By Martin C. E. Huber (auth.), Richard G. Marsden (eds.)

The release in October 1990 of the joint ESA-NASA Ulysses project marked the beginning of a brand new period within the learn of the heliosphere. For the 1st time, in-situ observations are being made protecting the whole variety of heliographic latitudes. Following the profitable gravity-assist manoeuvre at Jupiter in February 1992, Ulysses left the ecliptic airplane in a southerly course and headed again towards the sunlight, passing over the southern sunlight pole in mid-1994. To mark those detailed occasions, the twenty eighth ESLAB Symposium, held in Friedrichs­ hafen, Germany, on 19-21 April 1994, was once dedicated to "The excessive range Helio­ sphere". Following on from the hugely profitable nineteenth ESLAB Symposium "The solar and the Heliosphere in 3 Dimensions" (Les Diablerets, 1985), the aim of the assembly used to be to check out-of-ecliptic effects from the Ulysses project bought so far, and to supply a spotlight for the 1st polar go. proper effects from different house missions, in addition to ground-based and theoretical reports, have been additionally incorporated. Attended via one hundred thirty scientists, the most issues of the Symposium have been The solar and Corona, Large-Scale Heliospheric constitution, vigorous debris within the Heliosphere, Cosmic Rays within the Heliosphere, and Interstellar fuel and Cosmic dirt. The clinical programme consisted of a few Topical evaluate papers introducing a variety of as­ pects of those issues, supplemented by way of a great number of contributed papers (72 in to­ tal) awarded both orally or as posters. surely, the wonderful poster periods shaped one of many highlights of the meeting.

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Extra resources for The High Latitude Heliosphere: Proceedings of the 28th ESLAB Symposium, 19–21 April 1994, Friedrichshafen, Germany

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Ultraviolet spectroscopy also provides information about the velocity distribution, bulk outflow velocity and density of minor ions in the expanding coronal plasma (Kohl and Withbroe 1982; Noci, Kohl, and Withbroe 1987). It is best to combine the ultraviolet spectroscopy with visible polarimetry and in situ measurements of solar wind parameters in order to obtain as complete an empirical description of the expanding corona as possible. In the case of Spartan, there is a companion White Light Coronagraph (Fisher and Space Science Reviews 72: 29-38.

These Proceedings). Data were also available from the HAO Mark III Imaging Coronameter on Mauna Loa and from the NSO/GSFC Disk Spectromagnetograph. Images obtained on 11 April, 1993, are superimposed in Figure 8a. The dotted circles indicate that these instruments can observe the corona to a distance of 6 Ro. The streamer on the SouthEast limb is non-radial and inclined towards the equator at an angle increasing with height. 5 Ro to about 6xl04 cm- 3 at 5 Ro and are typical of those previously observed in such structures with variations of - 25% possibly due to uncertainties in filter calibration.

The most complete coverages were for the helmet streamer at 1350 and for the south polar region. Observations by the Spartan White Light Coronagraph indicate that the north and south polar regions are coronal holes with substructures consisting of polar plumes or rays that extend outward to heliocentric heights in excess of 5 Rev (Guhathakurta, et al. 1994). Figure 2 is a plot of measured HI Lya intensities versus position angle in the south polar coronal hole for heliocentric heights between 1.

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