Multi-scale physics in coronal heating and solar wind acceleration -
from the Sun into the inner heliosphere

 

Publication Plan

 

            The Workshop papers will be published in the journal Space Science Reviews (Vol. TBD) and reprinted as a hardcover book in the Space Sciences Series of ISSI (Vol. 38), both published by Springer.

            The workshop papers should not only reflect the presentations as made, but also address the subsequent discussions as much as possible.

            It may be advantageous or desirable to combine two (or more) presentations into a single paper. The authors planning to combine their papers are kindly asked to inform the editors before submitting.

            Each of the 3 sections will be concluded by a paper summarizing the main points of the discussion during and after the presentations. The editors are responsible for providing these papers, but they may ask participants for contributions.

            The volume will be edited by David Burgess, James F. Drake, Eckart Marsch, Rudolf von Steiger, Marco Velli, and Thomas H. Zurbuchen.

            Deadline for submission: March 31, 2010

            All papers will be reviewed by a referee (who may or may not be a workshop participant) and by one of the editors.

            Page allocation is about 12 pages per presentation; if two or more presentations are combined to a single paper the allocations are cumulated. There are about 650-700 words per page (minus the space used for figures, tables, etc.)

            Citations are in author-year format; paper titles are not given in the references.

            Manuscripts may be submitted in LaTeX or in Word. The LaTeX style file with a sample paper and a Word template are provided by Springer here.

            Papers must be submitted directly to Springer's electronic Editorial Manager system.

o   When first using that system you will need to register (fourth link from the top left corner). You will then receive a return email with username and password. Some systems may treat these return mails as spam, so please check your junk mail folder in case you dont get a reply within a few minutes.

o   Select Solar Wind as the article type of your submission.


 

Section I. What is the physical process that is responsible for the heating and acceleration of the solar wind from coronal holes? 

Ester Antonucci

UVCS observations of T and V profiles in coronal holes

Eckart Marsch

Helios: evolution of distribution functions 0.3-1 AU

Thomas Zurbuchen

What are the sources of the slow wind?

Rudolf von Steiger

Solar wind charge states and coronal temperatures

Klaus Wilhelm

SUMER observations of coronal hole temperatures

Scott McIntosh

Source observations of the fast solar wind in coronal holes

Viggo Hansteen

Solar wind models from the chromosphere to 1 AU

Yi-Ming Wang

Slow and fast phenomenological/empirical solar wind models

Steve Cranmer

Self-consistent solar wind models

Francesco Malara

Role of waves in coronal heating and solar wind acceleration

Andrea Verdini

Fully self-consistent MHD turbulence models of the solar wind

William Matthaeus

Turbulent MHD reconnection and particle acceleration

Marco Velli &          Rudolf von Steiger

Discussion / Summary I

Section II. What is the relative role of the magnetic topology and reconnection in the release of slow wind and coronal mass ejections?

Spiro Antiochos

Current sheets in the corona and the complexity of slow wind

Jon Linker

Interactions of closed field with open field in the corona: Importance of interchange reconnection

Kazunari Shibata

Fractal reconnection and particle acceleration in the corona

Sm Krucker

Observations of particle acceleration in partially occulted flares

Jack Gosling

Reconnection in the solar wind

Nancy Crooker

Interchange reconnection, signatures and importance for flux balance

Mike Shay

Do kinetic reconnection models produce fast reconnection in large systems?

Justin Edmondson

The role of reconnection in the generation of slow solar wind

Jim Drake

Particle acceleration and power law distributions during magnetic reconnection

Glenn Mason

Power law distributions of suprathermal particles in the quiet solar wind

Simone Landi

3D simulations of magnetic reconnection with and without velocity shears

Bill Daughton

The transition from collisional to collisionless reconnection

Paul Cassak

The onset of fast reconnection in the corona

Thomas Zurbuchen &    Jim Drake

Discussion / Summary II

Section III. What are the processes that dominate the thermodynamic evolution of the solar wind in the inner heliosphere?

Petr Hellinger

Coupling global expansion with local instabilities

Christian Vocks

Vlasov kinetic models of coronal expansion and solar wind acceleration

Viviane Pierrard

Solar wind electron transport - heat conduction and interplanetary electric field

Filippo Pantellini

Heat flux transport

Tim Horbury

Magnetohydrodynamic turbulence spectra in the solar wind - evolution and anisotropy

Vincenzo Carbone

MHD turbulence - scaling, cascading and intermittency

Alexander Schekochihin

Turbulent cascading in the framework of gyrokinetic theory

Jaime Araneda

Nonlinear Alfven/ion-cyclotron wave interactions with ions in the solar wind

Lorenzo Matteini

Effects of plasma wave instabilities on solar wind particle evolution

William Matthaeus

The role of incompressible MHD turbulence in the solar wind

Enrico Camporeale

Space plasma stability theory: a non-modal approach

Burgess, et al.

 

Models of kinetic-scale dissipation in the solar wind: Confronting theories with observations

Horbury,Carbone, Matthaeus

Anisotropy of solar wind MHD turbulence in the inertial and dissipation domain

David Burgess &      Eckart Marsch

Discussion / Summary III