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The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is being used to observe the extended solar corona from 1.25 to 10 R from Sun center. Initial observations of polar coronal holes and equatorial streamers are described. The observations include measurements of spectral line profiles for HI Lα and Lβ, Ovi 1032 Å and 1037 Å, Mgx 625 Å, Fexii 1242 Å and several others. Intensities for Mgx 610 Å, Sixii 499 Å, and 520 Å, Sx 1196 Å, and 22 others have been observed. Preliminary results for derived H^sup 0^, O^sup 5+^, Mg^sub 9+^, and Fe^sup 11+^ velocity distributions and initial indications of outflow velocities for O^sup 5+^ are described. In streamers, the H^sup 0^ velocity distribution along the line of sight (specified by the value at e^sup -1^, along the line of sight) decreases from a maximum value of about 180 km s^sup -1^ at 2 R to about 140 km s^sup -1^ at 8 R. The value for O^sup 5+^ increases with height reaching a value of 150 km s^sup -1^ at 4.7 R. In polar coronal holes, the O^sup 5+^ velocity at e^sup -1^ is about equal to that of H^sup 0^ at 1.7 R and significantly larger at 2.1 R. The O^sup 5+^ in both streamers and coronal holes were found to have anisotropic velocity distributions with the smaller values in the radial direction.[PUBLICATION ABSTRACT]

The Ultraviolet Coronagraph Spectrometer on the SOHO satellite covers the 940-1350 Aa range as well as the 470-630 Aa range in second order. It has detected coronal emission lines of H, N, O, Mg, Al, Si, S, Ar, Ca, Fe, and Ni, particularly in coronal streamers. Resonance scattering of emission lines from the solar disk dominates the intensities of a few lines, but electron collisional excitation produces most of the lines observed. Resonance, intercombination and forbidden lines are seen, and their relative line intensities are diagnostics for the ionization state and elemental abundances of the coronal gas.The elemental composition of the solar corona and solar wind vary, with the abundance of each element related to the ionization potential of its neutral atom (First Ionization Potential-FIP). It is often difficult to obtain absolute abundances, rather than abundances relative to O or Si. In this paper, we study the ionization state of the gas in two coronal streamers, and we determine the absolute abundances of oxygen and other elements in the streamers. The ionization state is close to that of a log T = 6.2 plasma. The abundances vary among, and even within, streamers. The helium abundance is lower than photospheric, and the FIP effect is present. In the core of a quiescent equatorial streamer, oxygen and other high-FIP elements are depleted by an order of magnitude compared with photospheric abundances, while they are depleted by only a factor of 3 along the edges of the streamer. The abundances along the edges of the streamer ('legs') resemble elemental abundances measured in the slow solar wind, supporting the identification of streamers as the source of that wind component.

Media discourse and public opinion are treated as two parallel systems of constructing meaning. This paper explores their relationship by analyzing the discourse on nuclear power in four general audience media: television news coverage, newsmagazine accounts, editorial cartoons, and syndicated opinion columns. The analysis traces the careers of different interpretive packages on nuclear power from 1945 to the present. This media discourse, it is argued, is an essential context for understanding the formation of public opinion on nuclear power. More specifically, it helps to account for such survey results as the decline in support for nuclear power before Three Mile Island, a rebound after a burst of media publicity has died out, the gap between general support for nuclear power and support for a plant in one's own community, and the changed relationship of age to support for nuclear power from 1950 to the present.

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at = 1.34, but are significantly larger at = 1.5 and much larger for > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least = 2.0, but never reach the values of O VI.[PUBLICATION ABSTRACT]

In this paper we discuss some characteristics of an equatorial streamer observed by UVCS in July 1997. We determine the height distribution of the Ly-[a] total intensity and of its width. We focus our attention, in particular, on the time variability of these parameters.

We made streamer observations with the Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) during the early part of 1998, which was a time of moderate solar activity. We present an empirical study of coronal ion kinetics using the line profiles from these observations. Our first and most striking result is that the mid-latitude (ML) streamers have much narrower O VI 1032 Å line profiles than the solar minimum equatorial (SME) streamers. Our second result is that the line profiles from a small collection of ions in ML streamers do not seem to be consistent with the ions having a single temperature and turbulent velocity. We discuss several interpretations, including line of sight (LOS) effects. This work is supported by the National Aeronautics and Space Administration under grant NAG-3192 to the Smithsonian Astrophysical Observatory.[PUBLICATION ABSTRACT]

With the equivalent area of a 16m telescope, ESPRESSO in 4UT mode allows to inaugurate high resolution spectroscopy for solar-type stars belonging to extragalactic globular clusters. We determine the chemical composition of an extragalactic blue straggler. The star has a G magnitude of 19.01 and belongs to the globular cluster Pal12, that is associated to the Sagittarius dwarf galaxy. Abundances are computed by using high resolution spectroscopy and LTE analysis. Two 50 minutes ESPRESSO spectra, co-added, provide a Signal to Noise Ratio of 25 with a resolving power R=70000. This allows us to measure with good precision abundance of several (13) elements. Li could help to distinguish between formation models of Blue Stragglers; we are able to set a 3 sigma upper limit of Li=3.1, which is still too high to discriminate between competing models. The abundances we retrieve for the BS are compatible with those of giant stars of Pal 12 published in literature, re-analyzed by us using the same procedure and line list. Small differences are present, that can be ascribed to NLTE effects, but for Mg the BS shows a large under-abundance. The most likely explanation is that the BS atmosphere is dominated by gas processed through the Mg-Al cycle, but we have no suitable Al or Na lines to confirm this hypothesis. We show that ESPRESSO with 4UT can be used to derive precise abundances for solar-type stars fainter than magnitude 19. At these magnitudes a proper sky subtraction is needed and in crowded field the targets must be chosen with outmost care, to avoid contamination of the sky fibre from nearby stars.

A theoretical framework is proposed for viewing the process of becoming embarrassed, and hypotheses are derived concerning personality traits which should be associated with greater susceptibility to embarrassment (embarrassability). These hypotheses are tested on 183 male college students by means of a paper and pencil battery of personality scales, one of which was designed for this study to assess embarrassability. Results show that Feelings of Inadequacy is strongly correlated with the Embarrassability Scale, Test Anxiety and Self Esteem moderately correlated, Empathy weakly correlated, and Instability of Self Esteem uncorrelated. The implications of these results for the theoretical framework and for social control are discussed.