The Cretaceous in southern China is mainly a set of red and mauve clastic rock, with evaporation layers. For lack of source rock, it has been paid little attention to in the exploration process. With the development of research on hydrocarbon exploration, the masses of Cretaceous reservoirs and shows have been found in recent years. This means that the Cretaceous has great exploration potential. According to the research, authors find that the high-quality reservoir and efficient cap rocks develop in the Cretaceous. At the same time, the Cretaceous and underlying Paleozoic-Early Mesozoic marine strata and overlying Cenozoic nonmarine strata constitute a superimposed basin. Moreover, high-quality source rocks developed in the above-mentioned two sets of strata. In the south, especially in the middle and lower Yangtze region since the Himalayan strong rift was associated with a large number of faults, These faults connect the Cretaceous reservoir and its overlying and underlying source rocks, forming the fault-based and unconformity-based discontinuous source-reservoir-cap accumulation assemblages. Because the Cretaceous has the abundant oil and gas from Paleogene source rocks or Mesozoic-Paleozoic source rocks with secondary hydrocarbon generation ability, three types of reservoirs develop in the Cretaceous: “new-generating and old-reservoiring” reservoirs, “old-generating andnew-reservoiring” reservoirs, and few “self-generating andself-reservoiring” reservoirs. The hydrocarbon enrichment depends on two key factors. Firstly, Cretaceous reservoirs are near to the source kitchens, so its oil and gas source is ample. Secondly, the fault system is well developed, which provides the necessary conducting systems for hydrocarbon accumulation.
We develop a theory for radar signal scattering by anisotropic Langmuir turbulence in the solar corona due to a t+l ⇄ t process. Langmuir turbulence is assumed to be generated within a cone by a narrow type III burst electron beam. Using wave-kinetic
theory we obtain expressions for the frequency shift, scattering cross-section of the turbulence, coefficient of absorption
(due to scattering) and optical depth. On the basis of those expressions we give some estimates for an echo spectrum. We show
that the minimum radar echo frequency shift is determined by the minimal phase velocity of the Langmuir waves, the maximum
shift is determined by the electron beam velocity, but in any case it can not exceed −wt/2 (decay) and wt (coalescence), where
wt is the frequency of a radar signal. The angular characteristics of the scattered signal differ dramatically for the cases
of coalescence and decay. The signal is scattered into a narrow cone high above the specular reflection point (wp ≪ wt), but
in the vicinity of wp ∼ wt/2 the red-shifted echo is scattered isotropically, while the blue-shifted echo is scattered into
a even narrower cone. We show that absorption (due to scattering) increases with increasing radar frequency. The dependence
of the absorption on the local plasma frequency is strongly determined by the Langmuir turbulence spectrum. Our theory shows
that the role of the nonlinear scattering process t+l ⇄ t is essential and that such process can be used for radar studies of the spectral energy density of anisotropic Langmuir turbulence. 相似文献
Velocity determination of 131 head echoes recorded during Perseid meteor shower observations by the Canadian 2 MW radar, has
been performed under the assumption of either their constant velocity or of its linear change with time. Even though the constant
velocities concentrated at 60 km s-1 generally accepted for the Perseids, a substantial number of echoes had velocities either
lower than 60 km s-1 or greater than this value. The inclusion of variable velocity into considerations led to surprising
result that a great portion of the head echoes accelerated (3 possibly decelerating echoes in comparison with 33 accelerating
cases on the level of relative standard deviations of output parameters not exceeding 10%). It seems that the allocation of
the ionization responsible for the head echo is not entirely identical with the instantaneous meteoroid position. As a consequence,
the velocity derived from the measured head echo coordinates can differ from the velocity of parent body. We are not able
to explain this finding at present.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
