxy
11. Challenges for the future
Nucleosynthesis basics and applications to supernovae
1. Thermonuclear Rates and Reaction Networks
1.1. Thermonuclear Reaction Rates
1.2. Nuclear Reaction Networks
2. Theoretical Cross Section Predictions
2.1. Thermonuclear Rates from Statistical Model Calculations
2.2. Transmission Coefficients
2.5. Applicability of the Statistical Model
3. Nucleosynthesis Processes in Stellar Evolution and Explosions
3.1. Hydrostatic Burning Stages in Presupernova Evolution
3.2.1. Explosive He-Burning
3.2.2. Explosive C- and Ne-Burning
3.2.3. Explosive O-Burning
3.2.4. Explosive Si-Burning
3.3. Nucleosynthesis in Super
4. Type II Supernova Explosions
4.1. Basic Nucleosynthesis Features
4.2. Ni(Fe)-Ejecta and the Mass Cut
4.3. Observational Constraints
5.1. Model-Independent Studies
5.2. Parameter Studies for High Entro
5.2.1. The Model and Nuclear Inpu
5.2.2. Superpositions of Entropies
Signatures of nucleosynthesis in explosive stellar processes
2. Reaction Rates and Decay Rates
3. Overview of Stellar Nucleosynthesis Processes
3.1. Stellar hydrogen burning through the pp-chains and the CNO cycles
3.2. Stellar helium burning and neutron sources for the s-process
3.3. Convective burning processes in AGB stars
4. Explosive stellar processes and radioactive beam experiments
5. Nucleosynthesis of 15N in Novae
5.1. CNO Nucleosynthesis in Ne Novae
5.2. 22Na Production in Ne-Novae
5.3. Experimental study of the23 Al(p,y)24 Si rate
6.1. The Lifetime Measurement of 44Ti
6.2. Implications for the understanding of the 44Ti production in supernovae
7. X-ray bursts as possible source for light p-nuclei?
7.1. rp-process in X-ray bursts
7.2. The rp-process in the thermal runaway of the x-ray burst
7.3. x-ray burst nucleosynthesis of the light p-nuclei?
Neutrino transport and large-scale convection in core-collapse supernovae
2. Hydrostatic Equilibrium
4. Quantum Gases and Degenerate Matter.
4.2. Transition from Classical to Quantum Gas Behavior
4.3. The Degenerate Electron Gas
4.4. Nonrelativistic Degenerate Electrons
5. The Hertzsprung-Russell Diagram.
5.2. The HR Diagram as an Evolutionary Sequence
6. Some Timescales of Significance
6.1. Nuclear Burning Timescales
6.2. Hydrodynamical Timescales
6.3. Timescale Set by Random Walk of Diffusing Particl
7. Advanced Stellar Burning Stages
7.5. Timescales for Advanced Burning
9. Energy Transport in Stars
9.2. Radiative Energy Transport by Photons
9.3. Energy Transport by Convection
10. Conditions for Convective Instability
10.1. Schwarzschild Instability
11. Critical Temperature Gradient for Convection
11.1. Role of the Adiabatic Index in Convection
11.2. Role of the Pressure Gradient in Convection
12. Stellar Temperature Gradients
13. Examples of Convective Regions in Normal Stars
13.1. Surface Ionization Zones
13.2. Convection in the Cores of Stars
14. Critical Luminosities
14.1. Eddington Luminosity
14.2. Limiting Neutrino Luminosities
15. The Death of Massive Stars
16. Sequence of Events in Core Collapse
17.1. Neutrino Interactions
17.2. Reheating of Shocked Matter
17.3. Calculations with Neutrino Reheating
18.1. The Diffusion Approximation
18.2. Causality Violation
18.4. Multigroup Diffusion
18.5. Multigroup Flux-Limited Diffusion
19. Convection and Neutrino Reheating
20. Convection in Multidimensional Hydrodynamics
20.1. Method of Calculation
20.2. Results for Prompt Convection
20.3. Analytical Model of "Leaky Convection"
20.4. Neutrino-Driven Convection
20.5. Summary of 2D Hydro + MGFLD Results
21. Boltzmann Neutrino Transport
1.1. Some observed neutron star properties
1.1.2. Thermal emissions and surface temperatures
2. Neutron star structure
2.1. Equations of stellar structure
2.2. Macroscopic properties
2.3. Constraints on the EOS
3.4. Charge neutral neutron-rich matter
3.5. State variables at nuclear density
3.6. EOS and the maximum mass of neutron stars
4.1. Matter with strangeness-rich baryons
4.1.1. Model calculations
4.1.2. Coupling Constants
4.1.3. Stellar structure with hyperons
4.2. Matter with Bose condensates
4.3.2. Condensation in nucleons-only matter
4.3.3. Condensation in matter with hyperons
4.4.2. Quark-hadron phase transition
4.4.3. Stellar structure results
5. Neutrino trapped matter
5.1. The Fate of a Newborn Neutron Star
5.2. Equilibrium conditions
5.3. Neutrino-poor versus neutrino-rich stars
6. Cooling of neutron stars
6.2. Neutrino emission processes
6.3. The direct Urea process revisited
6.4. Direct Urea processes with hyperons and A-isobars
6.4.1. Neutrino emissivity from hyperon Urea processes
6.4.2. Threshold concentrations for hyperon Urea processes
6.5. Neutrino emission from, exotic states
6.7. Model calculations of cooling
1. Introduction, formalism, and cosmological bound
1.1. Neutrino electron (or neutrino quark) interaction cross section (schematic)
1.2. Motivation for neutrino mass
1.3. Brief formal discussion of discrete symmetries
1.6. Cosmological constraint on neutrino mass
1.6.2. Density of relic neutrinos
1.6.3. Cosmological neutrino mass limit
2. Kinematic determination of neutrino mass. Neutrino Oscillations.
2.1. Time of flight method
2.2. Kinematic tests for neutrino mass
2.2.1. Tau neutrino mass limit
2.3. Muon and tau neutrinos from future galactic supernovae
2.4. Number of neutrino flavors from the width of Z
3. Solar neutrinos and matter oscillations
3.1. Neutrinos from the Sun
3.1.1. The predicted neutrino spectrum from the Sun
3.2. Neutrino Oscillations in Matter
3.3. MSW effect for solar neutrinos
4. Atmospheric neutrinos, LSND, double beta decay, conclusions
4.1. Atmospheric neutrino anomaly
4.3. Summary of oscillations evidence
4.4. Dirac versus Majorana neutrinos
4.4.1. Majorana neutrino in a uniform EM field
4.4.2. Neutral currents of Majorana neutrinos
4.5. Neutrinoless double beta decay
4.5.1. Decay amplitude, purely left-handed currents
4.5.2. The case of right-handed currents
4.5.3. Search for the Ov decay
Cosmic ray physics and astrophysics
2. Standard model of galactic cosmic rays
2.1. Propagation and energetics
2.2. Dynamic interstellar medium
2.3. Diffuse j-radiation from the galactic disk
2.4. Fermi acceleration and maximum energy
2.5. SNR as j-ray sources
3. The knee region and beyond
3.1. Models for higher energy galactic sources
3.2. Evidence from composition
3.3. Hybrid air shower detectors
3.4. Fly's Eye experiment
4. Extragalactic cosmic rays
4.1. Some possible accelerators
4.2. The highest energy cosmic ray
5. High energy neutrino astronomy?
Physical cosmology for nuclear astrophysicists
2. Age of the Universe and the Hubble Expansion
2.1. The Age From Dynamics
2.2. The Age From the Oldest Stars
2.3. Nucleocosmochronology
3. The Cosmic Microwave Background (CMB)
4. Big Bang Nucleosynthesis
5. Dark Matter and Visible Matter
6. The Need for Non-Baryonic Dark Matter
7. Seeds and Large Scale Structure
8. Alternative Measures of Ω B
Nuclear and Particle Astrophysics
( Cambridge Contemporary Astrophysics )
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