M3.1
From Soteria
Image:Example.jpgThe present page is a template of how to fill in a milestone report for the semiannual report. Note that milestone reports can be much less in depth than deliverables. We just need to say what they are and how far we are in reaching them (as a percent of total). Instead, it is important to describe in depth any problems in reaching the milestone in time (last section below).
To use this template, simply cut and paste it on the wiki page of your milestone.
Lead Beneficiary: LPI
Beneficiaries involved: KULeuven, HVAR, UNIGRAZ, OBSPARIS, ROB, UGOE, SRC-PAS
Due Date: Month 12
Contents |
Goal
Based on multi-wavelength ground and space observations for selected solar events, and with help of new data and models, the energy release in flares and CMEs and the photospheric/coronal magnetic flux budget will be quantified and compared to satellite measurements of their interplanetary consequences. Results will be summarized in the report "Energy release through flares and CMEs, their evolution and geo-space impact parameters for special events" (deliverable 3.1).
Progress so far
On January 30, the Russian CORONAS-PHOTON satellite was successively launched. It carries the TESIS EUV telescope/spectroheliograph (LPI) and the SphinX spectrophotometer (SRC-PAS) for studies of solar activity processes in the current 24th solar cycle.
LPI:
Methods for the modeling of full-Sun monochromatic images in the XUV region obtained by the spectroheliograph RES aboard the CORONAS-F mission along with other simultaneous XUV data (GOES, RHESSI) have been developed and used for a detailed study of physical conditions in coronal structures associated with active phenomena in the solar corona. The problem of particle acceleration in the solar corona has been studied in framework of collapsing trap model by taking into account the particle scattering and braking in the high-temperature plasma of solar flares.
KU Leuven
2.5D viscous/resistive MHD simulations with compressive effects show that a current-sheet in the high Chromosphere/low Corona undergoes to a self-feeding mechanism driving the system from a slow to a fast reconnection regime [Bettarini & Lapenta 2008]. A final turbulent state is reached and this situation is a promising candidate to trigger solar explosive phenomena. People involved: L. Bettarini, G. Lapenta
HVAR, UNIGRAZ, OBSPARIS, ROB
Multi-wavelength observations of six flare/CME events were studied to infere whether the associated coronal shock was ignited by the flare or launched by the CME. The analysis of the kinematics of high-frequency radio type II bursts (recorded by the Astrophysikalisches Institut Potsdam and the Nancay Radio Helioghraph), kinematics of low-height signatures of CMEs (observed by LASCO-C1; EIT), and the evolution of the energy release in the associated flares, showed that in four events the shock was ignited by the flare.
We have analyzed the pre-eruption filament evolution and activity for the 19 May 2007 CME (one of the selected events for SOTERIA). The filament, which later became part of a CME was formed over two days by merging of an active-region and a quiescent filament. Mergence was achieved through several episodes of magnetic reconnection. We also analyzed the eruption itself using data from the twin STEREO spacecraft. The 3-D reconstruction of the eruption shows that the active-region part of the filament erupted with greater speed than the quiescent part, making the eruption asymmetric.
UGOE
CME event list for 3D studies established. Flux rope models successfully applied and extended into the heliosphere based on STEREO/SOHO multipoint space observations. First CME tracked all the way along the Sun-Earth line (STEREO and ACE observations).
SRC-PAS
The SRC-PAS Team has been busy with collecting and archiving the first-light data from the SphinX spectrophotometer, aboard Coronas-Photon. During first 50 days of active operation, the instrument collected ~30 GB of data, including small flares on March 26th. The data analysis of 30 Aug. 2002 and 14 Nov. 2002 flares is in progress. Results of complex analysis of selected flares including HD simulations of interaction between the non-thermal and thermal plasma components have been accepted for publication (A&A) with the SOTERIA acknowledged.
Problem areas
To complete the deliverable 3.1 in time (October 2009) it is necessary to have a special short (1 day) meeting of the involved people for discussion of the draft report before summer vacations.
