1. Multiple-Dip Geomagnetic Storms: Solar-Wind Drivers or Internal Magnetospheric Processes
We invite you to participate in the joint GEM-SHINE session on multiple-dip geomagnetic storms that will be held during the 2008 Summer Workshop in Zermatt, Utah, on Monday afternoon 1:30-5:00 pm. The main objective of this session is to use observations, theory, and modeling to assess the current status and establish collaborative efforts towards understanding the physical processes of geomagnetic storms. In particular, we will focus on the role of external drivers and internal mechanisms in particle transport, acceleration, and loss during multiple-dip storms. The primary topics for discussion are:
1. Solar sources of multiple-dip storms
2. Interplanetary drivers of multiple-dip storms
3. Role of the ionospheric source populations
4. Effects of preconditioning of the plasma sheet
5. Particle injection into the ring current, dayside outflows
6. Effects of ion composition in multiple-dip storms
7. Radiation belt dynamics, contribution of electrons
8. Plasmasphere response, role of drainage plumes
9. Coupling between these regions and feedback to the global system
10. Methods of forecasting multiple-dip storms
We invite those interested in giving a short presentation, or with suggestions for other discussion topics, to contact the conveners Vania Jordanova ( vania@lanl.gov) or Ian Richardson ( ian.g.richardson@nasa.gov).
Speakers in this session include Charlie Farrugia, Michelle Thomsen, and Mikhail Sitnov, and Jie Zhang
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2. Creation and Propagation of CMEs and Plasmoids: Loss of Equilibrium and Subsequent Evolution
Analogies between substorm features in the Earth's magnetic tail and CME/flare releases have been invoked for some time: In both cases, there is a slow energy build-up leading into a rapid release ofprimarily magnetic energy which is then converted to kinetic energy in the form of bulk flow, and thermal and non-thermal particle energy. This process is associated with the ejection of a magnetic bubble, plasmoid, or flux rope from closed magnetic field lines into open space. In this session we focus on similarities and differences between the two scenarios, particularly on large scales, including
release mechanisms, loss of equilibrium or large-scale instability, formation, topology, evolution, momentum gain, energy partitioning.
Anyone interested in contributing should contact
Kathy Reeves <kreeves@cfa.harvard.edu> or Joachim Birn <jbirn@lanl.gov>.
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3. Small-Scale Structure in the Solar Wind and Its Effect on Earth
The solar wind is full of "structure" at all time scales. The structure can be categorized as turbulence, Alfven waves, pressure-balance structures, discontinuities, plasma boundaries, humps and holes, FTEs, microstreams, etc. In this joint-GEM-SHINE session we will explore the effects that these types of structure have on the Earth's magnetosphere. With informal talks and audience discussion we hope to learn more about the following questions pertaining to the various structures. What do they do? Are they important? Does this need more study? Can we ignore them and focus on the mean values of solar-wind parameters?
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4. Is there a Need for More-Detailed Solar-Wind Models
In this session, we plan to have an in-depth discussion on using solar wind models as input to geospace models. Specifically, we ask what output parameters, spatial resolution, cadence, accuracy, etc. do geospace models need from solar wind models in order for them to reasonably reproduce/describe the space environment about Earth? Certainly, the answer to this question will, more than likely, depend on what one is trying to model. Nevertheless, we hope to determine where the strengths of the solar wind models are (i.e., with respect to their use in geospace models) and where they need improvement. The objective of the session is to facilitate communication between the solar/solar wind and geospace communities with the ultimate goal of improving Sun-Earth system modeling and prediction. An in-depth plenary session on the first day of the meeting will precede this session and provide general background on solar wind models and what Magnetospheric researchers need from them.
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5. What Determines When Reconnection Turns On? Chromosphere,
Corona, Solar Wind, Magnetopause, and Magnetotail
6. SEPs from Heliosphere to Magnetosphere
This session will delve into the current understanding of SEP event
generation and transport based on current theories and observations.
We will then consider how these particles access the magnetosphere
and enter the upper atmosphere where they can have significant
space weather effects.The intent is to give an end-to-end perspective on this
aspect of the Sun-Earth Connection, and to encourage interdisciplinary
treatments of the problem.
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7. Comparing the Properties of Magnetic Reconnection in Various
Environments
Magnetic reconnection is a ubiquitous plasma transport and energy release process in space plasmas. Magnetic reconnection is understood to be a key ingredient in solar eruptions and other solar processes, has recently been detected in the solar wind, facilitates energy transfer into the magnetosphere, drives magnetospheric circulation, and produces the dynamical evolution associated with magnetospheric substorms. Owing to this breadth of applications, magnetic reconnection is perhaps the most important fundamental process in space plasmas. This session aims at analyzing observations and models of magnetic reconnection in different heliosphefric environments, with the specific goal to understand commonalities and differences in the way reconnection operates in different space plasmas. The session will include a small number of invited presentations. brief (2 viewgraph) presentations from the audience are invited as well, with an emphasis on discussion, not on AGU-style series of presentations.
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8. Perpendicular Ion Heating: observations at Earth and theory at the Sun
Ion heating transverse to the magnetic field and the associated ion outflow are common processes in the polar and auroral regions of the Earth and the corona of the Sun. The intent of this joint session is to bring together researchers in these areas and explore the similarities and differences between the two regions. On Earth, these heating and outflow processes can be studied with in situ satellite and rocket data, as well as with energetic neutral atom imaging, while in the corona, remote observations from instruments such as the Ultraviolet Coronagraph Spectrometer on SOHO can be used to diagnose the properties of these ions. Theory and modeling efforts have been carried out in both regions. Despite the official title of the session, we solicit short contributions on observations, theory and modeling from either of these regions. The session will be held on Friday, June 27, from 10:30 am-12:15 pm. Please contact Ben Chandran (benjamin.chandran@unh.edu) or Bob Lysak (bob@aurora.space.umn.edu) if you are interested in making a short, informal presentation.
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