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Call for Abstracts

Call for Abstracts

We are no longer accepting abstracts.



The agenda for this interactive 4-day meeting consists of plenary sessions with keynote presentations on the various coupling themes listed below, as well as many additional splinter and poster sessions.  We are soliciting abstracts on eight themes to be presented in several presentation formats:

  • Oral – Presentations will be in the main plenary session or a related splinter session.
  • Standard Poster – In the main exhibit hall on traditional poster boards.  You poster can be up to 4 feet wide x 5 feet tall.
  • Electronic Poster (e-poster) – An e-poster uses a large (46 inch) monitor and computer to display a multimedia version of a poster, giving a presenter an opportunity to effectively convey information that would not necessarily be possible with a traditional printed poster.

Please submit all abstracts by Aug. 1, 2014 via the online submission form or you can email them to This email address is being protected from spambots. You need JavaScript enabled to view it. .  Please include your session preference, presentation format preference, and your contact information (name, email, affiliation, co-authors).  Abstracts are limited to 250 words. We encourage your participation and hope that you will share this announcement with colleagues.

Session Topics: (There will be one plenary session, two splinter sessions, and two poster sessions for each theme.)

1a.  Magnetic Energy and Field from Solar Interior to Corona and Heliosphere
These sessions will host presentations that discuss the origin and evolution of the solar magnetic field and associated solar cycle, the storage mechanisms and heating processes in solar and coronal magnetic fields and the extended interplanetary environment. 

1b.  Reconnection and Magnetic Instabilities in Geospace, Heliosphere, and the Solar Atmosphere
These sessions will offer discussion of the energy release mechanisms that convert stored magnetic free energy. Reconnection occurs over many spatial scales in the solar atmosphere, within terrestrial magnetospheres, and has down-stream impacts on radiation and particle populations in geospace.

2a.  Evolving Coronal Mass Ejections from Corona, through the Heliosphere, into Geospace
These sessions will will address the "cradle to grave" physics of coronal mass ejections, from their origin in the solar atmosphere to their impact at Earth.  Relevant topics include energy storage and release, magnetic topology, propagation through the heliosphere, ICME in situ observations, and impact on geospace processes.

2b.  Dynamics of Energetic Particles, Wave-Particle Interactions, Shocks, and Turbulence
These sessions will address mechanisms for and effects of wave-particle interactions, energetic particle acceleration and transport, shocks, and turbulence throughout the Sun-Earth system.  

3a.  Ion-Neutral Interactions within Earth's Atmosphere and the Solar Atmosphere
These sessions will address the effects of ion-neutral interactions on the energetics and dynamics of the Earth's ionosphere, as well as discussions on the dynamics, energetics and ion-neutral effects in the solar chromosphere and transition region.

3b.  Heliosphere-Magnetosphere Interactions from Bowshock to Geotail
These sessions will address the flow of energy in and around the geospace system, focusing on global and local physical processes that govern the redistribution of energy within the terrestrial magnetosphere.

4a.  Origins of Solar Magnetic Fields, Variability, and Effects at Earth
These sessions will address the origins of the solar dynamo and the solar magnetic fields through helioseismology studies, solar activity, such as irradiance variations, flares, solar energetic particles (SEPs), and coronal mass ejections (CMEs), and how these solar activities influence variations throughout the heliosphere, including a myriad of effects in Earth's atmosphere.
4b.  Modeling and Forecasting Space Climate and Space Weather Events
These sessions will address how the extended fleet of heliospheric, geospace, and planetary spacecraft in NASA's Heliophysics System Observatory (HSO) have enabled improvements to, and also have benefited from, a variety of data assimilation and theoretical models of the Sun, heliosphere, and planets' magnetospheres and atmospheres. One aspect of some of these models is to provide predictions and forecasts for space weather events that affect the complex and coupled processes throughout our space environment.