On the uniqueness of the determination of the coronal potential magnetic field from line-of-sight boundary conditions

We consider a simple model in which the coronal magnetic field B is assumed to be potential in the region between the solar surface _o and an exterior source-surface ₁ of arbitrary shape. We prove that the boundary value problem that determines B from the value B _lof its component on ₀ along either (orthoradial direction) or (fixed direction) has at most one solution. On the other hand, we show that a solution can exist only if B _lsatisfies some solubility conditions.     

Resonant asteroids between the main belt and Jupiter's orbit

Selected orbits of asteroids close to the 3/2 and 4/3 resonances in the outer belt are studied by extended numerical integrations of the four-body problem Sun-Jupiter-Saturn-asteroid. Jupiter's variable eccentricity causes strong or dominant effects in the asteroidal eccentricity, rate of perihelion, and critical argument. However, a suitable transformation removes most of these effects by the transition to respective new quantities. Cases of circulation can change to permanent libration in the new critical argument. This happens in the case of (1256) Normannia, one of the two objects found to be circulating near the 3/2 resonance in former work. The other object, (334) Chicago, remains a case of circulation and shows significant deviations from quasi-periodic motion, contrary to all the other studied Hildas (3/2 cases) and to (279) Thule (4/3). Temporary libration with respect to a resonance of high order is visible in the long-period evolution of Chicago's orbit. There are cases of some analogy further inward in the belt: (903) Nealley changes to permanent libration at the 2/1 resonance by the use of the new critical argument, and (522) Helga's orbit shows a non-quasi-periodic behaviour.     

The light curved in the CM field

In this paper we introduce the CM field in Sections 2 and 3 based on the paper by Wang and Peng (1985), and calculate the light curved in the CM field in Section 4. The result shows thatP makes _CM larger than _C at , and smaller at . Under a special circumstance which source, CM lens, and observer are in the same line, if we get | ₀₌₀ , and | _=/2 , we can determine theP(M) andQ(M) of the CM lens,M is the mass of the CM lens.     

Near-infrared observations of the peculiar binary system epsilon Aurigae

Near-infrared photometric and low-resolution spectroscopic observations of Aurigae at two phases during the current eclipse are presented. The eclipse depths are found to be wavelength-independent in the infrared right up to 2.5 m. There is no infrared excess at wavelengths shorter than 2.5 m. The light absorbing particles in the eclipsing body must be larger than 10 m in size.     

Intercomparisons of earth gravity models by means of lumped coefficients: Terms for eccentricity and longitude

The comparisons of the Earth gravity field models by the order of their harmonic coefficients, performed with the basic lumped coefficients (Planet. Space Sci.29, 653, 1981, Paper I) are here extended to cover all harmonic coefficients (both odd and even degree). The lumped coefficients (the “e-terms” and “longitudinal” terms), corresponding to 18 Earth models, are compared mutually (Figs. 2–15). The large differences, observed for various models and orders, are of particular interest: they are gathered into Table 1. The result of Paper I was a little pessimistic. The same is true here: various inhomogeneities, sometimes very large, in the accuracy of the harmonic coefficients must exist—even for low orders. Most of our comments and objections, however, relate to the older Earth models, which have only a historical value now. Our comparisons are only relative ones; an actual test of the accuracy of the models (their calibration) is possible via data with independent status (Kloko?ník, 1982, 1983).     

A survey of Saturn''s Northern Hemisphere from 1979 to 1987

A photographic survey in four spectral regions (ultraviolet, blue, visible and red) of the Northern Hemisphere of Saturn's atmosphere, has been carried out between 1980 (epoch of the edgewise apparition of the rings) and 1987 (ring's maximum aperture), with the aim of analyzing the changes in the cloud morphology and reflectivity with respect to the spacecraft aspects in 1979 (Pioneer 11) and 1980–1981 (Voyager 1 and 2). Very few variations were detected in the meridional position of the belts and zones ; only a shift of 4000 km toward the North appeared to occur in 1984 in ultraviolet light to the region at latitude 46°N (occupied in 1980–1981 by the “ribbon” feature). Other belts and zones remained stable to ground-based telescopic resolution during the whole period. An increase of 7% in the reflectivity ratio of the belt NEB and the zone EZ, was noted in the spectral interval from 4000 to 6500 Å last year. This can be attributed to the seasonal insolation variation.     

Non-uniform propagation of weak waves through thermally-conducting and dissociating gases

Non-uniform propagation of weak discontinuities headed by wavefronts of arbitrary shape along bi-characteristics of a hyperbolic system through thermally-conducting and dissociating gases are studied. An explicit criterion for the growth and decay of weak waves along bi-characteristic curves in the characteristic manifold of the governing differential equations is given. The two fundamental theorems on the global behaviour of the time-dependent wave amplitude of a weak wave has been concluded.     

Surface heat fluxes and subsurface heat content at a site over the southeastern Bering Sea shelf, May–July 1996

Observations from a surface mooring, in a weak-flow regime over the southeastern Bering Sea shelf, were used to derive surface heat fluxes for the period May–July 1996. Changes in heat content of the water column also were determined from subsurface temperature measurements. Agreement of net surface heat flux and change in heat content was within 2%. This result provides additional evidence that heat advection and diffusion are small in this region.     

The motion of a 9.1 m yacht hull buoy moored in open sea

A 9.1 m yacht hull was instrumented to measure its three-dimensional motion when moored in the open sea. The hull was deployed on three occasions for a total period of about 2 months and encountered a wide range of wind-wave conditions including a strong gale. The data have been analysed to give the response for each component of motion in terms of amplitude and relative phases. The hull motion is compared spectrally to the waves observed by a nearby Waverider. The hull was found to behave as a surface-keyed buoy, with a well defined response for a wide range of conditions. The presence of a resonance in pitch and roll is evident in the data with typical rms values being 5° and 10°, respectively, for significant wave height of 5 m. From data on the mooring dynamics it is concluded that the peaks observed in the tension are a result of the viscous drag opposing the change in the catenary of the mooring and the slow drift oscillations of the buoy. This type of hull is a versatile and economical candidate as a platform for meteorological and oceanographic instrumentation.