D3 1 report
Below the outline of deliverable 3.1 (= minutes of meeting at ROB on June 22)
Introduction
Janusz writes the introduction on the basis of his presentation WP3_Sylwester.pptx
We focus on research with space weather implications and organize the report accordingly. This document should have a different focus than deliverable 3.3 (initiation of flares and CMES) There are 4 components to the energy releases for space weather (flares, CMES, shocks, particles). This correspond to the subsection in the next chapter.
JS: suggest to look at an old NASA SMM report.
This report is on the state of art with latest results.
The target public: specialized referee scientists
By July 10: Everybody to send a publication list to Vladimir of related papers since Nov last year. Everybody to send favorite events to Vladimir, these events become content for the report.
Transient solar phenomena associated with energy release in the chromosphere and corona: description and classificiation
Flares and flare-like phenomena
SRC- PAS J. Sylwester
Sphinx results: http://www.cbk.pan.wroc.pl/sphinxnews/?page_id=25
Catalog of A, S and Q flares exists: hunderds of events. Available on request.
Alexander on CORONAS F results on hot & superhot plasma sources such as SPIDERS.
Corona can be divived in warm 1-3 MK (EUV), hot 3-5 MK (XRT), superhot > 5 MK (Mg XII).
Hot plasma source can exist for longer than 24 hours while cooling times should be < 30min.
1. Determine the source region properties of solar eruptive events
Coronal mass ejections
LPI Slemzin
http://adsabs.harvard.edu/abs/2004ASPC..325..381Z
http://adsabs.harvard.edu/abs/2007ApJ...664L.131Z
Waves and shocks
This will be edited by Jasmina and Bojan. It will be based on a recent review by Bojan. Bojan's main contribution is however in the modelling. Volker will ask Graz if they have a list of Halpha moreton waves. This will be compared quickly with NEMO.
Jasmina studies coronal shocks. From radio data, she estimates different parameters such as electron density, velocity, Alfven Mach number, etc. She then links these to the source triggers, viz. flares and CMEs. http://adsabs.harvard.edu/abs/2008SoPh..253..305M http://adsabs.harvard.edu/abs/2004A%26A...427..705Z
Volker: Use coronal waves as diagnostic tools to remotely sense the corona EUV waves on the disk will be used as a source region tracker and we will see if this can be proxy for in-situ events.
Jasmina to ask Graz for any other contribution related to this.
It is sufficient here to report existing results and an outlook for future work & collaborations.
solar energetic particles
LPI S. Bogachev
Giovanni can contribute here work on particle acceleration by waves and shocks (note link with previous section).
New data, observations and analysis techniques
Here we describe the new stuff coming online with support of SOTERIA. Note that this is mostly a working plan for the near future;
Tesis
Presentation Vladimir on TESIS
PROBA2
David will contribute text on SWAP and LYRA (2 pages max).
Graz
To be asked what can be put here. There should be a section on Ca-II K telescope and H-alpha patrol (in proposal it says: to support studies on the flare energy release and related CME initiation processes)
Sphinx
New data resulting in new classification: Q and S flares. New analysis techniques: DEM.
New software
Solar Soft: Diffraction pattern for flares in TRACE images. This allows to restore the shape of the flare kernel and kernel temperature from diffraction pattern.
David: paragraph on CACTUS Pavel: paragraph on NEMO
Physical interpretation of observations and modelling of transient plasma
Energy release in impulsive solar flares
SRC- PAS J. Sylwester
The photospheric flux in the source region of CMEs is estimated to be at the order of in case of X- ray associated flares of class …
Dan Seaton theoretical talk: coronal inflows: TRACE 195 2002-april-21, Somov-Titov : integration across current sheet, heat conduction=thermal halo, structure of slow mode shocks, height of the X-line in the corona is deep down in the corona, Janusz confirms that he has RESIK data for this flare and can contribute temperature estimates.
Long duration hot coronal plasma structures
LPI A.Urnov 4. Advanced modeling of hot plasma dynamics in flare and CME events
Eruptive processes and CMES
UGEO, UNIGRAZ V. Slemzin
2. Understand the onset mechanisms of CMEs and flares and their energy disposal into the corona and solar wind 3. Understand the photospheric processes in the SRs
This section would be the most adequate to put in the KULeuven/CPA simulations. There are 3 types:
1) acceleration, 2) ? 3) interaction with streamers
Acceleration of particles in flare reconnection site
LIP S. Bogachev
Text from S. Bogachev The spacecrafts Yohkoh, SOHO, RHESSI and HINODE received clear evidences that the solar corona is not just a place for energy accumulation, but is also a region of highly effective energy release: we mean discovery of loop-top hard X-ray sources in the solar corona made by Yohkoh and RHESSI and regions of high-temperature plasma (spiders) revealed by CORONAS-F/SPIRIT. These phenomena do not fit into the standard model of solar flares and indicate that standard model needs for serious modification. During SOTERIA project we are going to develop at least two new models of solar flares: two-step model of flare with a collapsing magnetic trap and new model of multi-temperature flare proposed by XRAS. Both the models are in good agreement with data of observations.
The collapsing trap model in addition provides us a new approach to the problem of particle acceleration in flares and the problem of generation of the solar energetic particles. The acceleration of particles in this model takes place within the shrinking tubes of reconnecting magnetic lines under the action of two mechanisms: betatron and Fermi acceleration. Particle acceleration within the trap has high efficiency (typical acceleration time is of the order of several seconds), act on the particles of all masses (electrons, protons and heavy ions), and allows to explain most features of particle acceleration in flares: the mean and maximal values of particle energy and particle energy distribution.
The experimental contribution of XRAS laboratory to the SOTERIA project is development of new space experiment, TESIS, to study the Sun and solar activity. TESIS is a set of several solar instruments (telescopes and spectrometers), working in orbit since January 30, 2009 on board the Russian satellite CORONAS-Photon. TESIS is intended for exploration of the upper solar atmosphere (the transition layer, and the lower and intermediate solar corona) with angular resolution of about 1.5 arc seconds. In the framework of SOTERIA project, the TESIS will allow to realize multiple research programs for investigation of solar flares, eruptive prominences and coronal mass emissions. The first four months of the TESIS work showed its high efficiency for study the solar activity. There were detected several flares of GOES X-ray class A and B, found about 10 eruptive prominences, made observations of a number of active regions in dynamics, and provided unique observation of CME formation in far solar corona.
Acceleration of SEP
LPI
Geo-space impact of transient solar phenomena
ROB A. Zhukov
Andrei's together with Luciano made a text that is ready for copy and paste into this section.
Propagation of CMEs in the heliosphere
6. Understand the kinematics and evolution of CMEs Sun to Earth 7. Establish reliable Sun to 1 AU connections and quantitative estimates of the 1 AU parameters as derived from solar quantities
The study of these ICME events show that compression effects in ip space (stream interactions) contribute significantly (as much as xx%) to the total field strength of ICMEs at 1 AU. - A CME event observed stereoscopically by STEREO on xx May xxxx shows that the spatial extent and mass is … the kinetic energy …
http://adsabs.harvard.edu/abs/2008AnGeo..26..213R
http://adsabs.harvard.edu/abs/2005IAUS..226..437Z
Particle propagation and magnetic convection to source region
Physical processes in the Earth environment caused by solar eruptive events
MHD Modelling and Simulations
Include physical units. Don't normalise otherwise we cannot compare to observations.
Appendix Table: Overview of special solar events
LPI+ ...
Here we put a table listing the events. The analysis of the events goes into the sections above.
Criteria for selection of the events. List of analyzed events and their description ==
Conclusions
8. Establish advanced MHD simulations 9. Achieve advance in observing and forecasting flares and CMEs
