Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Input for Phil’s SOHO-17 talk...

Slides:



Advertisements
Similar presentations
Ion Heating in the Solar Corona Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Advertisements

Chapter 8 The Sun – Our Star.
Plasmas in Space: From the Surface of the Sun to the Orbit of the Earth Steven R. Spangler, University of Iowa Division of Plasma Physics, American Physical.
The Solar Corona and Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Understanding the Origins of the Solar WindS. R. Cranmer, SHINE, Maui, June 28, 2012 Understanding the Origins of the Solar Wind Steven R. Cranmer Harvard-Smithsonian.
Reviewing the Summer School Solar Labs Nicholas Gross.
“The Role of Atomic Physics in Spectroscopic Studies of the Extended Solar Corona” – John Kohl “High Accuracy Atomic Physics in Astronomy”, August.
Progress Report: Testing the S-Web Idea with “Time-Steady” Turbulence Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Turbulence and Wave Dissipation in the Chromosphere, Corona, and Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
1 The search for signatures of ion cyclotron resonance in the low corona Laurent Dolla Jacques Solomon Philippe Lemaire Institut d'Astrophysique Spatiale.
Alfvén-cyclotron wave mode structure: linear and nonlinear behavior J. A. Araneda 1, H. Astudillo 1, and E. Marsch 2 1 Departamento de Física, Universidad.
Nanoflares and MHD turbulence in Coronal Loop: a Hybrid Shell Model Giuseppina Nigro, F.Malara, V.Carbone, P.Veltri Dipartimento di Fisica Università della.
Turbulent Heating of Protons, Electrons, & Heavy Ions in the Tangled & Twisted Solar Corona Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Telescoping in on the Microscopic Origins of the Fast Solar Wind Steven R. Cranmer & Adriaan van Ballegooijen Harvard-Smithsonian Center for Astrophysics.
Tools for Predicting the Rates of Turbulent Heating for Protons, Electrons, & Heavy Ions in the Solar Wind S. R. Cranmer 1, B. D. G. Chandran 2, and A.
Turbulent Origins of the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Capabilities of UV Coronagraphic Spectroscopy for Studying the Source Regions of SEPs & the Solar Wind John Kohl, Steven Cranmer, Larry Gardner, Jun Lin,
Exploring the Solar Wind with Ultraviolet Light Steven R. Cranmer and the UVCS/SOHO Team Harvard-Smithsonian Center for Astrophysics.
A Summary of the Evidence in Favor of the Idea that the Solar Wind is Accelerated by Waves and/or Turbulence S. R. Cranmer 1 & B. D. G. Chandran 2 1 Harvard-Smithsonian.
The SPP Theory & Modeling Team: Exploring Predictions & Controversies Steven R. Cranmer Harvard-Smithsonian CfA.
Feb. 2006HMI/AIA Science Team Mtg.1 Heating the Corona and Driving the Solar Wind A. A. van Ballegooijen Smithsonian Astrophysical Observatory Cambridge,
Turbulence in the Solar Corona Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
1 The Connection between Alfvénic Turbulence and the FIP Effect Martin Laming, Naval Research Laboratory, Washington DC
Why does the temperature of the Sun’s atmosphere increase with height? Evidence strongly suggests that magnetic waves carry energy into the chromosphere.
Spectroscopic Diagnostics of Solar Wind, CME, and SEP Source Regions Imaging Workshop, NSSTC, Huntsville, AL, 9-10 November 2004 Spectroscopic Diagnostics.
Incorporating Kinetic Effects into Global Models of the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Ion Heating in the Solar Corona & Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Solar Wind Origin & Heating 2 Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Non-collisional ion heating and Magnetic Turbulence in MST Abdulgader Almagri On behalf of MST Team RFP Workshop Padova, Italy April 2010.
Waves, structures and turbulences Fluctuations: scales and parameters Magnetohydrodynamic waves Structures and Alfvénic fluctuations Turbulence spectra.
Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Amanda Persichetti Aad.
The Sun and the Heliosphere: some basic concepts…
1 Mirror Mode Storms in Solar Wind and ULF Waves in the Solar Wind C.T. Russell, L.K. Jian, X. Blanco-Cano and J.G. Luhmann 18 th STEREO Science Working.
Applications of MHD Turbulence to Modeling Solar (and Stellar) Coronal Heating and Winds Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
R. Oran csem.engin.umich.edu SHINE 09 May 2005 Campaign Event: Introducing Turbulence Rona Oran Igor V. Sokolov Richard Frazin Ward Manchester Tamas I.
Probing Coronal Magnetism with Multi-wavelength Polarimetry Silvano Fineschi INAF-Torino Astrophysical Observatory, Italy 25 May, 2013, Bern (CH)
The energetics of the slow solar wind Leon Ofman, Catholic University of America, NASA GSFC, Code 612.1, Greenbelt, MD 20771, USA
Large-Amplitude Electric Fields Associated with Bursty Bulk Flow Braking in the Earth’s Plasma Sheet R. E. Ergun et al., JGR (2014) Speaker: Zhao Duo.
MHD Turbulence driven by low frequency waves and reflection from inhomogeneities: Theory, simulation and application to coronal heating W H Matthaeus Bartol.
Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,
Voyager 2 Observations of Magnetic Waves due to Interstellar Pickup Ions Colin J. Joyce Charles W. Smith, Phillip A. Isenberg, Nathan A. Schwadron, Neil.
Solar Wind Turbulent Dissipation: A Collisionless Zoo Steven R. Cranmer University of Colorado Boulder, LASP A. van Ballegooijen, L. Woolsey, J. Kohl,
Mass loss and Alfvén waves in cool supergiant stars Aline A. Vidotto & Vera Jatenco-Pereira Universidade de São Paulo Instituto de Astronomia, Geofísica.
Alfvénic Turbulence in the Fast Solar Wind: from cradle to grave S. R. Cranmer, A. A. van Ballegooijen, and the UVCS/SOHO Team Harvard-Smithsonian Center.
1 SPD Meeting, July 8, 2013 Coronal Mass Ejection Plasma Heating by Alfvén Wave Dissipation Rebekah M. Evans 1,2, Merav Opher 3, and Bart van der Holst.
Quelques développements récents sur la physique
Solar Wind Origin & Heating 1
Applications of MHD Turbulence: from SUMER to Ulysses! Steven R. Cranmer, Harvard-Smithsonian CfA Polar coronal hole protons electrons O +5 O +6.
Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics
-1- Solar wind turbulence from radio occultation data Chashei, I.V. Lebedev Physical Institute, Moscow, Russia Efimov, A.I., Institute of Radio Engineering.
A shock is a discontinuity separating two different regimes in a continuous media. –Shocks form when velocities exceed the signal speed in the medium.
Stuart D. BaleFIELDS SOC CDR – Science Requirements Solar Probe Plus FIELDS SOC CDR Science and Instrument Overview Science Requirements Stuart D. Bale.
Shock heating by Fast/Slow MHD waves along plasma loops
Coronal Heating due to low frequency wave-driven turbulence W H Matthaeus Bartol Research Institute, University of Delaware Collaborators: P. Dmitruk,
Turbulence and Waves as Sources for the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Turbulence in the Solar Wind
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetic Structure Feb. 16, 2012.
Modeling the Solar Wind: A survey of theoretical ideas for the origins of fast & slow streams Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.
Turbulent Origins of the Sun’s Corona & Solar Wind S. R. Cranmer, 12 March 2010, London Turbulent Origins of the Sun’s Hot Corona and the Solar Wind Steven.
A Global Hybrid Simulation Study of the Solar Wind Interaction with the Moon David Schriver ESS 265 – June 2, 2005.
How is the Corona Heated? (Waves vs. Reconnection) A. A. van Ballegooijen, S. R. Cranmer, and the UVCS/SOHO Team Harvard-Smithsonian Center for Astrophysics.
An overview of turbulent transport in tokamaks
Why is the “fast solar wind” fast and the “slow solar wind” slow
Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics
2005 Joint SPD/AGU Assembly, SP33A–02
Progress Toward Measurements of Suprathermal Proton Seed Particle Populations J. Raymond, J. Kohl, A. Panasyuk, L. Gardner, and S. Cranmer Harvard-Smithsonian.
How does the solar atmosphere connect to the inner heliosphere?
ESS 154/200C Lecture 19 Waves in Plasmas 2
Introduction to Space Weather
In situ particle detection
Presentation transcript:

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Input for Phil’s SOHO-17 talk...

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily UVCS / SOHO 1979–1995: Rocket flights and Shuttle-deployed Spartan 201 laid groundwork. 1996–present: Solar and Heliospheric Observatory (SOHO), with 12 instruments probing solar interior to outer heliosphere. The Ultraviolet Coronagraph Spectrometer (UVCS) measures plasma properties of coronal protons, ions, and electrons between 1.5 and 10 solar radii. slit field of view: Mirror motions select height Instrument rolls indep. of spacecraft 2 UV channels: LYA & OVI 1 white-light polarimetry channel

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Coronal holes: the impact of UVCS UVCS/SOHO has led to new views of the acceleration regions of the solar wind. Key results include: The fast solar wind becomes supersonic much closer to the Sun (~2 R s ) than previously believed. In coronal holes, heavy ions (e.g., O +5 ) both flow faster and are heated hundreds of times more strongly than protons and electrons, and have anisotropic temperatures. (e.g., Kohl et al. 1997,1998)

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Coronal holes: over the solar cycle Even though large coronal holes have similar outflow speeds at 1 AU (>600 km/s), their acceleration (in O +5 ) in the corona is different! (Miralles et al. 2001) Solar minimum: Solar maximum:

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Ion cyclotron waves in the corona? UVCS observations have rekindled theoretical efforts to understand heating and acceleration of the plasma in the (collisionless?) acceleration region of the wind. Alfven wave’s oscillating E and B fields ion’s Larmor motion around radial B-field Ion cyclotron waves (10 to 10,000 Hz) suggested as a natural energy source that can be tapped to preferentially heat & accelerate heavy ions. Dissipation of these waves produces diffusion in velocity space along contours of ~constant energy in the frame moving with wave phase speed:

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily But where do ion cyclotron waves come from? Alfven waves with frequencies > 10 Hz have not yet been observed in the corona or solar wind, but ideas for their origin abound.... (1) Base generation by, e.g., “microflare” reconnection in the lanes that border convection cells (e.g., Axford & McKenzie 1997). Problem: low Z/A ions consume base-generated wave energy before it can be absorbed by, e.g., O +5, He +2, p + (Cranmer 2000, 2001; Tu & Marsch 2001) (2) Secondary generation: low-frequency Alfven waves may be converted into cyclotron waves gradually in the corona. Problem: Turbulence produces mainly high-kperp fluctuations (which still have low freq’s). Instabilities require stronger nonlinearity than may exist for low- freq Alfven waves.

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily MHD turbulence It is highly likely that somewhere in the outer solar atmosphere the fluctuations become turbulent and cascade from large to small scales: With a strong background field, it is easier to mix field lines (perp. to B) than it is to bend them (parallel to B). Also, the energy transport along the field is far from isotropic: Z+Z+ Z–Z– Z–Z– (e.g., Dmitruk et al. 2002)

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily An Alfvén wave heating model Cranmer & van Ballegooijen (2005) built a model of the global properties of non- WKB (low-frequency!) Alfvenic turbulence along an open flux tube. Background plasma properties (density, flow speed, B-field strength) are fixed empirically; wave properties are modeled with virtually no “free” parameters. Lower boundary condition: observed horizontal motions of G-band bright points.

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Resulting wave amplitude (with damping) Transport equations solved for 300 “monochromatic” periods (3 sec to 3 days), then renormalized using photospheric power spectrum. One free parameter: base “jump amplitude” (0 to 5 km/s allowed; 3 km/s is best)

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Turbulent heating rate Anisotropic heating and damping was applied to the model; L = 1100 km at the merging height; scales with transverse flux-tube dimension. The isotropic Kolmogorov law overestimates the heating in regions where Z – >> Z + Dmitruk et al. (2002) predicted that this anisotropic heating may account for much of the expected (i.e., empirically constrained) coronal heating in open magnetic regions...

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Anisotropic MHD cascade Can MHD turbulence generate ion cyclotron waves? Many models say no! Simulations & analytic models predict cascade from small to large k,leaving k ~unchanged. “Kinetic Alfven waves” with large k do not necessarily have high frequencies. In a low-beta plasma, KAWs are Landau-damped, heating electrons preferentially! Cranmer & van Ballegooijen (2003) modeled the anisotropic cascade with advection & diffusion in k-space and found some k “leakage”... probably not enough!

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily But does turbulence generate cyclotron waves? Impulsive plasma micro-instabilities that locally generate high-freq. waves (Markovskii 2004)? Non-linear/non-adiabatic KAW-particle effects (Voitenko & Goossens 2004)? Larmor “spinup” in dissipation-scale current sheets (Dmitruk et al. 2004)? KAW damping leads to electron beams, further (Langmuir) turbulence, and Debye- scale electron phase space holes, which heat ions perpendicularly via “collisions” (Ergun et al. 1999; Cranmer & van Ballegooijen 2003)? How then are the ions heated & accelerated? Preliminary models say “probably not” in the extended corona. (At least not in a straightforward way!) freq. horiz. wavenumber MHD turbulence cyclotron resonance- like phenomena something else?

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Two recent possibilities for “something else!” Markovskii et al. (2006): high k_perp turbulence generates strong horizontal shears that are unstable to generation of ion cyclotron waves. (May also explain in-situ steepening of frequency spectra.) Chandran (2006): nonlinear couplings between Alfven and Fast-mode waves. Fast waves cascade ~isotropically in k- space) and can “feed” into Alfven wave power at high k_parallel (high frequency).

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily The Need for Better Observations Even though UVCS/SOHO has made significant advances, We still do not understand the physical processes that heat and accelerate the entire plasma (protons, electrons, heavy ions), There is still controversy about whether the fast solar wind occurs primarily in dense polar plumes or in low-density inter-plume plasma, We still do not know how & where the various components of the variable slow solar wind are produced (e.g. “LASCO blobs”). (Our understanding of ion cyclotron resonance is based essentially on just one ion!) UVCS has shown that answering these questions is possible, but cannot make the required observations...

Title of talk SOHO-17: 10 Years of SOHO and Beyond 7-12 May 2006, Giardini Naxos, Sicily Future Diagnostics: more ions Observing emission lines of additional ions (i.e., more charge & mass combinations) in the acceleration region of the solar wind would constrain the specific kinds of waves and the specific collisionless damping modes. Example prediction of “new” ion line widths (Cranmer 2002, astro-ph/ )