RHESSI as a Hard X-Ray Polarimeter

Although designed primarily as a hard X-ray imager and spectrometer, the Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) is also capable of measuring the polarization of hard X-rays (20–100 keV) from solar flares. This capability arises from the inclusion of a small unobstructed Be scattering element that is strategically located within the cryostat that houses the array of nine germanium detectors. The Ge detectors are segmented, with both a front and rear active volume. Low-energy photons (below about 100 keV) can reach a rear segment of a Ge detector only indirectly, by scattering. Low-energy photons from the Sun have a direct path to the Be and have a high probability of Compton scattering into a rear segment of a Ge detector. The azimuthal distribution of these scattered photons carries with it a signature of the linear polarization of the incident flux. Sensitivity estimates, based on Monte Carlo simulations and in-flight background measurements, indicate that a 20–100 keV polarization sensitivity of less than a few percent can be achieved for X-class flares.     

Observations of short period oscillations in two dimensions

Observations of the photospheric velocity field at the disk center with a cadence of five frames per second strongly support the idea that short period oscillations arise from a combination of image motion and horizontal gradients of the line of sight velocity field. Any genuine solar short period oscillations are effectively masked by these false short period oscillations.Operated by the Association of Universities for Research in Astronomy Inc., under contract with the National Science Foundation.Visiting Astronomer, Solar Division, KPNO.     

Report on the solar physics-plasma physics workshop

This report summarizes the proceedings of a meeting held on 17–20 September 1974, at Stanford University. The purpose was to explore plasma physics problems which arise in the study of solar physics. Sessions were concerned with specific questions including the following: Is the solar plasma thermal or non-thermal? What spectroscopic data are required? What types of magnetic field structures exist? Do MHD instabilities occur? Do resistive or non-MHD instabilities occur? What mechanisms of particle acceleration have been proposed? What information do we have concerning shock waves? Very few questions were answered categorically but, for each question, there was discussion concerning the observational evidence, theoretical analyses, and existing or potential laboratory and numerical experiments.     

Measurement of stratospheric aerosol on Saturn using an eclipse of Titan

An eclipse of Titan by Saturn was observed on December 20, 1979, to measure the aerosol content in the atmosphere of Saturn. The measurements were made with the 74-in. telescope of the Helwan Observatory, Egypt, in the bandpass 6300–7300 Å and extend to ～5 magnitudes of eclipse darkening. The faint portion of the lightcurve unambiguously requires the presence of aerosol in the lower stratosphere of Saturn. The aerosol extends to at least 20 km above the tropopause and has a one-way stratospheric vertical optical depth of 0.4_?0.02^+0.04 at 6700 Å. The results apply to the sunset terminator at a cronographic latitude of 23°S.     

THE TIMMERSOI†, NIGER,HYPERSTHENE CHONDRITE

The Timmersoi meteorite, a new type L5 hypersthene chondrite from the Niger Republic is described and microprobe analyses of its olivine, orthopyroxene, clinopyroxene, plagioclase, kamacite, taenite, troilite, chromite, whitlockite, chlorapatite and limonite presented. Veins and patches of black “glassy” material are regarded as products of shock melting. In places this material contains immiscible droplets of troilite each with one or more well-formed crystals of taenite. Calculations indicate equilibrium between olivine and orthopyroxene with a temperature of equilibration of about 850 °C.     

Solar brightness distribution at 3mm wavelength from observations of the eclipse of 1976 October 23

Observations of the Sun were made at 3 mm wavelength during the total eclipse of 1976 October 23. Analysis of the record obtained near third contact indicates that the Sun at this wavelength is slightly limb-brightened, and that the solar radius is 1.007 times the photospheric radius.     

On the relative intensity of second branches of U-like solar radio bursts

The purpose of this note is to examine the suggestion of Fokker (1970) to explain why the second branch of U-bursts is ill-developed and to present an alternate possible explanation which was suggested by an examination of the trajectories derived by him.Postdoctoral Fellow on the U.S.-U.S.S.R. Cultural Exchange     

The formation of solar prominences by thermal instability in a current sheet

The energy balance equation for the upper chromosphere or lower corona contains a radiative loss term which is destabilizing, because a slight decrease in temperature from the equilibrium value causes more radiation and hence a cooling of the plasma; also a slight increase in temperature has the effect of heating the plasma. In spite of this tendency towards thermal instability, most of the solar atmosphere is remarkably stable, since thermal conduction is very efficient at equalizing any temperature irregularity which may arise. However, the effectiveness of thermal conduction in transporting heat is decreased considerably in a current sheet or a magnetic flux tube, since heat can be conducted quickly only along the magnetic field lines. This paper presents a simple model for the thermal equilibrium and stability of a current sheet. It is found that, when its length exceeds a certain maximum value, no equilibrium is possible and the plasma in the sheet cools. The results may be relevant for the formation of a quiescent prominence.     

SHERGOTTY METEORITE: MINERALOGY,PETROGRAPHY AND MINOR ELEMENTS

The unusual achondrite Shergotty resembles terrestrial diabases, and textural and chemical evidence indicates pre-settling and post-settling crystallization of zoned augite (En₄₈Fs₁₉Wo₃₃-En₂₅Fs₄₇Wo₂₈) and pigeonite (En₆₁Fs₂₆Wo₁₃-En₂₁Fs₆₁Wo₁₈) coupled with late crystallization of plagioclase (Ab₄₃An₅₆/Or₁-Ab₅₆An₄₁Or₃: now shocked to maskelynite), titanomagnetite-ilmenite composite grains, mesostasis (normative Qz₃₄Ab₂₁An₅Or₃₈Fs₂, assuming Fe as ferrous), whitlockite, pyrrhotite (Fe_0.94S), fayalite (Fo₁₀), baddeleyite and chlorapatite. The oxide compositions (Usp₆₂Mt₃₈, Al₂O₃ 2.4, Cr₂O₃ 0.8 wt %; Ilm₉₅Hm₅) indicate ～ 850 °C and log oxygen fugacity ? 14, while the occurrence of fayalite rims on mesostasis next to ilmenite indicates 890 °C. Bearing in mind experimental uncertainties, these data are consistent with late-stage crystallization under relatively high oxygen fugacity, as indicated by coexistence of fayalite, Ti-magnetite and a silica glass. The high alkali content of the maskelynite and mesostasis, coupled with the redox state, indicates that the Shergotty meteorite resembles terrestrial basalts more than any other meteorites. Nevertheless the absence of H₂O, as shown by the occurrence of phosphorus in whitlockite rather than in hydroxylapatite, distinguish the Shergotty achondrite from typical terrestrial diabases. Whereas the FeO/MnO ratios of pyroxenes from the Moon, Earth and several differentiated meteorites are independent of FeO, the ratio for Shergotty pyroxenes changes from 30 to 40 with increasing FeO, and the linear trend extrapolates to 0.2 MnO for zero iron. Hence caution is needed in using FeO/MnO as a planetary indicator. For pyroxenes, Na is almost independent of Fe/Mg while Ti increases and Cr decreases with increasing Fe/Mg. Maskelynite contains 0.5–0.25 wt % K₂O, 0.6 wt % FeO, 0.04 TiO₂, 0.04–0.07 MgO, ～ 0.01 BaO and 0.02–0.03 P₂O₅. A bulk analysis calculated from the mode and compositions of the minerals matches quite well with two bulk chemical analyses but not with a third.