Differential rotation of coronal holes

Using KPNO helium 10830 Å synoptic charts of Carrington rotations 1716 through 1739, and by assembling a time sequence representing single latitude zone, rotational properties of coronal holes for five zones of latitudes (±10°, ±20° – ±40°, and ±40° – ±60°) have been examined. It seems that the rotation period of coronal holes is a function of latitude, thus reflecting differential rotation of coronal holes.     

(A-X) system of SiO in sunspots

The calculated equivalent widths of some lines of SiO in the umbral spectrum suggest that strong lines of Si²⁸O¹⁶, Si²⁹O¹⁶ and Si³⁰O¹⁶ may be present in the sunspot ultraviolet spectrum. We also find that between 37 000 and 47 000 cm^–1 the quasi-continuous absorption of SiO dominates all other absorptions.     

Molecules in the solar photosphere

A consideration of the dissociation equilibrium of diatomic molecules in the Utrecht Reference Photosphere leads us to conclude that SH, SiO, CS, HF and HCl may show up in enough concentrations in the solar atmosphere. The number above photosphere for these molecules is comparable with or more than that of MgH.     

A study of massive classical polytropes in general relativity

A detailed study of classical polytropes in general relativity has been presented for _O ((dP/dE)_O) 1.0 and _O((P/E _O)_O. The behaviour of various structural parameters with _O/_O, _O and _O are the values ofP/E and dP/dE at the centre) has been studied. The most important result of this study is the fact the qualitative behaviour of all the structural parameters depends only on the value of µ_O for the various assigned _O values. The maximum value of surface red shift occurs when µ_O=0.6 and for _O=1.0 it equals 0.618. These structures are gravitationally bound for µ_O0.8 and most so for µ_O=0.4. The maximum value of binding coefficient comes out to be 0.181 when _O=1.0. These structures have been used to model neutron stars. The maximum mass of neutron star based upon such a model comes out to be 2.55M (for µ_O=0.4 and _O=1.0) and maximum size comes out to be 15.0 km (for µ_O=0.2 and _O=1.0). It is also seen that the structures are pulsationally stable for µ0.6.     

Physically realizable relativistic stellar structures

Relativistic stellar structures can be obtained both analytically and by computation, but all these models do not stand the tests of physical reality. It is shown that for a physically reasonable solution d/dr -r and d(e ^v /dr r near the centre, d(P/)/dr<-0 and (dP/d)>-(P/). If we change the variabler tox=Cr ², whereC is a constant, the field equations are reduced to a form which is easier to solve. A new set of exact solutions is obtained by consideringe ^v (1-x) ⁿ . Also, a method has been given to obtain generalized solution.It is shown that the solution discussed by Durgapal and Rawat (1980) is the only exact solution which in its most generalized form for a given density distribution stands all the tests of physical reality and for which both (P/) and (dP/d) decrase with increasing value ofr.Neutron star model is proposed by assuming >-2×10¹⁴g cm^–3. Two specific cases are considered, viz.,P<-1/3 and dP/d<-1, respectively. The structures are found to be bound and stable under radial perturbations. The models have been studied for slow rotation and the mass of the Crab pulsar has been estimated for different mechanisms.     

Use of aerial photo-interpretation techniques for land evaluation of a part of Bolangir district,Orissa

The land evaluation has been of paramount importance for the planned development and resource utilization of an area, specially for locating better potential zones for increasing agricultural production. Large areas in the country are yet to be evaluated based on their productivity and potentiality. A case study was undertaken in a part of Bolangir district of Orissa, by using small scale aerial photographs.     

Satellite remote sensing in soil resource inventory of Dibrugarh district (part), Assam

Remote sensing techniques have been employed to identify and delineate soils in a part of Dibrugarh district of Assam. Landsat-4 MSS data in the form of FCC (4, 5, 7) were interpreted visually for physiographic analysis in conjunction with Survey of India topographic maps. Ground data were translated in terms of soils using composite interpretation map as base. The abstraction level attained was Families of Soil Taxonomy. Four major physiographic units were delineated, viz. active flood plain, recent alluvial plain, gently undulating old alluvial plain and gently sloping to undulating piedmont plain. Dominant soils identified are: coarse loamy Aeric Fluvaquents and fine loamy Typic Udifluvents in active flood plain; fine Typic Haplaquepts and fine loamy Aquic Dystrochrepts in recent alluvial plain; fine loamy Umbric Dystrochrepts and fine Ultic Hapludalfs in old alluvial plain; coarse loamy Typic Udorthents and fine Mollic Hapludalfs in piedmont plain.     

Isotopic lines of SiO in sunspots

As the isotopic shift for the vibration rotation band is generally much larger than the isotopic shift for the corresponding electronic transitions and thus facilitating separation of isotopic lines, the vibration rotation bands of SiO may find use in the determination of isotopic abundance ratio Si²⁸ Si²⁹ Si³⁰. To help identify the isotopic lines of SiO the wavenumbers for Si²⁹O¹⁶ and Si³⁰O¹⁶ have been calculated with an uncertainty of ±0.05 cm^–1.Taking note of the fact that SiO shows strong vibration rotation bands in the spectra of some cool stars the equivalent width calculations for P(40) and R(40) lines of the 1-0 and 2-1 vibration rotation bands of Si²⁹O¹⁶ and Si³⁰O¹⁶ have been made at the centre of the disc for the model ZSM-74 using two values of isotopic abundance ratio and three values of dissociation energy.The search for the isotopic lines of SiO near 7 to 8m is recommended in low noise centre to limb sunspot spectrum scans with a view to help improve the isotopic ratio Si²⁸ Si²⁹ Si³⁰ and oscillator strengths for the vibration-rotation transitions.     

Deformation of the rocks of Simla Hills

Simla Hills form a part of Lesser Himalaya. Metamorphic rocks of this area (Pre-Cambrian), forming Chail-Jutogh nappe, are thrust over a series of mostly unfossiliferous rock formations ranging in age from Palaeozoic to Eocene. The rocks of the area are characterised by meso-structures belonging to three phases of deformation. The second phase structures, both in the allochthon as well as in the para-autochthon units are synchronous with the nappe formation. The third structure in the para-autochthon unit has been related with the movement of nappe. A model explaining the probable kinematics of thrusting in the Simla Hills has been suggested.

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Zusammenfassung Die Simla-Berge sind ein Teil des Lesser Himalaya. Metamorphe Gesteine dieses Gebietes (Präkambrium), die die Chail-Jutogh-Decke bilden, sind über einer Serie vorwiegend fossilfreier Formationen (Paläozoikum bis Eozän) überschoben. Die Gesteine dieses Gebietes sind durch Meso-Strukturen, die zu drei Phasen der Deformation gehören, gekennzeichnet. Die Strukturen der zweiten Phase, zu der allochthone sowie para-autochthone Einheiten gehören, sind gleichaltrig mit der Anlage der Deckenbildung. Die Strukturen der dritten Phase in der para-autochthonen Einheit hängen mit der weiteren Bewegung der Decke zusammen. Ein Modell, das die wahrscheinliche Kinematik der Überschiebung in den Simla-Bergen erklärt, wird vorgeschlagen.

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Résumé Les monts Simla représentent une partie du « Lesser Himalaya ». Les roches métamorphiques de cette région (Précambrien), formant la nappe du « Chail-Jutogh », ont glissé par-dessus une série de formations (du Paléozoique à l'Eocène) en majorité dépourvues de fossiles. Les roches de cette région sont caractérisées par des interstructures appartenant à trois phases de la déformation. Les structures de la 2^e phase, auxquelles appartiennent les unités allochtones et para-autochtones se sont formées en même temps que la nappe. Les structures de la 3^e phase, dans l'unité para-autochtone, sont en rapport étroit avec le déplacement postérieur de la nappe. Une possibilité d'explication de la cinématique probable du glissement dans les monts Simla est proposée.

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Simla Lesser Himalaya. — —, Chail-Jutogh, , - . -, . - , - , . - . , , , .

     

Lamprey (Geotria australis; Agnatha) reddening syndrome in Southland rivers,New Zealand 2011–2013: laboratory findings and epidemiology,including the incidental detection of an atypical Aeromonas salmonicida

From 2011, lamprey (Geotria australis) populations in Southland, New Zealand have been affected by reddening along the length of the body and increased mortalities, termed lamprey reddening syndrome (LRS). Molecular testing, bacteriology, histopathology and epidemiology were used to determine if an infectious agent was present and to increase the understanding of this syndrome. An atypical Aeromonas salmonicida was detected from affected lamprey in 2011. This organism has not previously been reported from New Zealand. Investigative molecular testing indicated the organism was an uncharacterised, unculturable, atypical A. salmonicida and a likely incidental finding. Histopathology did not indicate an infectious process was involved, but suggested the reddening may be due to blunt trauma. Epidemiological investigation found the Mokoreta River had a significantly higher prevalence of LRS than others in the Southland region, but there was no clear reason why. To date, no infectious aetiology for this syndrome has been identified.