Modelling accuracy limits for frequency-dependent anisotropy of magnetic susceptibility of rocks and soils

The frequency-dependent anisotropy of magnetic susceptibility (AMS) can be most easily determined through subtracting directional susceptibilities measured at two operating frequencies along each of the measuring directions and the differences subsequently processed using standard methods for AMS computation. The effect of the measurement precision on the accuracy of the determination of the frequency-dependent AMS is investigated through mathematical simulation of the measurement process using the statistical theory of measuring the AMS of rocks. The accuracy of the AMS determination is presented in terms of the errors in determining the principal susceptibilities and principal directions. By modelling the measuring errors, the limits are discovered for the investigation of the frequency-dependent AMS. The modelling shows extremely high requirements for measurement accuracy met by the most sensitive instruments, only.     

The use of the anisotropy of magnetic remanence in the resolution of the anisotropy of magnetic susceptibility into its ferromagnetic and paramagnetic components

The anisotropy of magnetic susceptibility (AMS) is often controlled by both ferromagnetic (sensu lato) and paramagnetic minerals. The anisotropy of magnetic remanence (AMR) is solely controlled by ferromagnetic minerals. Jelínek (Trav. Geophys. 37 (1993)) introduced a tensor derived from the isothermal AMR whose normalized form equals the normalized susceptibility tensor provided that the ferromagnetic fraction is represented by multi-domain magnetite. The present paper shows the close correlation between these tensors for a collection of strongly magnetic specimens containing multi-domain magnetite. In addition, acceptable correlation between the tensors was also found for a collection of specimens containing single-domain magnetite. A new method is developed for the AMS resolution into ferromagnetic and paramagnetic components using the AMR. Some examples are presented of this resolution in mafic microgranular enclaves in granodiorite and in gneisses of the KTB borehole.     

Spatial relations between preflares and flares

We have conducted an initial search for discrete preflare brightenings as observed in soft X-radiation by Yohkoh. The Yohkoh images allow us to identify, to within a few arc seconds, the location of a preflare event relative to the succeeding flare. Our initial motivation in this study was to search for early coronal brightenings leading to flare effects, as had been suggested by earlier studies; thus we concentrated on Yohkoh limb events. We find no evidence for such early coronal brightenings. Between 15% and 41% of the 131 suitable events matched our criteria for preflare brightening: the same active region; brightening within one hour of the flare peak; preflare brightness less than 30% of the flare peak. In the great majority of the preflare cases, we found that physically separate nearby structures brightened initially. Often these structures appeared to share a common footpoint location with the flare brightening itself. In a few cases the preflare could have occurred in exactly the same structure as the flare.     

Flaring arches

We show detailed observations in X-rays, UV lines, and H of an extended arch, about 300000 km long, which developed as a consequence of a compact subflare. This subflare occurred in an included magnetic polarity of relatively low magnetic field strength (compared to that of the sunspots). The apparition of this big arch was preceded by that of a smaller arch, about 30000 km long, which masked the polarity inversion line filament in the early phase of the subflare. The big arch which developed later, around the time of the main X-ray and UV spike of the subflare, connected the included polarity and the main leading sunspot of the region, and became fully developed in a few minutes. The fact that both arches were simultaneously observed in all spectral domains as well as their fine structure in H can only be explained by considering the arch as composed of several unresolved portions of material having widely different temperatures. The H observations can be interpreted as showing the appearance of this cool material as a result of condensation, but a more appealing interpretation is that there was almost simultaneous ejection of superhot (10⁷ K), hot (10⁶ K), mild (10⁵ K), and cool (10⁴ K) material from the subflare site along previously existing magnetic tubes of much lower density. The termination of the subflare was marked by a rather hard X-ray and UV spike which appeared to originate in a different structure than that of the main spike. The material in the arch gradually cooled and drained down after the end of the subflare.Member of Carrera del Investigador, CONICET, Argentina.     

Proton flares in the variation of the auroral electrojet in solar cycle no 21

Summary The effects of the solar proton flare product on ionospheric circumpolar currents (Auroral Electrojet Index) for the interval 1978–1986 (solar cycle No 21) are investigated. A significant increase of the AE two days after the zero-day of appearance of the proton flare was displayed.     

Robust finite-difference scheme for elastic waves on coarse grids

Summary An explicit scheme for 2-D problems of P-SV waves is proposed, 4th order accurate in space and 2nd order accurate in time. The elastodynamic equations are discretized without destroying their self-adjoint nature. Twenty—four effective parameters are introduced at every grid point that make the scheme sensitive enough to spatial variations of the actual Lamé parameters. The scheme is of the same form everywhere, including discontinuities. In particular, also the free surface is described without special formulas; the so-called vacuum formalism is developed. These features make the method simple and widely applicable. However, boundary conditions are only approximately satisfied. Nevertheless, comparisons with independent methods indicate satisfactory results. They include, for example, local Rayleigh waves and bidimensional resonances in basin-like models with strongly curved interfaces of a high velocity contrast (1 : 5), whose principal features were modelled by the present method well.     

Relation between macroseismic intensity and instrumental parameters of strong motions — A statistical approach

One hundred and twenty-eight strong ground motion CALTECH (Earthquakes in the U.S.A., 1940–1971) records of five Californian earthquakes, recorded at ground level and in basements, for which the modified Mercalli macroseismic intensities are known, were statistically processed to calculate 165 wave parameters. Correlation of the peak values of particle acceleration, velocity and displacement, energy, impulse and root-mean-square amplitude of the vibrations, durations of vibrations for certain levels of the peak amplitude, and spectral energies of 10 frequency windows with macroseismic intensity are discussed from the viewpoint of classification of ground-motion records.Paper presented at the 21st General Assembly of the European Seismological Commission held in Sofia 1988.     

X-ray bright surges

We present evidence of X-ray emission from surges that are bright in H. These surges have many features common to flaring arches of Martin and vestka (1988); the basic difference between the two is that in flaring arches cold and hot plasma are injected into clearly defined closed magnetic loops, while in the surges the injection goes into large-scale magnetic field structures of which the second footpoint is usually unknown. Because of the steep density gradient in such large-scale structures, the X-ray visibility of bright surges is limited to a few tens of seconds only. A series of repetitive surges, some of them bright and emitting X-rays, occurred on 8 July, 1980 from footpoints of two large-scale coronal structures, which might have been the legs of an enormous arch at least 600 Mm long.     

Magmatic fabrics and emplacement of the cone-sheet-bearing Knížecí Stolec durbachitic pluton (Moldanubian Unit, Bohemian Massif): implications for mid-crustal reworking of granulitic lower crust in the Central European Variscides

The ∼340 Ma Knížecí Stolec durbachitic pluton was emplaced as a deep-seated cone-sheet-bearing ring complex into the Křišt’anov granulite body (Moldanubian Unit, Bohemian Massif). Prior to the emplacement of the durbachitic magma, the steep sub-concentric metamorphic foliation in the granulite formed due to intense ductile folding during high-grade retrograde metamorphism. Subsequently, the durbachitic pluton intruded discordantly into the granulite at around ∼340 Ma. The steep margin-parallel magmatic fabric in the durbachitic rocks may have recorded intrusive strain during emplacement. After the emplacement, but prior to the final solidification, the pluton was overprinted by the regional flat-lying fabric under lower pressure–temperature conditions (T = 765 ± 53°C; P = 0.76 ± 0.15 GPa). Based on this study and comparison with other ultrapotassic plutons, we suggest that the flat-lying fabrics, widespread throughout the exhumed lower to middle crust (Moldanubian Unit), exhibit major variations in character, intensity, kinematics, and shape of the fabric ellipsoid. These fabrics may have formed at different structural levels and in different parts of the root prior to ~337 Ma. Therefore, we suggest that this apparently “single” orogenic fabric recorded multiple deformation events and heterogenous finite deformation rather than reflecting a single displacement field within the orogenic root.     

Flaring arches

We discuss first the development of the coronal arch-shaped structure of 57000 km length which was born at or before 08:00 UT on 6 November, 1980 and became the site of 13 quasi-periodic brightenings in hard X-rays from 10:00 to 14:30 UT. The same structure became the site of a series of 17 flaring arches between 15:30 and 24:00 UT on that day. The periodicity of 19 min, defined well for the quasi-periodic variations, seems to be partly retained during the occurrence of the flaring arches.The flaring arch studied in Paper I (called SB arch) was the brightest event of this set of events. This paper presents its extended analysis and also an analysis of three other flaring arches that occurred in this configuration. All these events exhibit similar characteristics and thus demonstrate that the flaring arch is a distinct solar phenomenon with specific characteristic properties.A comparison of H, Ov, and X-ray data for the SB arch essentially confirmed, in a quantitative way, the qualitative interpretation of the flow of emitting plasma through the arch proposed in Paper I. In particular, these data show: (1) a hot conduction front producing X-rays in the least dense plasma ahead, a decelerating more dense plasma bulk seen next in Ov, and still more decelerating very dense plasma eventually visible in emission in H; (2) a gradient of densities from the primary towards the secondary footpoint, by factor 3 in X-rays, one order of magnitude in Ov, and probably more in the densest loops emitting in H; (3) the secondary footpoint with hard X-ray spectrum, predominantly excited by particle streams.Member of the Carrera del Investigador, CONICET, Argentina.