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