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In the estimation of momentum fluxes over land surfaces by the bulk aerodynamic method, no unique value of the drag coefficient
(C
D) is found in the literature. The drag coefficient is generally estimated from special observations at different parts of
the world. In this study an attempt is made to estimate drag coefficient over the western desert sector of India using data
sets of Monsoon Trough Boundary Layer Experiment (MONTBLEX) during the summer monsoon season of 1990. For this purpose, the
fast and slow response data sets obtained simultaneously from a 30 m high micro-meteorological tower at Jodhpur are used.
All the observations used in this study are confined to a wind speed regime of 2.5–9.0 ms−1.
A comparison of momentum fluxes computed by eddy correlation (direct estimation) with profile and bulk aerodynamic (C
D = 3.9 × 10−3, Garratt, 1977) methods revealed that though the nature of variation of the fluxes by all these methods is almost similar,
both the indirect methods give an under-estimated value of the fluxes. The drag coefficient is estimated as a function of
wind speed and surface stability by a multiple regression approach. An average value of the estimated drag coefficient is
found to be of the order of 5.43 × 10−3. The estimated value ofC
D is validated with a set of independent observations and found to be quite satisfactory. The recomputed momentum fluxes by
bulk aerodynamic method using the estimated drag coefficient are in close agreement with the directly estimated fluxes. 相似文献
2.
The present study deals with locally rotationally symmetric (LRS) Bianchi type II cosmological model representing massive
string. The energy-momentum tensor for such string as formulated by Letelier (Phys. Rev. D 28:2414, 1983) is used to construct massive string cosmological model for which we assume that the expansion (θ) in the model is proportional to the shear (σ). This condition leads to A=B
m
, where A and B are the metric coefficients and m is proportionality constant. For suitable choice of constant m, it is observed
that in early stage of the evolution of the universe string dominates over the particle whereas the universe is dominated
by massive string at the late time. Our model is in accelerating phase which is consistent to the recent observations of type
Is supernovae. Some physical and geometric behavior of the model is also discussed. 相似文献
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