************************************************************** * * * European Physical Society * * European Astronomical Society * * * * S O L A R P H Y S I C S S E C T I O N * * * * N E W S L E T T E R * * * * 6 February 1998 * * * ************************************************************** SPS EPS-EAS =========== Chairman: G.M. Simnett (Birmingham) Secretary & Treasurer: P. Heinzel (Ondrejov) Newsletter Editor: J. Staude (Potsdam) SPS-Board members: ================== G. Simnett (U.K.) - President P. Heinzel (Czech Rep.) - Secretary C. Alissandrakis (Greece) G. Belvedere (Italy) M. Goossens (Belgium) I. Kim (Russia) J. Kuijpers (The Netherlands) E. Landi (Italy) E. Marsch(Germany) P. Martens (ESTEC) P. Palle (Spain) N. Vilmer (France) _______________________________________________________________________________ _______________________________________________________________________________ ESA SOLAR PHYSICS PLANNING GROUP _______________________________________________________________________________ _______________________________________________________________________________ Summary of Meeting on 16 Jan 1998, Paris ---------------------------------------- Present: E Priest (chair), M Coradini (secretary), T Appourchaux (SSD), C Chiuderi, L Dame, W Flury (ESOC), R Harrison, O Kjeldseth-Moe, O von der Luhe, E Marsch, D Rust, S Solanki. 1. Introduction The chairman welcomed members to this first meeting of the Group, especially Dave Rust as NASA representative and the advocates for missions on high-resolution (L Dame), stereoscopic studies (R Harrison) and near-Sun encounters or probes (E Marsch). He recalled that the purpose of the Group is to advise the european solar community and ESA on the best way forward to obtain a new solar and heliospheric mission after SOHO. It therefore aims to have a thorough, fair and in-depth comparison of the different ways forward. The perception in ESA is that the solar community is divided and does not know what to do after SOHO. A commitment was therefore given by each member of the Group to work for solidarity and the unity of the solar physics community on this issue. 2. Background M Coradini described the new implementation plan of ESA's Horizons 2000 Programme. A SMART 1 mission in 2001 will test ion drive which could be of interest for some solar missions. Our aim is to be able to propose an outstanding mission for the F2 and F3 slots in 2007 and 2008 at a rough cost of 175 mau (200 m$). For these a call for ideas is likely in 1999 leading to a pre-phase A study, so we shall try to reach a concensus by the end of 1998. E Priest described the Crawley meeting in March 1997, where the different ideas for possible future missions had been discussed. A brief review of the Yohkoh and SOHO missions was given. The next desirable steps seem to be for either higher spatial resolution or 3D imaging or in-situ sampling. D Rust described NASA's space science strategic plan and the Sun-Earth connection road-map. Future missions include TRACE (transition region and coronal explorer) in 1998, HESSI (high-energy solar spectroscopic imager) in 2000, STEREO (solar-terrestrial relations observatory), SolarB in 2004 and beyond that there is talk in the long-term of a solar probe and a solar polar imager. In addition, future mission concept studies are under way on stereo (Brueckner), solar bolometric imager (Foukal), high-resolution x-ray explorer (Golub), solar imaging radio array (Kaiser), stereo x-ray coronal imager (Liewer), solar polar sail mission (Neugebauer) and solar quadrupole moment mission (Smith). The following criteria were agreed for deciding between different mission possibilities: (i) Scientific excellence - the importance of the scientific aims; (ii) Technical feasibility within cost and time frame; (iii) Role in international scene - either distinctive or collaborative; (iv) Appeal to a wide solar and heliospheric community. 3. Possible European Solar Missions Three types of mission were discussed and in each case a small team was set up to examine the suggestion in more detail, with the help of the appropriate advocate. The teams would give a preliminary report back to the Group at its meeting at the Workshop on a Crossroads for european Solar and Heliospheric Missions in Tenerife (March 23-27). They would assess the pros and cons against the four criteria listed above and also against other questions that differ from one proposal to another, as listed below. (a) High Spatial Resolution L Dame described a three-telescope solar interferometer proposed for Proteus, which is a French programme with one launch every two years at roughly 1/5 the cost of an ESA F-mission. He is hopeful for its selection in March and launch in 2004, 2006 or 2008. It would give an improvement of a factor of 40 in spatial resolution over the best that is available at present and would work in the FUV and UV. If selected by CNES, he would like to see it extended to become a joint CNES/ESA mission in the spirit of the earlier SIMURIS proposal made for M3. Such a joint mission would include extra complementary European experiments, such as an EUV imager, fields and particles, XUV spectrograph, magnetograph, which would enable an understanding of context and consequences of the high-resolution images. The assessment team, led by O von der Luhe, will also include O Kjeldseth-Moe. It will consider the following additional questions: (i) is the concept technically viable (signal/noise, etc...); (ii) what are the detailed scientific aims; (iii) how does it compare with a single telescope (cf Hirex in x-rays) (iv) how could the PROTEUS proposal to CNES link up with a possible joint CNES/ESA mission ? (b) Stereoscopic Imaging R Harrison described the stereo mission that has been proposed by Europe and the rather different stereo mission that is being advocated in the USA and in which european representatives have been involved. The latest american proposal consists of two satellites each with euv and/or x-ray imagers, a coronagraph and a solar wind package. The angular separation of the two satellites would gradually increase, reaching for instance a separation of 105 degrees after two years. A launch of 2004 is possible. A study of cme's is their main aim. The european proposal has satellites remaining at the L4 points and has a broader goal including a greater study of 3D coronal structures with multiple line-of-sight spectroscopy. The assessment team, led by S Solanki, will include V Bothmer, D Rust and R Schwenn. It will open a link with the NASA stereo team in order to see best how to undertake a joint mission and bring the european and american plans together. The additional questions to be considered are: (i) what would the ESA role be (an extra spacecraft or extra instruments); would there be a NASA stereo mission (perhaps with some european instruments) and an ESA mission with complementary aims (and perhaps some american instruments); or could there be a single NASA/ESA stereo mission stopping at L4 rather than continuing to drift; (ii) should the european and american stereo groups be merged; (iii) what about the possibility of an out-of-the-ecliptic european satellite, using solar electric propulsion, and having the same instruments as the NASA stereo; (iv) what science would be the european focus; (v) what about the timing of the NASA and ESA missions; (vi) orbits and mass ? (c) Near-Sun Encounters or Probes E Marsch decribed the rationale and scientific objectives for the Interhelios Mission. It will provide observations of the Sun and solar wind from 30 solar radii. With a 10 cm mirror a resolution of 1 arcsec will be obtained. It will provide time-variability and fine-scale structure of the source regions of the solar wind. In future, for comparison, the Group plans to hear presentations on the solar probe, which has been studied in Europe and is part of NASA's Outer Planets/ Solar Probe line, with the first launch planned for 2002/3 and later ones at two-year intervals; the order of the three missions (Solar Probe, Pluto-Kuiper Express, Europa Orbiter) is expected to be decided in 3 or 4 months time. The assessment team, led by R Harrison, will include JC Vial and A Roux. The additional questions to be considered are: (i) how do the pros and cons of solar probe and interhelios compare (use will be made of previous JPL documents on the probe); (ii) what are the pros and cons of: different orbits and perihelions; a single pass or multiple orbits; including imaging or not; (iii) what can be accomplished within the F2/F3 financial envelope; (iv) how do the time-scales for ESA and for an interagency mission compare ? 4. Call for Input to Assessment Teams If you wish to send comments on any of the above questions (either in favour of or against a particular mission) to any of the leaders of the assessment teams, please feel free to do so. Their email addresses are Oskar von der Luhe ovdluhe@kis.uni-freiburg.de Sami Solanki solanki@astro.phys.ethz.ch Richard Harrison harrison@solg2.bnsc.rl.ac.uk **************************** Prof Eric Priest Mathematics and Computational Sciences Dept Tel. 0(44)1334 463709 St Andrews University Fax 0(44)1334 463748 ST ANDREWS Sec (Gill) 0(44)1334 463708 KY16 9SS Email eric@dcs.st-and.ac.uk UK Home page http://www-solar.dcs.st-andrews.ac.uk/~eric/index.shtml **************************** _______________________________________________________________________________ _______________________________________________________________________________ MEETING ANNOUNCEMENT _______________________________________________________________________________ _______________________________________________________________________________ * Please, note that the following announcement contains a correction as * * compared with the same announcement in the last issue of the * * SPS Newsletter: 1998 instead of 1997 is correct! * %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %%%% First Announcement of MHD Summer School in Crete %%%% % % % Dear Colleague: Please bring this announcement to the attention of % % anyone you know who might be interested. Thanks. % % % % Kanaris Tsinganos % %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %%% LATEX FILE %%% \documentstyle[12pt]{article} \sloppy \pagestyle{empty} \setlength{\textheight}{21cm} \setlength{\textwidth}{15cm} \setlength{\voffset}{-1 truecm} \begin{document} \begin{center} {\Large \bf Summer School: First Announcement \\[8mm] ``Dynamical MHD Phenomena in Solar \\[4mm] and Astrophysical Plasmas''\\[8mm] Fodele Beach Hotel and Conference Center (near Heraklion), Crete\\[4mm] 22 June\,--\,3\, July 1998}\\[1.5cm] \large \end{center} \noindent{\bf School Director: Kanaris Tsinganos} \noindent{\bf Scientific Organizing Committee: Jean Heyvaerts, Alan Hood, Moira Jardine, Fernando Moreno-Insertis, Giannina Poletto, Eric Priest, Manfred Schussler, Jurgen Staude} \noindent{\bf Local Organisation: John Contopoulos and Nektarios Vlahakis}. \bigskip\noindent This is the third of a series of three summer schools aimed at introducing young ($\le 35$ years of age) researchers to Solar Magnetohydrodynamics (MHD) and its interactions with other disciplines. The schools are funded by the European Commission, as part of its Training and Mobility Programme, in a grant coordinated by Eric Priest. The first school was held in St Andrews, and devoted to MHD Reconnection while the second in Berlin and devoted to MHD Waves and Turbulence. This School is concerned mainly with Dynamical MHD Phenomena, and through the organized lectures and contributions from the participants aims to introducing a wide area of current theoretical research activity in Dynamical Plasma Astrophysics and point out areas of cross-fertilisation between laboratory, magnetospheric, solar and astrophysical MHD. The Course will take place at the Fodele Beach Hotel and Conference Center (near Heraklion, Crete, Greece). This School should prove particularly appropriate for graduate students and postdoctoral researchers. {\bf Travel and subsistence funding will be provided for 40 EU students}. Participants from non-EU countries paying their full costs will also be welcome. Students are required to attend the whole of the School. There will be a Registration fee, details of which will be given in the Second Announcement. The Second Announcement will be issued by the end of January and will give further details of the programme, travel aspects, a Final Registration form, and details of payment of the registration fee. Announcements will also be available soon on the www: http://www.physics.uch.gr/$\sim$tsingan/mhd98/Announcement1.html If you are interested in attending the School, please return the registration of interest form (see below) {\bf as soon as possible} either by e-mail to mhd@physics.uch.gr, or by post to:\\ K. Tsinganos, MHD98 School, Dept. of Physics, University of Crete, Heraklion 71003, Crete, GREECE\\ Telephone: 30 - 81 - 394213, FAX: 30 - 81 - 394201 \subsection*{\bf Provisional programme of lectures/topics} \hoffset -1 truecm \begin{tabular}{rll} 1. & Dynamical Processes in Laboratory Plasmas & (P. Browning, UK)\\[3mm] 2. & Magnetospheric Dynamics & (K. Schindler, Germany) \\[3mm] 3. & Simulations of Dynamical Space \& Solar Plasmas & (D. Spicer, USA) \\[3mm] 4. & Review of SoHO Observations & (E. Antonucci, Italy) \\[3mm] 5. & Basic Theory of MHD Instabilities & (F. Moreno-Insertis, Spain) \\[3mm] 6. & Review of Yohkoh Observations & (L. Culhane$^*$, UK)\\[3mm] 7. & Eruptive Solar Prominences & (A. Hood, UK)\\[3mm] 8. & Review of Ulysses Observations & (A. Balogh$^*$, UK)\\[3mm] 9. & Constraints on Solar Wind Modelling & (G. Poletto, Italy)\\[3mm] 10. & Nonlinear Dynamos and MHD Turbulence & (G. Field, USA) \\[3mm] 11. & Magnetic Field Generation - A New Approach & (R. Rosner, USA) \\[3mm] 12. & Magnetic Fields of Rapidly Rotating Young Stars & (M. Jardine, UK) \\[3mm] 13. & Selfsimilar Collapse of Molecular Cloud Cores & (J. Contopoulos, Greece) \\[3mm] 14. & Magnetized Winds and Accretion Flows & (J. Heyvaerts, France) \\[3mm] 15. & Analytical Modelling of Winds/Jets & (E. Trussoni, Italy) \\[3mm] 16. & Particle Acceleration in Magnetized Accretion Disks & (M. Kafatos, USA)\\[3mm] \end{tabular} $^*$ to be confirmed \newpage %Registration of Interest Form \parskip 0.3 cm %****************************************************** {\bf Registration of Interest Form} {\it Return the completed form to:} {\bf mhd@physics.uch.gr} {\it (or post to address given in this announcement)} {\bf Dynamical MHD Phenomena in Solar \& Astrophysical Plasmas June 22 - July 3 1998 First Name and Family Name: Male/Female : Department : Institute : Address : Town : Post Code : Country : \it Please state briefly your area of research: Are you \begin{enumerate} \item an EU national student (please state nationality): \item a non-EU student : \end{enumerate} } %**************************************************** \end{document} ______________________________________________________________________________ ______________________________________________________________________________ SOLAR PHYSICS announces CD-ROM _______________________________________________________________________________ _______________________________________________________________________________ >From "Eugene J. de Geus" >28 Jan 1998 The editors are pleased to announce an important new addition to the journal. Starting in 1998, Solar Physics will publish a CD-ROM twice a year as an integral part of its publishing scheme. The CD-ROM shall serve as a platform for the publication of electronic addenda to articles published in the printed version of the journal, at no cost to the author. This can include items such as large, high-resolution images, colour figures, long series of images (showing a development observed or effects of variable parameters in a model), and time-lapse images from observations, models, or simulations. Electronic datasets will be considered for inclusion on the CD-ROM only if they are an integral part of a complete article accepted for publication in the main (printed) version of Solar Physics. The high standard of refereeing of Solar Physics shall, therefore, also apply to the information proposed for publication on the CD-ROM. The article and the electronic information will need to be fully integrated into a well-written and understandable publication, with the article describing and interpreting the information presented on the CD-ROM. Figure or Movie captions may be included on the CD-ROM, but the article itself will not be. The process of refereeing requires that the author of the article submit the text in standard fashion, and transfer the electronic data to an ftp site provided by the publisher. The format of this information shall be MPEG for movies, JPEG or GIF for images, and HTML for plain text such that commonly available Internet applications can be used for viewing purposes. The format of the materials on the CD-ROM will be the same (MPEG, JPEG, GIF, HTML) so that the CD-ROMs will not need to carry any tools for viewing the images contained on the disk. Upon acceptance of the paper for publication, the author(s) shall be responsible for providing the datasets in the appropriate form to the publisher. This implies that a "main" html file needs to be provided which shall constitute the homepage on the CD-ROM for that article. This file shall carry appropriate links to the electronic datasets. The datasets of course also need to be provided and need to be in the appropriate format. The publication frequency of the CD-ROM shall initially be twice a year, with the first CD-Rom scheduled for the Summer of 1998. The CD-ROM will be published and shipped accompanying the issue of Solar Physics which shall contain the papers associated with the electronic materials. Papers which make use of the electronic medium shall therefore be published only twice a year, and authors of papers with accompanying CD-ROM data should be aware that publication delays in their papers may occur because of this schedule. The editors hope that the community of Solar researchers shall find this a valuable addition to the journal. The Editors Zdenek Svestka zdenek@sron.ruu.nl Bob Howard howard@noao.edu Oddbjorn Engvold oddbjorn.engvold@astro.uio.no _______________________________________________________________________________ _______________________________________________________________________________ EMPLOYMENT OPPORTUNITY _______________________________________________________________________________ _______________________________________________________________________________ Solar-Terrestrial Postdoc in Denmark >From thejll@dmi.min.dk (Peter Thejll); 20 Jan 1998 A 3-year post-doctoral position in the field of Solar-Terrestrial physics and the Solar-Climatic relationship is announced at the Danish Meteorological Institute in Copenhagen, Denmark, starting in 1998. A PhD physicist is sought for working on the problems of external forcing of the climate - particularly the problems surrounding how the Sun may be controlling factors that influence climate. At the moment we are focusing on how the global cloud cover may be modulated by external factors. The successful candidate will work in collaboration with colleagues in the field of Solar-Climatic relationships, in geomagnetism, solar/heliospheric physics, and the solar wind as well as climatology and meteorology, at the newly established DMI Climate Centre. Our working methods at present rely on the analysis of observational data from the above disciplines, but we are seeking to expand our activity in the field of physical modeling of the processes, and/or experimental work. The DMI is a government institute serving the traditional needs for weather forecasting and climate services as well as operating the chain of magnetometers and other geophysical stations in Greenland and Scandinavia. The DMI can also count one of the largest parallel super-computers in Europe amongst its resources for researchers. Research into climatic changes and the reasons therefore is an important part of the work at the research department of the DMI, and the DMI currently holds a leading position in research on the Solar-Climatic link. Salary will be in agreement with standard Danish rules and depends on the candidates seniority (years since the MSc, or equivalent degree) - it will be about US$3500 to 4000/month, before Danish taxes. Interested candidates should contact Henrik Svensmark (hsv@dmi.dk) or Peter Thejll (thejll@dmi.dk, Tel.: (+45) 39 15 74 77) for further details. Applications with a CV and names of referees should be received no later than March 17 1998. DMI, Solar-Terrestrial Physics Group, Lyngbyvej 100, DK-2100 Copenhagen, Denmark. _______________________________________________________________________________ _______________________________________________________________________________ WEB SIDES _______________________________________________________________________________ _______________________________________________________________________________ Yohkoh Public Outreach ---------------------- >From David Alexander >21 Jan 1998 Dear Colleagues, I would like to take this opportunity to bring to your attention a web site that we have been putting together over the last two years as part of a public outreach and education project. The Yohkoh Public Outreach Project (YPOP) is a NASA funded educational outreach project designed to facilitate public access to high quality Yohkoh/SXT and other solar data via the Internet. As part of this project we were charged with the production of a high quality version of Yohkoh/SXT long-term movie. Over 5 years of the Yohkoh mission are now online with a cadence of approximately 1 frame per 6 hours. This provides a quick-look data access facility for use by the solar community as well as educators and the general public. The movie can be accessed via http://www.space.lockheed.com/YPOP/FilmArchives/data_access.html Another feature you might find of interest is the weekly Yohkoh science nugget from the SXT Chief Observer at ISAS. This can be found at http://www.space.lockheed.com/YPOP/ProjectionRoom/Weekly/ The general outreach site can be accessed via http://www.space.lockheed.com/YPOP/ and is full of interesting activities and information. The YPOP pages are being continually updated and improved but please have a look at our site and if you have any comments or suggestions let us know. Thank you, David Alexander Lockheed Martin Solar and Astrophysics Lab Org. H1-12, B252 3251 Hanover St Palo Alto CA 94304 USA ------------------------------------------------------------------------ New San Fernando Observatory Web Site ------------------------------------- >From stephen.walton@csun.edu (Stephen Walton) >3 Feb 1998 The San Fernando Observatory has recently reorganized its Web site. In particular, daily updated photometric full-disk solar images in two wavelengths are available. In the near future, we plan daily postings of sunspot number, area, and location, and facular areas. A downloadable archive of SFO's twelve years' worth of photometric full-disk solar images is being developed, and should be partially in place by the end of 1998. The site is located at http://davinci.csun.edu/~astro/sfo.html. _______________________________________________________________________________ _______________________________________________________________________________ ********************************************************* * SPS Newsletter * * Editor: J"urgen Staude * * Astrophysikalisches Institut Potsdam * * Sonnenobservatorium Einsteinturm * * Telegrafenberg * * D-14473 Potsdam * * Germany * * tel.: 49-331-288-2300 (49-331-288-2331 - secretary) * * fax: 49-331-288-2310 * * e-mail: JSTAUDE@AIP.DE * * JStaude@solar.Stanford.EDU * *********************************************************