Title: International Solar Cycle Study (ISCS) 1998 - 2002
Author: S. T. Wu
Affil: Center for Space Plasma and Aeronomic Research and Department of Mechanical and Aerospace Engineering, The University of Alabama in Huntsville, Huntsville, AL 35899 USA
Email: wus@cspar.uah.edu
Authors: V. Obridko
Affils: IZMIRAN, Troitsk, Moscow Region, 142092, Russia
Abstract: The ISCS is a post-STEP project of SCOSTEP. This project's aim is to study the sun's variability during the rising phase of the 23rd solar cycle. The project consists of three major parts: (i) solar energy flux study, (ii) solar magnetic field variability study and (iii) solar emission. We will summarize briefly the goals and achievements of these topics. Future research programs in these areas to be sponsored by the SCOSTEP will also be discussed.
Title: Solar Energy Flux Study: from the Interior to the
Outer Layers, ISCS WG 1 Report
Author: Judit M. Pap
Affil: Goddard Earth Science and Technology Center, UMBC
Email: papj@marta.gsfc.nasa.gov
Authors: Claus Frohlich
Affils: Physikalisch-Meteorologisches Observatorium Davos
Abstract: ISCS WG1 is dealing with measurements, results, and the interpretation of solar irradiance variations from EUV to infrared and their effect on the Earth's atmosphere and climate system. Since 1998, the start of ISCS, considerable effort has been put into the the measurements and understanding of irradiance changes. Measurements of the SOHO/VIRGO experiment in the entire spectrum and in near-UV at 402 nm, visible at 500 nm and infrared at 862 nm showed that spectral irradiance changes similarly to total irradiance and the effect of active regions are clearly resolved. It has also been shown that both total irradiance and UV irradiance in the vicinity of 280 nm (Mg II h & k core-to-wing ratio) reach about the same level during the maximum of solar cycle 23 than during the previous two cycles. In contrast, the sunspot number and magnetic field has a lower maximum during solar cycle 23. Results from the SOHO/CELIAS/SEM experiment, providing the first continuous EUV data over half a solar cycle, show that EUV irradiance varies similar to the Mg c/w ratio.
Title: Solar Magnetic Field Variability Study: From the Lower Atmosphere to the Inner Corona, ISCS WG2
Author: Richard A. Harrison
Affil: Rutherford Appleton Laboratory
Email: r.harrison@rl.ac.uk
Authors: Don Michels
Affils: Naval Research Laboratory
Abstract: The activities of Working Group 2 have to a large extent been driven by demand from the community. The basic desire has been to disseminate information and arrange relevant scientific meetings. This has been done through a Web site facility and several specific meetings have been arranged under the ISCS banner. Rather than attempt to cover all scientific topics suggested by the title, we have provided a service to a number of large research activities which have made use of the organisation offered. These have included, multiwavelength studies of coronal mass ejection (CME) onsets, investigations of large 'chains' on the Sun, numerical modelling techniques, and the whole Sun month campaigns. Numerous 'hot' topics have been debated within these efforts at the meetings, and these include coronal dimming and coronal waves under CME onsets, the importance of solar sigmoid configurations, and methods for multiwavelength observations and analyis. Particular emphasis has been put on the projection or propagation of solar events into the low corona and outwards, in particular with the study of CMEs onsets, and in this way, the activities interface with Working Group 3.
Title: Solar Emissions: Origins and Transport through the Heliosphere, ISCS WG 3 Report
Author: D. Webb
Affil: Boston College
Email: david.webb@hanscom.af.mil
Authors: G. Simnett
Affils: Univ. of Birmingham, UK
Abstract: The main scientific objective of ISCS Working Group 3 (WG3) is to study the origins and transport of solar emissions through the heliosphere. The emphasis of the group is on observational and theoretical studies of dynamic activity in the mid to outer corona and its influence on the solar wind. Our studies differ from those of Working Group 2 which emphasize observations and modeling of dynamic magnetic field activity in the low solar atmosphere and inner corona. WG3 has three subareas of study: 1) Dynamic solar emissions in the increasing and maximum portion of solar cycle 23; 2) Propagation in the interplanetary medium of transient disturbances, i.e., coronal mass ejections, interplanetary shocks, and energetic particles); and 3) Interaction of coronal mass ejections and solar wind streams with Earth's magnetosphere. We will report on progress that WG3 has made and outline the main topics to be discussed during this meeting.
Title: Storm23 - Chinese Solar Maximum Program
Author: Jingxiu Wang
Affil: Beijing Astronomical Observatory,Chinese Academy of Sciences
Email: wjx@ourstar.bao.ac.cn
Abstract: Storm23 - Solar Activity and Its Terrestrial Effects: Observations and Research in the Maximum Phase of Solar Cycle 23, is a major project funded by The Chinese Academy of Sciences for the period of Solar Maximum 23 systematic observations of catastrophic solar events and their consequences in the space environment, thus, to achieve fundamental progress in understanding the mechanisms of catastrophic solar events and their influence on geomagnetic field, ionosphere, thermosphere, and mesosphere, to develop models of solar and space weather forecast. New instruments have been developed for this major project. Among them, Broadband Spectrometers for Decimeter and Centimeter Wave Burst has been put into full operation, and revealed new phenomena on particle acceleration and propagation in flare process; a Stokes Parameter Telescope is currently in test observations. Great efforts have been made in the studies of Earth-directed coronal mass ejections with the emphasis on identifying the surface sources of CMEs, by combining the space-borne and ground-based vector magnetogram observations. Systematic observations from the solar surface activity to the geospace storms, as well as the disturbance in higher Earth atmosphere have been obtained for a few major solar events. Combined data analysis is undertaken.