Fine structure of a solar flare region at 3.7 and 11.1 cm wavelengths

On June 9, 1973, a flare associated burst was observed with the NRAO 3-element interferometer at 3.7 and 11.1 cm wavelength. The burst was of gradual rise and fall type. Comparing the fringe amplitudes at 3.7 cm to the visibility computed for model flare regions we found that the precursor data are best fitted by a region of 3 in size while at the time of the peak, the flare appears to have a size of 2. During the post-maximum phase a size of 5 is the best estimate. Similar computations have been done for 11.1 cm data. The peak brightness temperatures are 1.2 × 10⁹ K and 1.65 × 10⁸ K at 3.7 and 11.1 cm respectively. Such high temperatures would imply that a significant fraction of the burst radiation has a non-thermal origin.     

Active region magnetic fields inferred from simultaneous VLA microwave maps,X-ray spectroheliograms,and magnetograms

A series of VLA maps at 6 cm wavelength have been generated from observations of a solar active region (NOAA 2363) on 29 and 30 March, 1980. During the same period, X-ray spectroheliograms were acquired for this region in the lines of O viii, Ne ix, Mg xi, Si xiii, S xv, and Fe xxv, with X-rayn Polychromator (XRP) aboard the Solar Maximum Mission (SMM). Intervals of relative quiescence (i.e., when X-ray flares and centimeter wave bursts were not evident) were selected for microwave mapping. The resulting VLA maps have spatial resolution of 4 × 4, and generally show two or more sources whose slowly evolving substructures have spatial scales of 10–30. These maps were co-registered with H photographs (courtesy of AF/AWS SOON, Holloman and Ramey AFB) to an accuracy of ± 8. Similarly, the X-ray spectroheliograms have been co-registered with white light photographs to about the same accuracy. Magnetograms from KPNO and MSFC have also been co-aligned, and the magnetic X-ray, and microwave features compared. In general we have found that (a) the peaks of X-ray and 6 cm emission do not coincide, although (b) the sources in the two wavelength domains tend to overlap. These facts in themselves are evidence for the existence of opacity mechanisms other than thermal bremsstrahlung. In order to quantify this assertion, we have computed differential emission measures to derive densities and temperatures. Using these and calculated force-free magnetic fields from Kitt Peak magnetograms, we present an assessment of the mechanism of gyroresonance absorption at low harmonics of the electron gyrofrequency as the source of opacity responsible for the microwave features. We conclude that large-scale currents must be present in the active region loops to account for the bright 6 cm sources far from sunspots.Lockheed Missiles and Space Company, Palo Alto: currently at GSFC.Currently at NASA/MSFC.     

Time variability and structure of quiet Sun sources at 6 cm wavelength

Using the Westerbork Synthesis Radio Telescope (WSRT) we produced a synthesized map of a quiet Sun region on June 15, 1976, and studied the structure and time variability of the quiet emitting regions at 6 cm wavelength with a spatial resolution of 6 arc sec. Comparison of the 12hr synthesis map with Ca⁺ K filtergram shows that bright and dark features on the 6 cm quiet Sun synthesized map correspond to the chromospheric networks and cells observed in Ca⁺ K. All 6 cm bright features lie over bright Ca⁺ K network elements. The reverse correlation is not true, that is, not all bright Ca⁺ K network features have their 6 cm counterparts. Comparison with the photospheric magnetogram shows that about 72% of the photospheric magnetic field enhancements (¦B¦ 5 G) are coincident with 6 cm emissive regions. Only one 6 cm feature could be positively identified with a bipolar magnetic structure. This implies that no more than 20–25% of the 6 cm emitting features could be associated with X-ray bright points. Intercomparison of our 12hr two-dimensional synthesis map, a 4hr two-dimensional synthesis map (around meridian) and the one-dimensional fan beam scans of the quiet Sun region at 6 cm, along with the Ca⁺ K filtergram and photospheric magnetogram shows that: (1) All of the 15 time-varying elements at 6 cm were located on Ca⁺ K networks; (2) about 40% of the 15 time varying elements at 6 cm are coincident with enhancements of the photospheric magnetogram; (3) individual time-varying sources have minimum source size (FWHM) of 15 arc sec and maximum brightness temperature of 10⁵ K; (4) the life time of the time varying sources varies from a few minutes to several tens of minutes; (5) the intensity of the sources varies by factors of 2 to 7 over time periods of 1 min to tens of minutes; and (6) the sources tend to disappear for periods of up to tens of minutes and to reappear at the same locations.     

Observations of solar filaments at 8, 15, 22 and 43 GHz

On April 3, 4, 6, and 8, 1978, solar observations were made using the Haystack 120 ft telescope at 8, 15, 22, and 43 GHz. H filtergrams obtained at the Sacramento Peak Observatory on the same days showed an average of more than 30 filaments or filament fragments (per day) on the disk. Most of these appeared as depressions in brightness temperature at 15 and 22 GHz. Because of the relatively low spatial resolution at 8 GHz, only a few appeared at that frequency, and presumably because of lower opacity in filaments at higher frequencies, few depressions were visible at 43 GHz. At 15 and 22 GHz, more depressions appeared than H filaments, but virtually all the radio depressions overlay magnetic neutral lines. Taking the data sets for each day as independent samples, we found that at 22 GHz, 46 of the 77 radio depressions were associated with H filaments; at 15 GHz the correlation was smaller; only 27 out of 48 being associated with the H filaments. The data imply that the microwave depression features are the result of absorption by filaments and perhaps also the result of other effects of the associated filament channel, but not necessarily coronal depletion. The effects of filament absorption are, statistically, about twice as effective as other phenomena (such as absorption by material invisible in H, for example) in creating the radio depression. A center-to-limb study of a single large filament clearly showed that at 15 and 22 GHz the absorption by cool hydrogen supported above the neutral line was the predominant factor in producing the observed depression at radio frequencies.     

Sharp edges in solar microwave spectra: Neutral current sheets or cyclotron lines?

We have mapped two solar active regions using the VLA at three closely spaced frequencies (4496, 4716, and 4996 MHz) in an attempt to determine the origin of the steep spectra (index –5 to –8) sometimes observed with large single telescopes. One of the regions observed indeed shows an anomalously large slope ( –6) compared to the usual ( –2 to –2.5). The other region shows a similar slope ( –5) but with a larger range of statistical error. Two possible explanations for such steep edges in solar spectra are (1) transmission effects of neutral current sheets, and (2) the appearance of cyclotron lines. The internal evidence of the microwave maps and simultaneous optical observations favor an explanation in terms of cyclotron lines.On leave from Indian Institute of Astrophysics, Bangalore, India.     

The change of shape of a viscous ellipsoidal region embedded in a slowly deforming matrix having a different viscosity

The general theory of the elastic fields round ellipsoidal inclusions and inhomogeneities is applied to solve the problem of the slow deformation of a viscous material containing an ellipsoidal inhomogeneity of different viscosity. The theory is used to calculate the twodimensional finite strain of an elliptic cylinder and of prolate and oblate spheroids under applied pure-strain rates, and attention is drawn to applications in the fields of rock deformation and in the mixing and homogenization of viscous liquids.     

Salinity Tolerance and Salinity Induced Changes in Ionic and Metabolite Composition in a Penaeid Prawn,Parapenaeopsis sculptilis (Heller)

Summary: Experiments were carried out to study the salinity tolerance and the impact of salinity changes on ions and metabolite in the body of a marine penaeid prawn, Parapenaeopsis sculptilis. Juveniles of this prawn species have a comparatively wide range of salinity tolerance than adults. Juveniles can tolerate 60 … 100 %, but adults only 100 % seawater concentrations. Behavioural observations showed that the juvenile and adult prawns became inactive with decrease in seawater concentrations followed by paralysis and death. Death occurred probably due to failure of the neuromuscular system. A highly significant variation existed in the amount of sodium, potassium and calcium ions in juveniles as well as adults. Exposure to different seawater concentrations probably caused breakdown of the osmoregulatory mechanism in the prawn body. Protein and carbohydrate decreased in both juvenile and adult prawn body, with the decrease in seawater concentrations indicating the utilization of large amounts of protein and carbohydrate from the internal reserve.     

Nayagarh氟化物污染区土壤的地球化学性质：因素分析评价

本文旨在研究奥里萨邦[印度邦名]Nayagarh区温泉地带土壤受氟化物污染的情况。文中分析两种土壤（大部分是在0-30cm深度采集的土壤以及0-90cm深度采集的剖面土壤）的总氟化物浓度（Ft）和0．01MCaCl2可萃取的氟化物浓度（Fca）主要的元素、pH、EC以及有机碳。通过对Singhpur村周围区域和温泉的观察，结果表明Ft和Fca浓度都高。大部分土壤参数的主要因素分析（PFA）表明，两种主要的化学过程是由于三个因素控制区域土壤的地球化学性质。第一个因素占总变化的37．11％，对Al、Si、Fe、F。和F。有很强的载荷能力，而且说明了土壤富集氟化物的原因；而第二和第三个因素分别占16．6％和12．2％，说明碳酸盐沉淀的控制过程和土壤的碱度。对因素做多元回归分析是为了取得土壤的氟化物污染指数。因素影响范围的大小（因素-1〉因素-2〉因素-3）影响污染指数。污染指数的空间分布可以用来划分污染区域的污染等级，即：高度污染区、中度污染区和未污染区。     

Transient sonar signal classification using hidden Markov modelsand neural nets

In ocean surveillance, a number of different types of transient signals are observed. These sonar signals are waveforms in one dimension (1-D). The hidden Markov model (HMM) is well suited to classification of 1-D signals such as speech. In HMM methodology, the signal is divided into a sequence of frames, and each frame is represented by a feature vector. This sequence of feature vectors is then modeled by one HMM. Thus, the HMM methodology is highly suitable for classifying the patterns that are made of concatenated sequences of micro patterns. The sonar transient signals often display an evolutionary pattern over the time scale. Following this intuition, the application of HMM's to sonar transient classification is proposed and discussed in this paper. Toward this goal, three different feature vectors based on an autoregressive (AR) model, Fourier power spectra, and wavelet transforms are considered in our work. In our implementation, one HMM is developed for each class of signals. During testing, the signal to be recognized is matched against all models. The best matched model identifies the signal class. The neural net (NN) classifier has been successfully used previously for sonar transient classification. The same set of features as mentioned above is then used with a multilayer perceptron NN classifier. Some experimental results using “DARPA standard data set I” with HMM and MLP-NN classification schemes are presented. A combined NN/HMM classifier is proposed, and its performance is evaluated with respect to individual classifiers