The SPP Theory & Modeling Team: Exploring Predictions & Controversies Steven R. Cranmer Harvard-Smithsonian CfA.

Slides:

Advertisements

Similar presentations

SOLAR WIND TURBULENCE; WAVE DISSIPATION AT ELECTRON SCALE WAVELENGTHS S. Peter Gary Space Science Institute Boulder, CO Meeting on Solar Wind Turbulence.

Advertisements

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.

Low-Frequency Waves Excited by Newborn Interstellar Pickup Ions H + and He + at 4.5 AU Charles W. Smith, Colin J. Joyce, Philip A. Isenberg, Neil Murphy,

Progress Report: Testing the S-Web Idea with “Time-Steady” Turbulence Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

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.

Turbulent Origins of the Sun’s Corona & Solar WindS. R. Cranmer, September 22, 2011, B.U. CSP Turbulent Origins of the Sun’s Hot Corona and the Solar Wind.

Connections Between the Magnetic Carpet and the Unbalanced Corona: New Monte Carlo Models Steven R. Cranmer & Adriaan van Ballegooijen Harvard-Smithsonian.

Solar Flare Particle Heating via low-beta Reconnection Dietmar Krauss-Varban & Brian T. Welsch Space Sciences Laboratory UC Berkeley Reconnection Workshop.

Testing Models of CTTS Coronal Heating, X-Ray Emission, & WindsS. R. Cranmer, July 14, 2010 Testing Models of Coronal Heating, X-Ray Emission, and Winds...

Self Consistent Solar Wind ModelsS. R. Cranmer, 25 January 2010, ISSI, Bern, Switzerland Self Consistent Solar Wind Models Steven R. Cranmer Harvard-Smithsonian.

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.

Testing and Refining Models of Slow Solar Wind Acceleration Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

Winds of cool supergiant stars driven by Alfvén waves

Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics

Turbulent Origins of the Sun’s Corona & Solar WindS. R. Cranmer, February 21, 2011, U. Iowa Turbulent Origins of the Sun’s Hot Corona and the Solar Wind.

Feb. 2006HMI/AIA Science Team Mtg.1 Heating the Corona and Driving the Solar Wind A. A. van Ballegooijen Smithsonian Astrophysical Observatory Cambridge,

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...

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.

MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric Model.

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.

Turbulence as a Unifying Principle in Coronal Heating and Solar Wind Acceleration Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics A. van.

Stuart D. BaleFIELDS iCDR – Science Requirements Solar Probe Plus FIELDS Instrument CDR Science and Instrument Overview Science Requirements Stuart D.

Two-dimensional hybrid modeling of wave heating in the solar wind plasma L. Ofman 1, and A.F. Viñas 2 1 Department of Physics, Catholic University of America,

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.

ABSTRACT This work concerns with the analysis and modelling of possible magnetohydrodynamic response of plasma of the solar low atmosphere (upper chromosphere,

The Sun and the Heliosphere: some basic concepts…

Converging Ideas!!.  Great discussion led by the 4 invited speakers  Chuck Smith – Observational challenges  Ben Chandran – Theoretical questions &

Stuart D. BaleFIELDS iPDR – Science Requirements Solar Probe Plus FIELDS Instrument PDR Science and Instrument Overview Science Requirements Stuart D.

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.

Turbulence as a Unifying Principle in Coronal Heating and Solar/Stellar Wind Acceleration Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

Space Science MO&DA Programs - September Page 1 SS It is known that the aurora is created by intense electron beams which impact the upper atmosphere.

MHD Turbulence driven by low frequency waves and reflection from inhomogeneities: Theory, simulation and application to coronal heating W H Matthaeus Bartol.

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.

IMPRS Lindau, Space weather and plasma simulation Jörg Büchner, MPAe Lindau Collaborators: B. Nikutowski and I.Silin, Lindau A. Otto, Fairbanks.

Applications of MHD Turbulence: from SUMER to Ulysses! Steven R. Cranmer, Harvard-Smithsonian CfA Polar coronal hole protons electrons O +5 O +6.

ALFVEN WAVE ENERGY TRANSPORT IN SOLAR FLARES Lyndsay Fletcher University of Glasgow, UK. RAS Discussion Meeting, 8 Jan

Kinetic Alfvén turbulence driven by MHD turbulent cascade Yuriy Voitenko & Space Physics team Belgian Institute for Space Aeronomy, Brussels, Belgium.

-1- Solar wind turbulence from radio occultation data Chashei, I.V. Lebedev Physical Institute, Moscow, Russia Efimov, A.I., Institute of Radio Engineering.

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,

MHD Turbulence driven by low frequency waves and reflection from inhomogeneities: Theory, simulation and application to coronal heating W H Matthaeus Bartol.

Turbulence and Waves as Sources for the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

Turbulence in the Solar Wind

Modeling the Solar Wind: A survey of theoretical ideas for the origins of fast & slow streams Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

Solar energetic particle simulations in SEPServer How to deal with scale separation of thirteen orders of magnitude R. Vainio, A. Afanasiev, J. Pomoell.

What is the Origin of the Frequently Observed v -5 Suprathermal Charged-Particle Spectrum? J. R. Jokipii University of Arizona Presented at SHINE, Zermatt,

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.

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.

The Physics of Coronal Heating and Solar Wind Acceleration:

Field-Particle Correlation Experiments on DIII-D Frontiers Science Proposal Under weakly collisional conditions, collisionless interactions between electromagnetic.

Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics

2005 Joint SPD/AGU Assembly, SP33A–02

Student Day Working Group III summary

How does the solar atmosphere connect to the inner heliosphere?

Introduction to Space Weather

Heavy-Ion Acceleration and Self-Generated Waves in Coronal Shocks

Coronal Loop Oscillations observed by TRACE

Presentation transcript:

The SPP Theory & Modeling Team: Exploring Predictions & Controversies Steven R. Cranmer Harvard-Smithsonian CfA

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 SPP Theory & Modeling Team Started in November Chair: Marco Velli (JPL/Arcetri) 9 other members: 1st meeting: December 2010, AGU Meeting, San Francisco Ben Chandran Steve Cranmer Jim Drake Ron Ghosh Joe Giacalone Mark Linton Bill Matthaeus Zoran Mikić Gary Zank “One of our roles is to provide an up to date theoretical basis for estimates of the various plasma/magnetic field/energetic particle parameters we will be going to measure as SPP moves into the inner heliosphere, and help out in getting from the Level 1 objectives to data requirements.” Goals: Still being defined. But according to Marco...

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Goal: assemble predictions of what SPP will see Step 1: Online “database” of measurements, extrapolation techniques, empirical models, theoretical models, simulation codes, etc. As of March 2011, there are 13 entries: More are welcome!

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Example extrapolations Salem & Bale collected inward extrapolations of a wide range of plasma parameters from Helios measurements between 0.3 and 1 AU. Cranmer & Chandran extrapolated in situ wave amplitudes inward assuming either no damping or empirically constrained turbulent damping. (2010 SHINE meeting) proton density

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Example theoretical model Cranmer et al. (2007) wave/turbulence models; plot swiped from SWEAP proposal

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Global 3D MHD models? CORHEL/MAS (Predictive Sciences) SWMF/BATS-R-US (Michigan) MS-FLUKSS, ENLIL, etc... CCMC CISM Has anyone yet taken a few solar rotation’s worth of models & folded in SPP’s trajectory? Rušin et al. (2010)

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Controversies...

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 How is the solar wind accelerated? Mass? Momentum? → Parker (1958) was largely right! Energy? What physical processes provide the solar wind’s

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 What is the dominant source of mass? Until relatively recently, the dominant idea has been that the time-steady rate of “evaporation” is set by a balance between downward conduction, upward enthalpy flux, and local radiative cooling (Hammer 1982; Withbroe 1988). (i.e., coronal heating sets mass flux!) heat conduction radiation losses — ρvkT 5252

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 What is the dominant source of mass? Until relatively recently, the dominant idea has been that the time-steady rate of “evaporation” is set by a balance between downward conduction, upward enthalpy flux, and local radiative cooling (Hammer 1982; Withbroe 1988). (i.e., coronal heating sets mass flux!) heat conduction radiation losses — ρvkT 5252 More recently, Hinode & SDO observations of the chromosphere have fueled the idea that much of the corona’s mass is injected from below in the form of jets and spicules (e.g., Aschwanden et al. 2007; De Pontieu et al. 2011; McIntosh et al. 2011).

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 What is the dominant source of energy? vs. i.e., what heats the corona in open flux tubes? Two general ideas have emerged... Wave/Turbulence-Driven (WTD) models, in which open flux tubes are jostled continuously from below. MHD fluctuations propagate up and damp. Reconnection/Loop-Opening (RLO) models, in which energy is injected from closed-field regions in the “magnetic carpet.” Counterpoint: Roberts (2010) says WTD doesn’t work. Cranmer & van Ballegooijen (2010) say RLO doesn’t work.

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 What is the dominant source of energy? There is a natural appeal to the RLO idea, since only a small fraction of the Sun’s magnetic flux is open. Open flux tubes are always near closed loops! The “magnetic carpet” is continuously churning. Open-field regions show frequent coronal jets (SOHO, STEREO, Hinode, SDO). Fisk (2005) But is there enough energy released in the subset of reconnection events that turn closed fields into open fields to account for the coronal heating?

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 What is the dominant source of energy? No matter the relative importance of RLO events, we do know that waves and turbulent motions are present everywhere... from photosphere to heliosphere. How much can be accomplished by only WTD processes? (Occam’s razor?) Hinode/SOT G-band bright points SUMER/SOHO Helios & Ulysses UVCS/SOHO Undamped (WKB) waves Damped (non-WKB) waves

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Controversies about waves & turbulence In situ spacecraft see a dizzying array of variability: The inertial range is a “pipeline” for transporting magnetic energy from the large scales to the small scales, where dissipation can occur. f -1 energy containing range f -5/3 inertial range f -3 dissipation range 0.5 Hzfew hours Magnetic Power

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Controversies about waves & turbulence Origin of the low-frequency (1/f) spectrum:  The self-consistent product of a turbulent cascade?  Spacecraft passage through “spaghetti-like” flux tubes rooted on the solar surface? (Borovsky 2008) Physics of the inertial range (f –5/3 ) of the spectrum:  Is it really 5/3 or 3/2 ? It matters for some models! (Chandran 2010)  Is the magnetic fluctuation spectrum different from velocity and/or density spectra?  How does the “spacecraft-frame frequency” map into true wavenumber space (k ┴ ≠ k ║ ) ?

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Controversies about waves & turbulence Physics of the dissipation range:  Is it really dissipation, or just a different dispersion relation?  If dissipation, what processes are responsible? Minor ions may be able to distinguish one process from another! In the fast wind: waves: varying E, B inhomogeneous & non-Maxwellian particle VDFs dissipation & particle energization instabilities

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 The heating is multi-fluid & collisionless electron temperatures O +5 O +6 proton temperatures heavy ion temperatures In the lowest density solar wind streams... UVCS/SOHO p+p+ e–e–

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 How are ions preferentially heated? MHD turbulence may have some kind of “parallel cascade” that gradually produces ion cyclotron waves in the corona and solar wind. When MHD turbulence cascades to small perpendicular scales, the small-scale shearing motions may be unstable to generation of cyclotron waves (Markovskii et al. 2006). Dissipation-scale current sheets may preferentially spin up ions (Dmitruk et al. 2004). If MHD turbulence exists for both Alfvén and fast-mode waves, the two types of waves can nonlinearly couple with one another to produce high-frequency ion cyclotron waves (Chandran 2005). If nanoflare-like reconnection events in the low corona are frequent enough, they may fill the extended corona with electron beams that would become unstable and produce ion cyclotron waves (Markovskii 2007). If kinetic Alfvén waves reach large enough amplitudes, they can damp via wave- particle interactions and heat ions (Voitenko & Goossens 2006; Wu & Yang 2007). Kinetic Alfvén wave damping in the extended corona could lead to electron beams, Langmuir turbulence, and Debye-scale electron phase space holes which could heat ions perpendicularly (Matthaeus et al. 2003; Cranmer & van Ballegooijen 2003).

SPP Theory & Modeling Team: Exploring Predictions & ControversiesS. R. Cranmer, March 8, 2011 Conclusions The SPP Theory & Modeling Team welcomes additional predictions – especially those that come with tabulated or analytic data that we can play work with. See: It is becoming easier to include “real physics” in 1D → 2D → 3D models of the complex Sun-heliosphere system, so hopefully some of the controversies will be resolved by the time of SPP’s launch! Added inspiration from SDO/AIA