WP3
Participants
OBSPARIS, SPD-SRC-PAS, ROB, HVAR, UGOE, LPI, UNIGRAZ
Summary
WP3 (Chromosphere and Corona) will investigate the initiation of coronal mass ejections and their impact on the corona and heliosphere based on a unique set of ground- and spaceobservations at visible, EUV and X-ray wavelengths. The waves triggered by coronal mass ejections will be used as a diagnostic tool to remotely sense the plasma and magnetic field characteristics of the ambient corona. Using multi-spacecraft observations will allow to infer the 3D structure of CMEs and flaring regions and to help quantify their energy input into the low corona and their heliospheric modulation up to Earth orbit. The newly established data sources will be integrated into the VO and results will be used as input for Vizualization for E/PO purposes.
Objectives
a) Understand the onset mechanisms of CMEs and flares and their energy disposable into the corona (heating) and solar wind.
b) Understand the kinematics of CMEs and impact on the global corona with emphasis on the excitation of large-scale coronal waves and acceleration of particles.
c) Remote sensing of the plasma and magnetic field structure of the solar corona by means of wave diagnostic tools (large-scale coronal seismology).
d) Understand the 3D structure of CMEs and evolution into the heliosphere
e) Quantify the energy input to geo-space from flare and CME models, including heliospheric stream interactions.
Deliverables
1. The energy release in flares and CMEs will be modelled based on emitting plasma diagnostics using multi-wavelength space- and ground-based observations. The method provides a spatial distribution of the electron temperature and density along with the differential emission measure function.
2. Based on multi-wavelength space- and ground-based photospheric and coronal observations, a 3D model for the structure of CMEs will be developed and tested using SOHO and STEREO observations from different vantage points. For scientific demonstration, educational and public outreach purposes the derived 3D CME model will be visualized.
3. The new observations from STEREO and Hinode, in conjunction with SOHO data and ground-based measurements will be used as input, in addition to the results from 3.1 and 3.2 to improve existing CME, flare initiation models and to settle ground for quantitative forecasting.
4. UNIGRAZ will construct and mount the Ca-II K telescope at Kanzelhöhe observatory and take high cadence observations in H-Alpha (flare patrol) and Ca-II K that will be delivered to the SOTERIA consortium via an Internet data server. H-alpha data from OBSPARIS and HVAR, and USET data provided by ROB will complement the database.
5. The SphinX database established by SRC-PAS will provide (soft) X-ray measurements in the 0.5-12 keV range from 256 energy channels from the CORONAS satellite.
6. LPI will provide a CORONAS/SPIRIT/TESIS X and EUV spectral images (8.42-335 Å) database.
7. UGOE will provide at Planetarium Hamburg a STEREO database for analysis and visualization purposes.
8. ROB will provide a database for SWAP and LYRA data from the Proba2 mission.
