IR and UV spectroscopic data for polyynes: predictions for long carbon chain compounds in Titan's atmosphere.

A better understanding of the complex organic chemistry occurring in the methane rich atmosphere of Titan can be achieved via the comparison of observations with results obtained by theoretical models. Available observations are still few but their analysis requires the knowledge of a large set of data, namely frequencies and absolute band intensities. Cross sections are also needed to develop the chemical schemes of photochemical models, in particular the schemes leading to the formation of haze particles visible on Titan. Unfortunately, some of these parameters are not well known, especially if one takes into account the extreme physical conditions of the studied object. This lack of data is particularly enhanced for polyynes because these compounds are highly unstable at the usual pressure and temperature conditions of a laboratory and therefore are very difficult to study. We have developed UV and IR studies, coupling experimental and theoretical approaches, in order to extrapolate the parameters available for short polyynes to longer carbon chains. In the mid-UV range, when the length of the chain increases, the absorption system of polyynes is shifted to longer wavelength and its oscillator strength increases linearly. In the IR range, with the increase of the number of carbon bonds, the positions of the CCC and CCH bending modes shift to lower energy, the latest converging rapidly to a fixed value of 620.5 cm-1 for an infinite length polyyne. Implications for detection and evolution of polyynes in Titan's atmosphere are emphasised.     

The ion energy and mass analyzer on board the ‘Intercosmos-Bulgaria-1300’ satellite

An original instrument for ion energy distribution measurement in ionospheric plasma above the F-layer was designed and launched on board the ‘INTERCOSMOS-BULGARIA-1300’ satellite. The instrument performs differential energy analysis of ion species within the two energy ranges of 1 – 27 eV/q and 0.2–8keV/q.     

Observability analysis of piece-wise constant systems. I. Theory

For pt.II see ibid., vol.28, no.4, p.1068-75, Oct. 1992. A method for analyzing the observability of time-varying linear systems which can be modeled as piece-wise constant systems (PWCS) is presented. An observability matrix for such systems is developed for continuous and discrete time representations. A stripped observability matrix (SOM) is introduced which simplifies the analysis in cases where the use of this matrix is legitimate. The observability analysis is presented as a step-by-step procedure     

Behavior of Japanese tree frogs under microgravity on MIR and in parabolic flight.

Japanese tree frogs (Hyla japonica) were flown to the space station MIR and spent eight days in orbit during December, 1990. Under microgravity, their postures and behaviors were observed and recorded. On the MIR, floating frogs stretched four legs out, bent their bodies backward and expanded their abdomens. Frogs on a surface often bent their neck backward and walked backwards. This behavior was observed on parabolic flights and resembles the retching behavior of sick frogs on land--a possible indicator of motion sickness. Observations on MIR were carried out twice to investigate the frog's adaptation to space. The frequency of failure in landing after a jump decreased in the second observation period. After the frogs returned to earth, readaptation processes were observed. The frogs behaved normally as early as 2.5 hours after landing.     

Hydromagnetics of the magnetosphere

Different models of the magnetosphere are discussed critically. It is pointed out that there is a principal difference between the case when the impinging interplanetary plasma has no initial magnetization, B ₀ = 0, (as in the Chapman-Ferraro theory), and the case when the plasma is initially magnetized, B ₀ 0, even if B ₀ is very small.In the former case the plasma remains unmagnetized (like a superconductor) and cannot penetrate into the magnetosphere. Therefore the plasma is separated by a sharp boundary from the magnetosphere, (closed magnetosphere model).In the latter case when the plasma is magnetized (which is more realistic) there is a possibility that field lines run from the earth to infinity (open magnetosphere model). Particles from the interplanetary space may penetrate into the magnetosphere. At the same time there may be a number of discontinuity surfaces of different character, such as the Cahill discontinuity.It is important to make terrella experiments in order to study the complicated phenomena occurring when a magnetized plasma penetrates into a dipole field.     

Intense magnetic fields in astrophysics

In this paper we summarize the current knowledge of research on the influence of intense magnetic fields on physical processes. The contents are summarized in the enclosed Table of Contents.NAS-NRC Senior Postdoctoral Resident Research Associate.Also with Physics Dept. and Earth and Space Sciences Dept., State University of New York at Stony Brook.     

Suppression of Weibull-Distributed Clutters Using a Cell-Averaging LOG/CFAR Receiver

The parameters of the Weibull distribution and the threshold level for an adaptive CFAR detector are determined by calculating the mean value and the mean-squared value of the input signal voltage before it passes through a logarithmic amplifier. By using this threshold level an adaptive method for suppressing various VVeibull-distributed clutters is proposed.     

Dynamical behaviour of the corona in association with radio emissions

From a combined analysis of radioheliographic observations and white light images of the Corona, it is shown that metric continua onsets or enhancements are associated with a great variety of dynamical changes of the Corona. It is found that if the most spectacular radio bursts (type IV) are associated with mass ejection transients, the more common noise storm onsets or enhancements are systematically associated with coronal changes which are not necessarly mass ejections.Simultaneous observations of Radio type III bursts and Hα mass ejecta are related. We are looking to the signature at low levels in the corona of the electron beam acceleration triggering type III bursts. The results deal with the relationship between the type III occurrence and optical features : the presence of velocities in Hα, the shape of Hα line which reveals trubulent motions and the probable existence of a shock wave.     

Comparison of subpeak electron density profiles deduced from ionograms with the International Reference Ionosphere (IRI)

A comparison is made between the subpeak electron density profiles, obtained at selected local hours by vertical ionospheric sounding at the ionospheric station at Sofia (42.6°N; 23.3°E) and the IRI profiles for spring, summer, winter and two levels of solar activity (R = 10 and 100). It is demonstrated that the ionospheric profiles above Sofia are in rather good agreement with the values computed with IRI.     

On-line Vehicle Motion Estimation from Visual Terrain Information Part II: Ground Velocity and Position Estimation

An algorithm, combining velocity/height estimates, obtained from an airborne body fixed image shift estimator with auxiliary on-board measurements and sparsely stored terrain profile information constitutes an entirely passive autonomous navigation system suitable for moderate-g flight missions. Two versions are addressed. The "naive estimator," in which altitude estimates are multiplied by velocity/height estimaters, yields ground velocity. Position, obtained by integration, diverges with time. The "extended Kalman filter" (EKF) version, in which velocity and position are defined as state space components, locks on the stored terrain profile and does not diverge with time. It degenerates into the "naive estimator" if the terrain is completely flat. Numerical examples indicate excellent performance potential of the EKF estimator.