Study of the Source Regions of Coronal Mass Ejections Using Yohkoh SXT Data

The scientific objective of the program was to better understand how CMEs (Coronal Mass Ejections) are initiated at the sun by examining structures on the disk which are related to the origins of CMEs. CMEs represent important disruptions of large-scale structures of closed magnetic fields in the corona, and result in significant disturbances of the interplanetary medium and near-Earth space. The program pertained to NASA's objectives of understanding the physics of solar activity and the structured and evolution of the corona, and the results are being applied to understanding CMEs currently being observed by SOHO near the sun and by WIND and Ulysses in the heliosphere. Three general areas of research were pursued in the program. One was to use Yohkoh soft X-ray telescope (SXT) images of eruptive events visible against the solar disk to examine the coronal structures and the boundaries of the large-scale magnetic fields considered to be involved in coronal mass ejections (CMEs). The second area involved a survey and study of SXT X-ray arcade events which exhibit dimming, or the possible depletion of coronal material above and possibly before onset of the bright long-duration event (LDE). Finally, we studied the SXT data during periods when white light CMEs were observed the HAO Mauna Loa K-coronameter and, conversely, we examined the white light data during periods when expanding X-ray loops were observed at the limb

Variations of Heavy Ion Abundances Relative to Proton Abundances in Large Solar Energetic (E \u3e 10 MeV) Particle Events

The elemental composition of heavy ions (with atomic number Z \u3e 2) (hi-Z) in large gradual E \u3e 10 MeV nuc-1 SEP events has been extensively studied in the 2-15 MeV nuc-1 range to determine the acceleration processes and transport properties of SEPs. These studies invariably are based on abundances relative to those of a single element such as C or O and often neglect H and He, the elements of primary interest for space weather. The total radiation of an SEP event is determined not only by the H and He properties but also by those of hi-Z ions whose abundances and variations relative to H from one event to another are unknown. We report a study to determine those variations in a group of 15 large SEP events over the period 2000 to 2015. Five hi-Z ions (He, C, O, Mg, & Fe) were selected to determine variations of their fluences relative to those of H in the 13.5-50.7 MeV nuc-1 energy range for each SEP event. Our average hi-Z abundance ratios slightly exceed those reported by [1] at lower energies, with the Fe event abundances showing the largest standard deviation of an order of magnitude. The event abundances were weakly correlated with H fluences and strongly correlated with speeds Vcme of associated coronal mass ejections (CMEs). These correlations may be evidence of streaming limits in the shock regions of H in the largest events

DETECTION AND DIAGNOSTICS OF A CORONAL SHOCK WAVE DRIVEN BY A PARTIAL-HALO CORONAL MASS EJECTION ON 2000 JUNE 28

A fast partial-halo coronal mass ejection (CME) was observed on 2000 June 28 by instruments on the SOHO spacecraft. The CME leading edge and filamentary cold core were detected over the northwest limb at 2.32 R? by the SOHO UV Coronagraph Spectrometer (UVCS). The broad profile of the O?VI ?1032 line gives evidence of a shock front at the leading edge, supporting the identification of white-light CME sharp leading edges as fast-mode shocks. Line-of-sight speeds are as high as 1500 km s-1, comparable to the projected speed obtained from LASCO. Pumping of the O?VI ?1032 by Ly? (v = 1810 km s-1) and of O?VI ?1037 by O?VI ?1032 (v = 1648 km s-1) were detected, which provide diagnostics of outflow speed and density. The angle of the ejecta with the plane of the sky is obtained, combining the projected speed from LASCO with the line-of sight-speed, and varies between 7? and 46?. In the latter case the projected height of 2.32 R? was at an actual heliocentric distance of 3.6 R?. An associated solar energetic particle (SEP) event was observed at the L1 point following this CME. The abundance and charge-state data are consistent with a gradual shock-accelerated SEP event. A type II radio burst was observed at the same time the shock front was detected by UVCS

International Perspectives on Nonformal Education

The New England Regional Meeting of the Comparative and International Education Society was held on the campus of the University of Massachusetts, Amherst, on 3 May, 1979. The conference was co-sponsored by the Division of Community Education, Springfield College, and the Center for International Education, School of Education, University of Massachusetts. The theme of the conference was International Perspectives on Nonformal Education. The papers delivered ranged in topics from the use of traditional art forms and poetry as a medium of nonformal education to the discussion of the philosophical foundations underlying the field. Case studies of specific nonformal education projects helped to highlight the conference. A total fifteen papers were delivered, all of which are included in their original form in this document. The papers represent the views of the authors and not necessarily those of the organizers

The solar particle event of July 16–19, 1966 and its possible association with a flare on the invisible solar hemisphere

An energetic solar proton and electron event was observed by particle detectors aboard Explorer 33 (AIMP-1) and OGO-3 during the period July 16–19, 1966. Optical and radio observations of the sun suggest that these particles were produced by a flare which may have occurred on July 16 near the central meridian of the invisible hemisphere. The active region to which the flare is assigned is known to have produced the energetic particle events of July 7 and 28 , 1966. The propagation of the particles in the July 16–19 event over the ∼180° extent of solar longitude from the flare to the earth is discussed, and it is concluded that there must exist a means of rapidly distributing energetic particles over a large area of the sun. Several possible mechanisms are suggested.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/43748/1/11207_2004_Article_BF00150955.pd