• Discussion of approach to the course
• Basic hydrostatic balance in stars is gravity vs pressure gradient, with required high central pressure achieved with high temperature
• Since nuclear burning rates are very temperature sensitive, higher mass implies much higher luminosity, going from p-p chain to C-N-O cycle
• Examine origin of OBAFGKM spectral sequence, and nature of H-R diagram
• Reviewed stages in evolution of one-solar-mass star, from main sequence (H core burning), to red giant (H shell burning, inert core), to horizontal branch (He core burning), to supergiant (both H and H shell burning). More to follow ...

Lecture 2: Whirlwind stellar evolution Part II (Juri Toomre) (Thur, 24 Jan 13)

• Blowing off outer shell as "planetary nebula", on the way to becoming white dwarf
• White dwarf properties, and its boring fate if alone -- but if in binary, mass exchange could lead to much more interesting things
• Evolution story, including "layers of onions", for massive stars
• Massive stars' final fates strongly influence by how much mass lost along the way
• Core collapse supernovae may leave behind neutron star, a black hole, or possibly nothing
• White dwarfs and neutron stars typically possess extremely strong magnetic fields

Lecture 3: Structure and dynamics of solar interior (Mark Miesch) (Tues, 29 Jan 13)

• What controls the basic structure and dynamics of solar and stellar interiors
• Energy source for convection and magnetic dynamo action is ultimately nuclear burning
• There is much nitty gritty (and complexity) in understanding the conservation of energy equation involving the radiative and convective heat fluxes
• Properties of convection and the crucial role of boundary layers
• Effects of rotation and magnetism on general structure of convection

Lecture 4: The many scales in space and time of solar convection (Mark Miesch) (Thur, 31 Jan 13)

• Solar convection exhibits many of the fundamental physics discussed in last lecture...and more
• It is stratified, rotating, magnetized, and strongly driven from the top (photosphere) by efficient radiative cooling
• This gives rise to a hierarchy of convective size and length scales, increasing as you go deeper
• The largest scales (giant cells) must be influenced by rotation and must give rise to the prominent differential rotation (DR) seen in surface measurements and helioseismic inversions -- discuss DR in next lecture

Lecture 5: Solar differential rotation and meridional circulations (Mark Miesch) (Tues, 5 Feb 13)

• Sun's differential rotation at surface, with fast equator and slow poles, has long been known, and has changed little from Carrington's time in 1860's
• Helioseismology has revealed interior behavior of angular velocity of rotation with radius and latitude, confirming the nearly 30% latitudinal contrast
• Two boundary layers evident in angular velocity: near-surface shear layer of speed up with depth in first 35 Mm, and a tacholine of shear at the base of convection zone leading to uniform rotation in deeper radiative interior
• Meridional flows are mainly poleward at surface in both hemisphere, but modest in amplitude
• Detailed discussion of balances involved to understand these mean flows, with Reynolds stresses of convection and baroclinity having key roles
• `Gyroscopic pumping' helps to interpret the meridional flows

Lecture 6: Elements of the solar dynamo (Mark Miesch) (Thur, 7 Feb 13)

• General properties of the solar 11-year magnetic reversals
• Convection breeds magnetism in many stars
• MHD magnetic induction equation and its consequences
• Implications of Lagrangian chaos in kinematic dynamos
• Differences between small-scale and large-scale dynamos
• Inverse cascades of magnetic helicity crucial to building global magnetic field
• Essentials of the alpha-effect and the omega-effect in dynamo action
• Rotation promotes magnetic self-organization

Lecture 7: Magnetohydrodynamics (MHD) -- formulating the equations (Juri Toomre/Brad Hindman) (Tues, 12 Feb 13)

• Assumptions of MHD: large spatial and temporal scales allow continuum treatment
• The basic equations in overview, then start taking them apart
• Magnetic induction equation and role of magnetic diffusivity
• High magnetic Reynolds number Rm: "ideal MHD limit", while low Rm, diffusive limit
• Analogy between vorticity equation and induction equation: magnetic field lines and vortex lines move with fluid if diffusion small
• Hannes Alfven: Flux freezing in ideal MHD limit

Lecture 8: Further elements of MHD (Juri Toomre/Brad Hindman) (Thur, 14 Feb 13)

• Brief review of prior MHD equation set and properties
• Lorentz force in momentum equation
• Magnetic tension and pressure
• Parallel-transverse decomposition of magnetic tension
• Magnetic pressure yields magnetic evacuation and buoyancy
• Reduced gas pressure and density in flux tubes -- light fibers
• Magnetic energy equation and Poynting flux
• Recap of MHD

Lecture 9: Dynamo theory, Part I (Matthias Rempel) (Tues, 19 Feb 13)

• Overview: magnetic fields in the universe
• Ohm's law and induction equation
• General definition of dynamo, and of small-scale / large-scale dynamos
• Small-scale dynamo action in the solar photosphere

Lecture 10: Dynamo theory, Part II (Matthias Rempel) (Thur, 21 Feb 13)

• Definition of dynamo
• Anti-dynamo theorems
• Induction by differential rotation and meridional flow
• Meanfield electrodynamics

Lecture 11: Dynamo theory, Part III (Matthias Rempel) (Tues, 26 Feb 13)

• Physical interpretation of turbulent induction effects
• How to make a large scale dynamo?
• General properties of mean field dynamos
• Dynamos and magnetic helicity
• Nonlinear feedback, quenching of alpha-effect

Lecture 12: Elements of the solar dynamo (Matthias Rempel) (Thur, 28 Feb 13)

• Key solar observations of magnetism
• Overview of mean-field and 3-D dynamo models
• Discussion of uncertainties in models
• Flux emergence and sunspot formation

Lecture 13: Intro solar radiative transfer, Part I. Basic RT (Han Uitenbroek) (Tues, 5 Mar 13)

• Intensity, emission, absorption
• Source function
• Optical depth
• Transfer equation
• Line formation

Lecture 14: Solar RT, Part II. Detailed radiative processes (Han Uitenbroek) (Thur, 7 Mar 13)

• Spectral lines
• Radiative transitions
• Collisions
• Polarization
• Non-LTE radiative transfer

Lecture 15: Solar RT, Part III. Solar observations of magnetism (Han Uitenbroek) (Tues, 12 Mar 13)

• Solar telescopes and their design issues
• Spectroscopy and its instruments
• Adaptive optics and its magic
• Polarimetry and Stokes subtleties in measuring vector magnetic fields

Lecture 16: Solar atmosphere, Part I. Magnetic energy storage (Sarah Gibson) (Thur, 14 Mar 13)

• Solar corona and how observed
• Coronal heating and solar wind acceleration
• Coronal magnetism, force free fields, magnetic helicity
• How to measure magnetic twist
• First look at coronal prominence cavities and flux ropes

Lecture 17: Solar atmosphere, Part II. Coronal magnetic cavities and flux ropes (Sarah Gibson) (Tues, 19 Mar 13)

• Examples of sigmoids, prominences and cavities from your "homework"
• Cavity like a croissant: expanded twisted flux
• Cavity density and substructure: reconnection and gravity both matter
• Cavities are multi-thermal and dynamic: field aligned flows
• Linear polarization images suggest "lagomorphs", or bunnies!

Lecture 18: Solar atmosphere, Part III. Magnetic energy release and eruptions (Sarah Gibson) (Thur, 21 Mar 13)

• Examples of various CMEs in the heliosphere
• Thresholds for magnetic energy and helicity that lead to instability
• Magnetic topologies leading to eruptions
• Importance of magnetic reconnection
• Reconnections in kink instability-driven partial eruptions
• End state: tethered spheromak
• Cavity clues to CMEs: teardrop shape and height

Lecture 19: Observations of stellar magnetism (Ben Brown) (Tues, 2 Apr 13)

• Signatures of magnetic activity in stars: coronal x-ray emission, chromospheric calcium H & K
• Connecting x-ray emission to photospheric magnetic flux
• Star spots deduced from photometric light curves
• Large-scale magnetic topology from Zeeman and spectropolarimetry
• Detection of magnetic cycles in other stars

Lecture 20: Stellar convective dynamo simulations (Ben Brown) (Thur, 4 Apr 13)

• Small stars (M-dwarf) can have very big flares, making life nearby interesting
• 3-D simulations of convection and dynamos are now tractable across the main sequence
• Models of solar-like stars with differential rotation can build organized magnetic fields that reverse in polarity
• These fields can have wreath-like structures that fill the convective envelope
• The wreaths can be achieved even without tachoclines of shear

Lecture 21: Helioseismology overview (Brad Hindman) (Tues, 9 Apr 13)

• Observations of the sun's acoustic oscillations
• The Sun's resonant acoustic and gravity waves and their properties
• Granulation is the source of acoustic energy
• Eigenfunctions for acoustic and gravity waves
• Where have all the gravity modes gone?

Lecture 22: Acoustic-gravity waves in the Sun (Brad Hindman) (Thur, 11 Apr 13)

• What are the important restoring forces?
• Acoustic waves and gravity waves in isolation
• The wave equation for acoustic-gravity waves
• Properties of the local dispersion relationship
• Wave cavities and propagation diagrams

Lecture 23: Helioseismic inversions (Brad Hindman) (Tues, 16 Apr 13)

• Propagation and evanescence
• Wave cavities and propagation diagrams
• What is the information content of a mode frequency?
• Sensitivity kernels
• Using RLS inversion to obtain the physical properties of a star from measured mode frequencies

Lecture 24: Helioseismic discoveries (Brad Hindman) (Thur, 18 Apr 13)

• Results from global helioseismology: sound speed and rotation rate inversions
• What is local helioseismology?
• How does ring analysis work?
• Meridional flows obtained with ring analysis
• The flows that form around magnetic active regions
• Imaging sunspots before they emerge
• Imaging active regions on the farside of the sun

Lecture 25: MHD waves (Brad Hindman) (Tues, 23 Apr 13)

• Scattering and absorption of waves by sunspots
• Derivation of the MHD wave modes: Alfven wave, fast and slow magnetosonic waves
• Properties of the Alfven wave
• Properties of magnetosonic waves
• Restoring forces for each wave mode

Lecture 26: MHD waves in a stratified atmosphere (Brad Hindman) (Thur, 25 Apr 13)

• Acoustic holography measurements of absorption by sunspots
• Derivation of coupled wave equations describing the fast and slow mode for a simple atmosphere
• Alfven waves decouple if the atmosphere is horizontally homogenous
• Vertical stratification leads to coupled fast and slow modes
• Asymptotic decoupling high and low in the atmosphere
• Mode conversion

Lecture 27: Participant presentations (Juri Toomre/Andrew Gerrard) (Tues, 30 Apr 13)

• Kate Goodrich: Magnetic flux tubes in dynamo models
• Courtney Peck: Solar dynamo models: Incorporating meridional flows and physical constraints
• Andrew Sturner: Intermittency and grand minima
• Anthony Teti: Solar adaptive optics
• Dhvanit Mehta: Tachocline and internal waves

Lecture 28: Participant presentations (Juri Toomre/Andrew Gerrard) (Thur, 2 May 13)

• Chris Moore: Solar-stellar flare connection
• Kevin Urban: Secrets of the solar wind (MHD turbulence)
• Paul Dupiano: Questions for solar dynamo models (role of meridional flow)
• James LeMaire Jr: Flux tube models
• Natsuha Kuroda: Solar observations in 10.7 cm wavelength

Lecture 29: Participant presentations (Juri Toomre/Andrew Gerrard) (Tues, 7 May 13)

• Xin Chen: Solar dynamo -- 3-D numerical simulations
• Zhicheng Zeng: Probing mean-field models including meridional circulation
• Shaheda (Begum) Shaik: The Sun and the models
• Zhitao Wang: Flux-transport model of solar cycles