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UV spectroscopy with IRIS - experience learned from Hinode/EIS

Author(s): Peter Young

Institution(s): George Mason University

Abstract:

IRIS will be the fourth in a sequence of solar ultraviolet spectrometers, following on from CDS and SUMER on SOHO and Hinode/EIS. The experience gained from these missions will be valuable for ensuring that high quality science results emerge from IRIS right from the beginning of the mission. This presentation will summarize the experience gained from over five years of Hinode/EIS operations and science, and identify where that experience may benefit the IRIS team.




The 3D Analysis of Polar Jets Using Thomson-Scattering Observations from LASCO C3 Images and the Solar Mass Ejection Imager (SMEI)

Author(s): H.S. Yu and B.V. Jackson

Institution(s): Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA 92093, U.S.A.

Abstract:

The X-Ray Telescope (XRT) onboard Hinode provides an opportunity to observe solar jetting activity above the solar poles. LASCO C3 images allow measurements of the coronal response to some of these jets, giving a determination of their speeds and energies that we compare with Hinode observations (Sako et al. 2010, 38th COSPAR). By using the full SMEI (Solar Mass Ejection Imager) image data set, we are able to study these same solar jet responses in the inner heliosphere. Preliminary results from 3D-reconstructed SMEI pseudo C3 coronagraph images have shown a good agreement at the correct position angles and time with the jet responses observed in LASCO (Jackson, 2012, Adv. in Geosciences). Using the SMEI volumetric data we carry this analysis farther, attempting to determine the extent to which these 3D jet responses maintain their identity into the inner heliosphere.




Ejection of cool plasma into the corona - comparison of results from a 3D MHD model with results from AIA/SDO, EIS/Hinode and a 1D loop model

Author(s): Pia Zacharias, Sven Bingert, Hardi Peter

Institution(s): International Space Science Institute, Bern, Switzerland; Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany; Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany

Abstract:

The formation and subsequent ejection of cool plasma into the corona will be discussed, as observed in our three-dimensional magnetohydrodynamic (3D MHD) model of the solar atmosphere extending from the photosphere into the corona. The model accounts properly for the energy balance, especially for heat conduction and radiative losses, allowing us to reliably synthesize the profiles of optically thin extreme ultraviolet emission lines and compare them to existing observations. A detailed description of the nature of this particular phenomenon will be provided. The analysis of the various forces acting upon the plasma in the 3D model shows that the pressure gradient which is driving the ejection is due to Ohmic dissipation of currents resulting from the braiding of the magnetic field lines by photospheric plasma motions. Preliminary results of a parameter study on the reproduction of the phenomenon in a one-dimensional loop model support the scenario of a heating event that leads to the ejection of cool plasma into the corona in both, the 1D loop model and the 3D model. In addition, results of the numerical model will be compared to observations from the Extreme Ultraviolet Imaging Spectrometer (EIS) onboard Hinode and the Atmospheric Imaging Assembly (AIA) onboard SDO, where we have also found evidence of cool plasma ejecta that are moving along magnetic field lines.





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Last Updated on Tuesday, 24 January 2012 13:45