Sample Course Syllabi
D. Backer, 95F
Main References: Shu, The Physics of Astrophysics Vol. I : Radiation Rybicki & Lightman, Radiative Processes in Astrophysics AY201 Big Black Binder in 5th floor Campbell library Arons, Notes from AY 201A Other References: Spitzer, Physical Processes in the Interstellar Medium Longair, High Energy Astrophysics, 2nd edition, 2 Vol. Mihalas, Stellar Atmospheres Bond, Watson, & Welch, Atomic Theory of Gas Dynamics Allen, Astrophysical Quantities Lang, Astrophysical Formulae Maran (ed.), The Astronomy and Astrophysics Encyclopedia [von Nostrand] Introduction: radiation definitions, black body radiation, photon/wave approaches, noise Shu 1 presents some definitions and photon equation of state; Shu 11-12 treat wave approach and polarization; problem 3.3 is an E&M exercise. RL 1.1-1.4 discuss definitions; 1.5 black body radiation; 2.1-2.3 E&M approach; 2.4 polarization. Continuum radiative transfer Shu 1 sets up the radiative transfer equation; Shu 2 looks at a closure approach to solution; Shu 3 looks at radiative equilibrium solution; Shu 4 considers classical problem of plane parallel LTE stellar atmosphere; Shu 5 applies these concepts to IR radiation from spherical dust accreting onto a protostar; problem 1.2 deals with iterative techniques and problem 1.3 with LTE grey atmosphere. RL 1.4 presents radiative transfer equation; 1.7 comments on scattering opacity; 1.8 looks at stellar photosphere; 2.6 makes link between photon/wave approaches. Spitzer 3.1-3.2 introduce radiative transfer and 3.5 deals with example of free-free emission/absorption. Multipole radiation, bremsstrahlung, Raleigh/electron scattering Shu 13-14 develop classical dipole radiation; the end of Shu 14 discusses Rayleigh and Thomson (electron) scattering as limiting cases of more general classical theory of radiation damping; Shu 15 presents emission and absorption bremsstrahlung processes; problem 3.2 involves Thompson scattering. RL 2.5,3.1-3.6 are counterparts to Shu 13-14; bremsstrahlung, including relativistic regime are in RL 5 (with relitivity introduced in RL 4); Compton regime is discussed in RL 7. Physical state of matter and interactions with radiation Shu 6-8 discuss the state of matter and interactions; Shu 10 looks at the classical problem of ionization balance of HII regions as an example system; problem 1.1 and problem set 2 deal with state of matter; problem 3.1 looks at radial structure of an HII region while problem 4.3 addresses radio wavelength observations of same. RL treat this lightly -- see introduction of Einstein coefficients in 1.6; scattering in 1.7 and Boltzmann/Saha in 9.5; collisions are discussed as a line broadening source in 10.6. Spitzer 4-5 is comprehensive discussion on excitation/ionization/dissociation topics (for case of ISM); basics on Einstein coefficients are introduced in 3.2-3.3. Bond, Watson, & Welch incorporate a broad study of this and item 6 below in their chapters 4,5,6,8. Line Radiative Transfer Shu 3 mentions line radiative transfer, but the basic treatment is in Shu 6; the latter half of Shu 6 discusses several simple examples. RL do not treat this. Spitzer presents curve of growth for interstellar absorption lines in 3.4. Parameters of Atomic and Molecular Processes Shu 21-27 presents basic quantum theory of atomic processes; Shu 28-30 then pick up molecular quantum theory; problem sets 5 and 6 deal with these fundamental processes. RL deal with these topics in 9-11: atomic structure, radiative transitions, and molecular structure. Synchrotron Radiation, Inverse Compton Shu 16-19 starts with radiation from relativisitically moving charge, then develops synchroton theory semi-qualitatively, then rigorously. RL discuss this in 6. Pulsar Radiation, Interstellar Medium Propagation Shu 20 addresses propagation effects in interstellar medium; problems 4.1 and 4.2 are concerned with the classical problem of electromagnetic torque on a neutron star (pulsar). RL deal with plasma effects on radiation in 8. Gravitational Radiation, Gravitational Lensing
J. Graham, 95S
The Cosmos is a wonderful hydrodynamics laboratory that provides us with examples of supersonic motion, magnetohydrodynamic flows, turbulence, and a rich array of instabilities. Astronomers and astrophysicists need a framework within which to explore and understand these phenomenon. This class, the second part of the "Physics for Astrophysics" course taught in the Astronomy Department, will provide the basic tools for understanding astronomical observations by developing a theoretical description of gas dynamics.
No background in fluid mechanics is assumed, but the course is intended for physics/astrophysics students with a strong grounding in mathematics at a senior undergraduate level. Astronomical phenomenology will be introduced in context.
Recommended Textbook:
"The Physics of Astrophysics: Vol 2, Gas Dynamics", F. H. Shu,
University Science Books, Mill Valley, 1992.
Useful texts include:
"Fluid Mechanics", Landau \& Lifshitz, Pergamon Press, London.
"An Album of Fluid Motion", van Dyke, Parabolic Press, Stanford.
"Introduction to Mathematical Fluid Dynamics", R. E. Meyer, Dover, New York.
Syllabus
Basic Fluid Dynamics 1: Inviscid Flow
Hydrostatics
Equations of motion: Euler's equations
Steady flow: Bernoulli's theorem
Circulation
Vortex lines
Basic Fluid Dynamics 2: Viscous Flow
Viscosity
Viscous flow
Reynolds number
Flow past a cylinder
Limit of zero viscosity
Couette flow
Kinetic Theory
Boltzmann's equation
Moment equations
Transport coefficients
Navier--Stokes' equation
Fluids as Continua
Stokes' theorem
Eulerian and Langranian descriptions
Conservation equations
Accretion
Collisionless spherical accretion
Hydrodynamic spherical accretion
Accretion disks and X--ray sources
Disk structure
Instabilities
Sound waves
Jeans' instability
Convective instability
Rotational instability
Rayleigh--Taylor, Kelvin--Helmholtz, \& Parker instabilities
Thermal instability
Turbulence
Boundary layers and vortex sheets
Blasius' problem
Transition to turbulence
Kolmogorov spectrum
Convection
Mixing length theory
Convective flux
Spiral Density Waves
Basic equations
Equilibrium and perturbations
WKBJ approximation
Observational background
Kinematics
Dispersion relations and stability
Wave propagation and amplification
Shock Waves
Characteristics and simple waves
Formation of shocks
Jump conditions
Riemann invariant and flow visualization
Oblique shocks
Radiative shocks
Strong explosions
Gravitational Collapse
Hayashi tracks
Non--homologous collapse
Self--similar collapse
Evolution of HII Regions
Ionization fronts
Expansion and evolution
Observations
Magnetohydrodynamics
The MHD approximation
MHD waves
Parker instability
Virial theorem
MHD shocks
Dynamos
D. Backer, 99S
In AY 201 we define the received radiative flux and intensity from a source and follow these to the emission region to determine first the 3D emissivity structure, and then the physical properties. In AY 203 the goal is to follow the radiation in the reverse direction - through the telescope optics and into the detector from which data is recorded for subsequent calibration, deconvolution of instrumental artifacts and analysis. A broad wavelength approach is taken which is appropriate to the range of facilities available to UCB scientists. The broad wavelength approach is also appropriate to many concepts that, while couched in different jargon across the spectrum, share many fundamental ideas. Examples are optics, solid state physics of pn junction, deconvolution.
The great breadth of this course will be complemented by depth as students ``adopt a wavelength band'' for assignments and presentations. In addition to lectures, reading assignments, oral & written reports and lab work, there will be field trips to nearby observatories and visits to campus labs. Students will work with real data and build models that simulate astronomical signals, noise and errors.
References: Lena, Observational Astrophysics
Extensive notes, reprints and texts in reading room
Organization & Cosmic Window & Pollution
Organization & Introdutory remarks
Cosmic window & Pollution
Volts & Counts & Statistics I
Probability, Random Variables & Stochastic Processes
Signal to Noise Ratio : from Waves (volts) to Photons (counts)
Telescope Optics
Geometrical Optics & Demonstrations
Physical Optics & Student Presentations
Receivers
Radio Telescopes, Feeds, Arrays
Heterodyne Receivers
Backends (IR)
Power Detectors, Correlators
AOS, Pulsar Processors
Array Detectors (IR/OPT)
CCD Arrays, Background
IR Arrays
Spectrometers (>= IR)
Introduction, filters, gratings
More gratings, optics
High Energy Systems
Detectors
Spectrometers; student presentations
Interferometry
Basics of interferometry
BIMA Array; VLA; VLBA
Array sensitivity; array simulation in MIRIAD (Lab)
Calibration, Absolute Standards & Astrometry/Geodesy/Time
Student reports
Image Processing
Deconvolution
Optical interferometry
Corrupted Visibility/Image Processing - I
Unstable visibility phase & self calibration
Unstable image
Corrupted Visibility/Image Processing - II
Speckle interferometry, Knox Thompson, Triple Product/Bispectrum
Proposals due; presentations
Concluding presentations and final remarks
J. Graham, 99S
References:
Spitzer, "Physical Processes in the Interstellar Medium"
Osterbrock
CNM/WNM
Jenkins, Jura, Loewenstein 1983, ApJ, 270, 88
Wolfire et al. 1995, 443, 152
WIM
Taylor and Cordes 1993, ApJ, 411, 674
Reynolds ApJ 1991, 372, L17
Heiles, Reach, & Koo 1996, ApJ, 466, 191
HIM
McKee and Ostriker 1977, ApJ, 218, 148
Magnetic Fields & Cosmic Rays
Boulares and Cox 1990
IS Abundances
Savage & Sembach 1996, ARAA, 34, 279
INTRODUCTION
RADIATIVE TRANSFER & GAS-DYNAMICS
GAS-DYNAMICS
PHOTOIONIZED GAS & HII REGIONS
Photoionization: Cross-sections
Radiative Recombination
Photoionization Equilibrium
Temperature of Photoionized Gas: Pure H Region; Cooling by Heavy Elements
Ionization Structure: Stromgren Sphere; Characteristics of HII Regions; Dust
Physical Conditions: Temperature & Density
Spectra; Inferring Densities from Forbidden Lines; Inferring Temperatures
Abundance & Abundance Gradients
Optical Lines; FIR Fine-structure Lines; Primordial He Abundance
Radio Emission from HII Regions: Continuum; Radio Recombination Lines
Stellar Associations
Dynamics of HII Regions (1952-63)
Ionization Fronts; Early Expnasion of HII Regions; Late Dynamics of HII
Regions;
Cloud Photoevaporation; GMC Destruction
THE WIM (1964-76)
Pulsar Dispersion Measure
Optical Emission Lines
Electron Density from Emission & Dispersion Measures; Temperature;
Ionization; Turbulence
Radio Recombination Lines & Free-Free Emission
Sources of Ionization of the WIM
Models for the WIM
Ionization of the Local ISM
Interstellar Scintillation
Rotation Measures - the WIM B-Field
INTERSTELLAR DUST
Optical Properties of Grains
Extinction in a Dusty Medium
Observations
Grain Temperature
Grain Size Distribution: Extinction; Dust Emission
Spatial Distribution of Dust
Formation and Destruction
Stellar & Interstellar Sources; Destruction in Interstellar Shocks
NEUTRAL ATOMIC GAS - THE WNM & CNM
Basics: Spin Temperature; Optical Depth
Evidence for a Two Phase Medium: Temperature of WNM & CNM
HI 21 cm EMISSION
Spatial Distribution of HI
Vertical Distribution; Radial Distribution; Morphology
ABSORPTION LINES of the WNM & CNM
Optical Absorption Lines
UV Absorption Lines
HI & H2; Pressure in the ISM; HST Observations of the CNM & WNM
TWO PHASE MODEL OF THE ISM
Cooling Processes
Heating Processes
Cosmic Rays; X-rays; Photoelectric Heating of Grains; Dissipation of
Mechanical Energy
THERMAL STABILITY
Isobaric Thermal Instability
Two-Phase Equilibrium
CORONAL GAS: Supernova remnants and the HIM
Energy Injection by Stars: Radiation; Mechanical Energy
Cooling Time for Hot Gas: Line Emission and Free-Free; Dust Cooling
CREATION/DESTRUCTION OF THE HIM
Thermal Conduction: Cloud Evaporation; Evaporative Cooling
BLAST WAVES AND SUPERNOVA REMNANT EVOLUTION
Equations of Motion
Sedov-Taylor Blast Wave; Radiative Blast Wave; Momentum Conserving
Snowplough;
Pressure Drive Snowplough; Adiabatic Bubble; Bubble with Radiative Shock
Free Expansion
Sedov-Taylor Expansion
Radiative Stage
Merger with ISM: Effects of Clouds
Stellar Wind Bubbles: Non-radiative Injection; Radiative bubbles
SUPERSHELLS & SUPERBUBBLES & THE THREE-PHASE MEDIUM
Supershells & Superbubbles
The Three Phase Model of the ISM
Filling Factor of Hot Gas; Energy Balance; Mass Balance;
Spectrum of Clouds with Ionized Edges
MOLECULAR GAS
Molecular Spectra: Energy Levels; H2; Dissociation of H2; CO
Polyatomic Molecules
Radiative Transfer: Line trapping; Large Velocity Approximation
CHEMISTRY
Types of Reaction
Gas-grain Chemistry; Ion-Molecule Reactions; Neutral-Neutral reactions;
Radiative Association; Dissociative Recombination
Formation of H2 on Grains
Ion-Molecule Chemistry
Photo-ionization Dominated Regions
Heating & Cooling in Molecular Gas
CO Cooling; Photoelectric Heating Dominated Cloud Envelopes
Photon Dominated Regions
Shocks in Molecular Gas: J Shocks & C Shocks
OBSERVATIONS OF GIANT MOLECULAR CLOUDS
Star Formation and GMCs
CO Surveys: Mass Spectrum
Larson's Laws
Molecular Structures
Galactic Distribution; Out Flow Sources; Hot Cores; Cloud Statistics;
Bipolar Outflows
MOLECULAR CLOUD STRUCTURE
Virial Theorem: Thermal Limit; Rotational Limit; Magnetic Limit
Support by Alfven Waves
STAR FORMATION
Spectra of Young Stellar Objects
Associations of YSO & Molecular Clouds
Infall & Outflows
Problems of Star Formation: Angular Momentum; Magnetic Flux
Subcritical vs. Supercritical Star Formation
Inside-out Collapse
Description: this reading course explores how physical conditions in
astrophysical objects can be diagnosed from their spectra. Using stars
as a relatively well-understood springboard, we discuss how energy flows
determine the thermal state of radiating objects (which are at opaque at
least at some wavelengths). Non-thermal processes (especially associated
with magnetic fields) can also have important effects. Since all we can
see is the radiation emitted, we also discuss the physics of radiative
transfer which leads to emergent spectral characteristics. These
fundamentals are then applied to the problem of understanding stellar
spectra, accretion disks in various contexts (particularly star formation
and AGN), and winds from stars, disks.
Material from the astrophysical literature will be used extensively, in
conjuction with some textbook material. Observational considerations
will be touched upon as they come up. This will be conducted as a reading
seminar (similar to a tutorial); lectures may occaisionally be given.
Syllabus Formation of the Continuum Plane-parallel, LTE, Static Radiative Transfer Radiative Equilibrium and Grey Atmospheres Opacities Spectral Energy Distributions of Stars Formation of Spectral Lines Statistical Equilibrium Line Opacities Line Profile Formation Stellar Spectral Types Thermal and Chemical Line Diagnostics Effect of velocity fields Line Blanketing NLTE effects Gravity and Magnetic Diagnostics Chromospheres and Heated Layers Line and Continuum formation in Disks Spectral Energy Distributions of Disks Thermal structure of disks and reprocessing T Tauri disks AGN disks Diagnostics of Winds and Outflows Coronal Winds Spherical Atmospheres Radiatively Driven Winds Winds and Jets in Star Formation --------------------------------- Reference Reading List Selected papers from astrophysical journals Radiative Transfer in Stellar Atmospheres (Rutten, online) The Physics of Astrophysics. I. Radiation (Shu) Stellar Atmospheres (Mihalas) Accretion Processes in Star Formation (Hartmann) The Observation and Analysis of Stellar Photospheres (Gray)
H. Spinrad
This course will survey the phenomenology of galaxies, including the Milky Way. There will be theoretical discussion of galactic structure, and a brief introduction to galactic dynamics and stability. The intent is to integrate the discussion of our galaxy in comparison with other galaxies, and to discuss the common questions of formation and evolution of galactic systems.
1. Some basics about our galaxy and its neighbors.
a) Stars near the sun.
b) Stellar populations in our galaxy and nearby systems.
c) Gas in galaxies, (and how to use it).
d) More sysnthesis of populations: metals, ages, and galactic
distributions...(Freeman Law).
2. Milky Way Kinematics.
a) Differential Rotation of the Galaxy.
b) Vertical Structure.
c) Oort Constants.
d) The Galactic Center..hot stuff!
3. Rotation Curves for other Spirals.
a) Spider diagrams.
b) Masses and mass decomposition. Dark matter vs visible matter.
4. Elliptical galaxies.
a) Photometry of Es.
b) Velocity dispersions and (some?) rotation.
c) Relaxation times.
d) Mass determinmmations.
5. More on Dark matter evidense in Milky Way and Spirals and E gals.
6. Extragalacic Star Formation (Morphological).
a) UV radiation from hot young stars. Calibration in terms of SFR.
b) The older populations; previous SF episodes and ancient history.
7. More on GAS (3 phases) and DUST in nearby galaxies.
a) IR explorations..pre SIRTF (just).
8. The Hubble Expansion and the velocity field nearby.
a) Determination of Ho; the extrgactic distance scale.
b) A smooth Hubble Flow??
c) Voids and density contrasts. Gas (abs) vs galaxies.
9. The Galaxian Luminosity Function.
a) Catalogues and the Field Population Lumin. function.
b) Clusters and their function. Schechter's fit.
10. The Physical situation in Rich Clusters.
a) Galaxies; their types in clusters.
b) X-ray gas, 1E x7 temp in rich clusters.
c) Cluster masses.
11. AGN.
a) History since 1963.
b) Physical situation in nuclei...SMBH likely.
c) Unifications and modeling.
d) AGN evolution? Probably so.
12. At the Limit. Star forming galaxies at large redshifts.
a) Ways to locate the rare and distant SF galaxies.
b) Modern results beyond z=5.
c) QSO's and the termination of the 'Dark Ages" (z>6).
13. Theory and observations of Galaxies "IN Formation".
M. Davis
This course will present an overview of current topics in physical cosmology, with an emphasis on structure formation on all scales. Topics for discussion include: the Robertson-Walker metric, Friedman solutions, measurement of cosmological parameters, the thermal history of the Universe, early universe physics, fluctuation generation and growth, microwave background radiation, dark matter, statistics of the galaxy distribution, gravitational lenses, linear and nonlinear evolution of structure, and the formation of galaxies.
Recommended texts:
"Galaxy Formation" M. Longair
"Structure Formation in the Universe", T. Padmanabhan
"Cosmological Physics" J. Peacock
SYLLABUS
Observational Background:
Galaxies
Groups and Clusters
Statistics of the Galaxy Distribution
CMBR, etc.
The Expanding Universe
Robertson-Walker Geometry
Classical Cosmological Measurement
Fluctuations in an Expanding Universe
The Cosmic Microwave Background
Blackbody Spectrum
Thermal History of the Universe
Primordial Nucleosynthesis
Early Universe
Inflation
Fluctuation Generation
Dark Matter, Hot and Cold
Tests of Cosmological Models:
Global measures of q_0, Lambda
Local Tests of Omega, e.g.
Virial arguments, X-ray gas, weak lensing
cosmic energy equation
velocity-gravity field comparisons
Galaxy Formation and clustering
Numerical methods:
Zeldovich Approximation
Formation of Caustics
N-body simulations
Hierarchical dark matter models
The Formation of Galaxies
Counts of galaxies, redshift distribution
Ly-break galaxies at z=3
Models of Galaxy Formation
Confrontation of LSS models with observations:
Anisotropy of the CMBR, large and intermediate scale
Bias in the Galaxy distribution
Power Spectrum of the galaxy distribution
The Normalization of the matter clustering amplitude
Gravitational Lenses as a Cosmological Tool
Fundamentals
Measurement of Cluster Potential Well Depth
Measurement of matter fluctuations
The Intergalactic Medium and Ly-alpha clouds
Thermal history of the IGM
I. dePater, 98F
Solar System research comprises many different areas of research, such as atmospheric science, geology, magnetospheric physics, comets, formation theories. An extensive outline of the various topics is listed below. Though we won't be able to cover all topics in detail, we will touch upon most of them, and cover some of them in detail. Extensive notes (or the book) will be available, as well as problem sets.
SYLLABUS: The wonders of our nearby Universe: the Solar System} General overview (general appearance of planets, sizes, distance to sun, terminology, history). Dynamics: basic laws of mechanics and some applications (Kepler's laws, tidal interactions, resonance interactions, ring dynamics); Solar radiation. Solar heating and energy transport Planetary atmospheres/ionospheres (observations, composition, line shapes, cloud physics, meteorology). Surfaces of planetary bodies (including impact processes, rocks/minerals, magmas). Planetary interiors (basic principle to deduce the structure of a planet's interior from the observed quantities; terrestrial and giant planets). Magnetospheres (basic ideas about particle motion in magnetic field, "origin" magnetic field, plasma sources, radio emissions). Meteorites Asteroids Comets Planetary Rings Formation Theory Extrasolar Planets
L. Bildsten, 98S
A one semester graduate course on stellar birth, life and death. Star formation by gravitational collapse of molecular clouds. Main sequence evolution of high and low mass stars. Thermonuclear processes and element formation. Stellar death via supernovae or planetary nebulae, leading to white dwarfs, neutron stars and black holes. Structure and emission properties of the isolated and cooling compact remnants. Additional topics include: stellar oscillations, binary evolution, stellar mass loss, and neutrino astrophysics.
You are also invited to attend the weekly "Brown Dwarfs and Giant Planets" seminar that I am running with Prof. Geoff Marcy. Some of this seminar's topics will overlap with this class, but not too much. Much of the seminar will go into more details about Jupiter size objects (both in our solar system and beyond) and brown dwarfs. Basically all of those objects that never burn their hydrogen.
Required texts:
"Stellar Interiors: Physical Principles, Structure and Evolution"
by C. J. Hansen and S. D. Kawaler
"Principles of Stellar Evolution and Nucleosynthesis" by D. Clayton
On reserve:
"Stellar Structure and Evolution" R. Kippenhahn & A. Weigert
"Frontiers of Stellar Evolution" D. L. Lambert
"Physics of Compact Objects" S. Shapiro & S. Teukolsky
Very useful:
Mihalas and Binney's "Galactic Astronomy"
two volume tome by Cox and Giuli on stellar structure
Schwarzschild's "Structure and Evolution of the Stars"
Syllabus
HYDROSTATICS AND THERMODYNAMICS OF SELF-GRAVITATING OBJECTS
(a) Hydrostatic equilibrium in spherical symmetry, Virial Theorem
(b) Equations of state (ideal gas, radiation pressure)
(c) Simple Stellar models and gravitational contraction.
(d) Importance of Radiation pressure.
(e) Diffusion of heat and stellar luminosities. Electrons vs. photons
STAR FORMATION
(a) Gravitational Collapse of Molecular Clouds
(b) Evolution of Protostars, Fully Convective Models. The Hayashi track.
LIFE ON THE MAIN SEQUENCE
(a) Thermonuclear energy generation - processes and rates.
(b) CNO vs pp burning, the Solar neutrino problem.
(c) Degeneracy and Brown Dwarf formation
(d) Stellar masses, temperature, radii and lifetimes. IMF.
(e) Convection: Where and why it occurs
(f) The Saha Equation, Simple atmospheres, Spectroscopy.
(g) Stellar Wind Theory
LIFE AFTER THE MAIN SEQUENCE
(a) Degeneracy during stellar evolution. Chandrasekhar Limit.
(b) Low Mass Stars: Red Giants, Mass Loss, Shell Burning
(c) Massive Stars: C/O Burning, Ne photodisintegration, neutrinos
(d) Collapse of Iron Cores: Type II Supernovae, nucleosynthesis.
COLLAPSED STARS-STRUCTURE AND EMISSION IN ISOLATION
(a) White dwarf Formation. Thermal Cooling and Observations
(b) Neutron star formation, structure and Cooling. The TOV equation.
(c) Black Holes. Formation and Observations
STELLAR PULSATIONS
(a) Equations for Radial and Non-Radial Pulsations
(b) Instability Mechanisms and the Cepheids
(c) Non-Radial Oscillations in the Sun, White Dwarfs and B-Stars
ROTATION AND MAGNETIC FIELDS (if time allows)
(a) Role and Evolution of rotation in stars.
(b) Magnetic braking on the lower mass main sequence.
(c) Rotation rates for the compact objects
(d) Magnetic field strengths and supposed causes on the MS.
L. Bildsten, 98F
This is a one semester lecture course on the broad field of High Energy Astrophysics. The highly recommended texts are ``Accretion Power in Astrophysics'' by J. Frank, A. King and D. Raine and Volumes 1 and 2 of ``High Energy Astrophysics'' by M. S. Longair. They should be available in the local bookstores.
The "bare minimum" prerequisites for this course are all of physics at the upper division undergraduate level. The more basic physics you have had at the graduate level, the easier the course will be for you. You can take this as a first year physics or astronomy graduate student, just be sure to talk to me if you feel the need to confirm that you have enough physics. Though helpful, no astronomy background is needed.
The following books are helpful to different degrees for this course:
"Principles of Stellar Evolution and Nucleosynthesis", D. Clayton,
"Stellar Structure and Evolution", R. Kippenhahn & A. Weigert,
"Stellar Interiors: Physical Principles, Structure and Evolution"
C. J. Hansen and S. D. Kawaler,
"Physics of Compact Objects", S. Shapiro & S. Teukolsky,
"Active Galactic Nuclei" by R. D. Blandford, H. Netzer & L. Woltjer,
"Interacting Binaries" by S. Shore, M. Livio and E. van den Heuvel.
SYLLABUS
THE SIMPLE PHYSICS OF ACCRETION DISKS
(a) The Bondi-Hoyle Accretion Rate, Energy Release
(b) Steady Spherically Symmetric Accretion and the Eddington Limit
(c) The role of angular momentum and need for a large viscosity
(d) The Shakura-Sunyaev $\alpha$-disk. Thermal Spectrum and Dependence on
central mass.
(e) Thick disks, quasi-spherical accretion, and inefficient emission.
(f) Recent application to our Galactic Center and other Black Holes
ACCRETION ONTO COMPACT OBJECTS IN BINARIES
(a) Review of Stellar Structure and Evolution in Binaries
(b) Conservative Mass Transfer and Effects on the Orbital
Elements. Evidence for orbital evolution.
(c) How Gravitational radiation, magnetic braking and
stellar evolution fix $\dot M$
(d) Unstable Mass transfer and Common Envelopes.
Origin of short-period Cataclsymic variables.
(e) The thermal instability of accretion disks, dwarf novae, X-ray transients
(f) Magnetic White Dwarfs: Hard X-ray emission, Comptonization
and cyclotron cooling.
(g) Accreting Neutron Stars: Why X-rays rather than Gamma-rays?
(h) Magnetic accretion onto neutron stars: X-ray pulsars, torques and
cyclotron lines
SUDDEN THERMONUCLEAR ENERGY RELEASE FROM ACCRETED MATTER
(a) Accretion onto White Dwarfs (WD) and Classical Novae:
Nucleosynthesis and mass ejection.
(b) Are the Super-Soft Sources from ROSAT steadily burning their accreting
fuel?
(c) What happens when a WD is pushed over the Chandrasekhar limit by
accretion?
(d) The Physics of Combustion Fronts. Deflagration versus
Detonation, Rayleigh-Taylor Instabilities
(e) Type Ia supernovae versus
Accretion-Induced Collapse to neutron stars
(f) Type I Bursts from Neutron Stars and Neutron Star Spin Measurements
NON-THERMAL EMISSION: SUPERNOVAE REMNANTS, COSMIC RAYS AND PULSARS
(a) Galactic Non-Thermal Radio emission: Synchotron radiation from
relativistic electrons.
(b) Polarization and the Galaxy's magnetic field.
(c) Gamma-ray Emission from the Galactic Plane.
(d) Cosmic Ray Acceleration and Evolution in the Galaxy
(e) Supernovae Remnants and the Need for Energy Injection in Plerions
(f) Simple Aspects of Tapping Rotation and Inferences on NS Magnetic Fields
(g) "Magnetars" as Soft-Gamma Repeaters and recent progress
on $B\sim 10^{14} \ {\rm G}$ neutron stars.
RELATIVISTIC JETS AND GAMMA-RAY BURSTS
(a) Theory and observations of Radio sources and "superluminal" motion.
Radio lobes
(b) Blazars from EGRET: beamed jets and models for the
gamma-ray emission. High energy neutrinos?
(c) What is the energy source? Blandford-Znajek ?
(d) Overview of Gamma-Ray Bursts: Spectra, Durations and Repetition?
(e) Statistical Motivation for Cosmological GRB Origin and Coalescing NS/NS
Binaries.
(f) Simple Fireball Models and Repercussion for Optical/ X-Ray Afterglows.
(g) Gravitational Wave detection of NS/NS binaries with LIGO.
BLACK HOLES IN GALACTIC CENTERS: ACTIVE GALACTIC NUCLEI
(a) The Phenomena of Active Galactic Nuclei. The Center of Our galaxy
(b) Simple Application of an accretion disk and the big blue bump.
(c) The observed non-thermal emission as shown by X/Gamma-rays.
Hot Coronae and Comptonization
(d) What is the source of material for the AGN? Bar
dynamics? Interactions?
R. Klein, 99S
This new course will present a broad survey of state-of-the-art approaches to astrophysical self-gravitational gas dynamics with application to modern simulation of coupled non-linear astrophysical flows and their solutions on supercomputers. We will begin with the development of the fundamental concepts underlying finite-difference approaches for Lagangian and Eulerian astrophysical hydrodynamics. We will develop a unified approach to the coupling of radiation with hydrodynamics. The lectures will examine currently favored N-body gravitational techniques including direct N-body, P-M and P3M formulations as well as hierarchical Tree-approaches. Standard particle gas dynamic methods such as Smooth Particle Hydrodynamics (SPH) as well as recent developments with Adaptive SPH will be discussed and contrasted with finite difference approaches. Methods unifying SPH and Tree hierarchies (TREE-SPH) and their application to cosmological simulation will be examined. More advanced techniques such as higher order finite difference hydrodynamics with Adaptive Mesh Refinement (AMR) will be presented.
Applications of these approaches in three broad areas will be presented: Cosmology, including cluster, galaxy and large scale structure formation; High Energy Astrophysics including accretion onto compact objects with application to the recent RXTE discovery of fast time variability in neutron stars and their interpretation as photon bubbles, and the Interstellar Medium including the interaction of supernova shocks with interstellar clouds, collisions of interstellar clouds and supernova explosions and related hydrodynamic instabilities.
The course will stress an active participation of students in projects involving the application of the simulation methods to solving contemporary astrophysics gas dynamic problems on the computer. This course is extremely useful for developing essential numerical simulation techniques for a wide range of modern theoretical astrophysics.
Syllabus
I. Basic Concepts of Finite Difference Solutions of Partial Differential
Equations in Astrophysics
A. Finite difference techniques; Taylor series expansions, integral methods,
control
volume approach.
B. Fundamentals of convergence, stability, consistency and accuracy.
C. Basic finite difference schemes.
D. Stability analysis of finite difference schemes; Von Neumann stability
analysis.
II. Hydrodynamics of Compressible Flows
A. Eulerian, Lagrangian formulations with shocks.
B. Finite difference methods for compressible flows; Richtmyer-Von Neumann
difference equations, concept of artificial viscosity and effect on
solutions,
conservation forms; Eulerian formulation.
C. Numerical solutions for 1-D compressible flows; strong shock problems,
spherical blast waves, supernova evolution, Sedov similarity solutions.
III. Radiation-Hydrodynamics for Astrophysical Flows
A. Computational methods for solution of the radiative transfer equation.
B. Combined moment approach and flux limitiing.
C. Multi-Frequency Grey transport techniques in radiation-hydrodynamics.
IV. N-Body Techniques in Multi-Dimensional Hydrodynamics
A. General survey of different methods.
B. Analytic methods; Green's function approaches.
C. Finite difference algorithms.
D. Direct N-body summation.
E. Fast Fourier transform (FFT) methods.
F. Cyclic Reduction and FACR approach.
G. Particle Mesh scheme (PM).
H. Particle-Particle-Particle--Mesh (P3M) scheme.
I. Integration of equations of motion of particles in expanding universe.
J. Hierarchical P-M.
V. N-Body Techniques: Gridless Schemes
A. Tree hierarchical structures and Tree codes.
B. Basis function expansions; spherical harmonic expansions,
self-consistent field methods.
VI. Smooth Particle Hydrodynamics
A. Standard SPH.
B. Adaptive SPH.
VII. Unified Particle-Hydrodynamic Schemes
A. TREE + SPH (TREESPH).
B. P3M + SPH (P3MSPH).
VIII. Advanced Methods in Multi-Dimensional Hydrodynamics
A. Adaptive Mesh Refinement (AMR) with Godunov hydrodynamics.
IX. Applications
A. Cosmology; large scale structure, gravitational evolution of cluster
formation.
B. Interstellar Medium; supernova shock-cloud interactions, cloud-cloud
collisions,
induced star formation, supernova explosions.
C. Star Formation; gravitational collapse and fragmentation of molecular
clouds,
formation of binaries and multiple stars.
D. High Energy Astrophysics; prompt emission from supernovae, dynamics of
accretion onto neutron stars, formation of photon bubbles, radiation-
hydrodynamics of winds and coronae of accretion disks.