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1.
Although numerous factors influence soil-water content, it is considered a key indicator of rangeland health. This paper investigates the effect of grazing on soil-water content using three treatments within the same soil association. The treatments, simulated holistic planned grazing (SHPG), rest-rotation (RESTROT), and total rest (TREST) applied stocking rates of 36, 6, and 0 animal days/hectare respectively. Soil-water content was measured continuously from 2006 to 2008 using 36 capacitance sensors. Statistical analyses revealed differences in percent volumetric-water content (%VWC) and in all treatments, the SHPG pasture had the highest %VWC. Mixed procedures models indicate strong environmental and treatment effects as explanatory variables for the observed difference in %VWC. Although results of vegetation cover analyses indicated no difference in percent shrub cover in the two production pastures (SHPG and RESTROT), percent litter cover differed in the latter years of this study. It was concluded that in addition to a variety of other factors, management decisions (grazing and rest) can have substantial influence upon soil-water content and that soil-water content can vary substantially as a result of animal impact and the duration of grazing. 相似文献
2.
It is known for over two decades now that the rotation of the photospheric magnetic fields determined by two different methods
of correlation analysis leads to two vastly differing rotation laws - one the differential and the other rigid rotation. Snodgrass
and Smith (2001) reexamining this puzzle show that the averaging of the correlation amplitudes can tilt the final profile
in favour of rigid rotation whenever the contribution of the rigidly rotating large-scale magnetic structures (the plumes)
to the correlation dominates over that of the differentially rotating small-scale and mesoscale features. We present arguments
to show that the large-scale unipolar structures in latitudes >40 deg, which also show rigid rotation (Stenflo, 1989), are
formed mainly from the intranetwork magnetic elements (abbreviated as IN elements). We then estimate the anchor depths of
the various surface magnetic elements as locations of the Sun's internal plasma layers that rotate at the same rate as the
flux elements, using the rotation rates of the internal plasma layers given by helioseismology. We infer that the anchor depths
of the flux broken off from the decay of sunspot active regions (the small-scale and mesoscale features that constitute the
plumes) are located in the shallow layers close to the solar surface. From a similar comparison with helioseismic rotation
rates we infer that the rigid rotation of the large-scale unipolar regions in high latitudes could only be coming from plasma
layers at a radial distance of about 0.66–0.68 R
⊙ from the Sun's centre. Using Stenflo's (1991) ‘balloon man’ analogy, we interpret these layers as the source of the magnetic
flux of the IN elements. If so, the IN flux elements seem to constitute a fundamental component of solar magnetism. 相似文献
3.
The degree of convective instability as expressed by the growth rate of linear modes, is calculated for a plane parallel polytropic atmosphere in the presence of radiative damping, without using Boussinesq approximation. A comparison with the results based on the Boussinesq approximation reveals that the use of the Boussinesq approximation leads to an overestimation of the radiative damping. The computation of as a function of the horizontal wave number yields a wavelength of maximal instability under a variety of conditions. For reasonable choices of physical parameters appropriate to the solar atmosphere, the fastest growing wavelengths turn out to be in the range 600–1200 km, and their e-folding times are in the range 200–2000 s.NAS-NRC Senior Research Associate on leave of absence from the Tate Institute of Fundamental Research, Bombay. 相似文献
4.
We show that up to second order in the thinness parameter, the equations of equilibrium of a thin, isolated, axisymmetric, force-free magnetic flux tube in a stratified atmosphere and the other essential constraints form a mathematically closed system. Auxiliary assumptions about temperature of the tube plasma are neither needed nor possible. 相似文献
5.
The acoustic overstability in a polytropic plane-parallel atmosphere with superadiabatic temperature gradient and radiative dissipation is demonstrated for optically thick disturbances. The periods of oscillation are found to be in the range 250–480 s and the associated wavelength of the order of 4000 km. The five-minute oscillations in the solar surface are attributed to self-excited sound waves in a layer in the subphotospheric convection zone of about 1000 km thickness. 相似文献
6.
The stability of a plane-parallel polytropic fluid layer in the presence of a uniform horizontal magnetic field is investigated to explore the possibility of identifying the running penumbral waves and the penumbral filaments with different types of instabilities. 相似文献
7.
M. H. Gokhale 《Journal of Astrophysics and Astronomy》2000,21(3-4):155-160
Data on sunspot groups have been quite useful for obtaining clues to several processes on global and local scales within the
sun which lead to emergence of toroidal magnetic flux above the sun’s surface. I present here a report on such
studies carried out at Indian Institute of Astrophysics during the last decade or so. 相似文献
8.
M. H. Gokhale 《Journal of Astrophysics and Astronomy》1986,7(4):241-257
We present preliminary results of a spherical-harmonic-Fourier analysis of sunspot activity during the twenty-two years 1933–1954.
The results indicate that the sunspot activity might be originating in global solar oscillations with periods of years and
decades. However, except for the axisymmetric mode of degree 6, the set of other axisymmetric modes showing ∼ 11 yr periodicities
are different from one sunspot cycle to another. A more detailed analysis, preferably with larger data series, will be needed
to arrive at a more definite conclusion. 相似文献
9.
We investigate the effects of radiative heat losses and thermal conductivity on the hydromagnetic surface waves along a magnetic discontinuity in a plasma of infinite electrical conductivity. We show that the effects of radiative heat losses on such surface waves are appreciable only when values of the plasma pressure on the two sides of the discontinuity are substantially different. Overstability of a surface wave requires that the medium in which it gives larger first-order compression should satisfy the criterion of Field (1965). Possible applications of the study to magnetic discontinuities in solar corona are briefly discussed.Collaborative programme in Astronomy and Astrophysics, Department of Physics, Indian Institute of Science, Bangalore 560012, India. 相似文献
10.
P. C. Agrawal G. S. Gokhale V. S. Iyengar P. K. Kunte R. K. Manchanda B. V. Sreekantan 《Astrophysics and Space Science》1972,18(2):408-424
Experimental results on the intensity, energy spectrum and time variations in hard X-ray emission from Cyg X-1 based on a balloon observation made on 1971, April 6 from Hyderabad (India) are described. The average energy spectrum of Cyg X-1 in the 22–154 keV interval on 1971 April 6 is best represented by a power law dN/dE=(5.41±1.53)E
–(1.92±0.10) photons cm–2s–1 keV–1 which is in very good agreement with the spectrum of Cyg X-1 derived from an earlier observation made by us on 1969 April 16 in the 25–151 keV band and given by dN/dE=(3.54±2.44)E
–(1.89±0.22) photons cm–2s–1 keV–1. A thermal bremsstrahlung spectrum fails to give a good fit over the entire energy range for both the observations. Comparison with the observations of other investigators shows that almost all balloon experiments consistently give a spectrum of E
–2, while below 20 keV the spectrum varies fromE
–1.7 toE
–5. There is some indication of a break in the Cyg X-1 spectrum around 20 keV. Spectral analysis of data in different time intervals for the 1971 April 6 flight demonstrates that while the source intensity varies over time scales of a few minutes, there is no appreciable variation in the spectral slope. Analysis of various hard X-ray observations for long term variations shows that over a period of about a week the intensity of Cyg X-1 varies upto a factor of four. The binary model proposed by Dolan is examined and the difficulties in explaining the observed features of Cyg X-1 by this model are pointed out. 相似文献