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301.
302.
M. V. Belyaeva A. S. Drofa V. N. Ivanov 《Izvestiya Atmospheric and Oceanic Physics》2013,49(2):154-161
Comparative estimates of the efficiency of hygroscopic reagents for the seeding of convective clouds to obtain additional precipitation are performed based on numerical simulation. It is shown that the use of polydisperse salt powders has many benefits over other known hygroscopic reagents. The effect of seeding with salt powders manifests itself at mass concentrations of hygroscopic particles an order of magnitude less than when pyrotechnic flares are used. With salt-powder seeding, it is possible to obtain precipitation from warm convective clouds of moderate thickness from which precipitation does not typically fall. In this case the effect of “reseeding” of clouds, which can be observed in seeding with hygroscopic reagents having narrow size distributions of particles, does not reveal itself. 相似文献
303.
Oceanology - The kinetic energy of six jets of the Antarctic Circumpolar Current (ACC) and of the cyclonic and anticyclonic mesoscale eddies generated by these jets is studied in application to the... 相似文献
304.
Edward B. Jenkins 《Astrophysics and Space Science》2004,289(3-4):215-223
A recent survey of the fine-structure excitation of neutral carbonreveals that the interstellar medium in the Galactic plane exhibits athermal pressure, nT/k, that ranges from about 103to 104cm-3K from one location to the next, with occasional excursions in excess of about 105 cm-3K. The large excitations for small amounts of gas indicate that some regions are either subjected to shocks or must be pressurized within time scales much shorter than the time needed to reach thermal equilibrium. These rapidfluctuations probably arise from the cascade of macroscopic mechanical energyto small scales through a turbulent cascade. One consequence of thiseffect is that changes in gas temperature can arise from near adiabaticcompressions and expansions, and this may explain why investigations of21-cm emission and absorption reveal the presence of hydrogen attemperatures well below the expected values derived from the balance ofvarious known heating and cooling processes. 相似文献
305.
306.
G. M. Tovmasyan R. Kh. Oganesyan R. A. Epremyan S. E. Nersesyan M. A. Mkrtchyan Yu. M. Khodzhayants M. N. Krmoyan A. L. Kashin D. Huguenin S. I. Serova Yu. V. Romanenko A. P. Aleksandrov V. G. Titov M. Kh. Manarov 《Astrophysics》1990,32(1):1-5
Byurakan Astrophysical Observatory; SKB Granit; Geneva Observatory; Flight Control Center. Translated from Astrofizika, Vol. 32, No. 1, p. 5–13, January–February, 1990. 相似文献
307.
308.
J. A. Docobo V. S. Tamazian N. D. Melikian M. H. Eritsian A. A. Karapetian 《Astrophysics》2000,43(2):162-169
The results of photometric and polarimetric observations of the star Μ Cep at Byurakan Observatory are presented. Some interesting
correlations between the parameters of the star’s brightness variation and the degree of polarization of the light are obtained.
It is suggested that the recorded rapid changes in the degree of polarization may result from Μ Cep being a double star.
Translated from Astrofizika, Vol. 43, No. 2, pp. 219-228, April–June, 2000. 相似文献
309.
In this paper we have studied the possible proton collisions in cosmic ray sources. On the basis of our calculations of background temperature, the operational domains of various proton collisions are suggested. The energy rate loss through the photo-neutrino processes on protons is computed and we have discussed the energy distribution of the secondary particles in various collisions. 相似文献
310.
The magneto-rotational evolution of a neutron star in the massive binary system 4U 2206+54 is discussed in light of the recent
discovery of its 5555 s rotational period and its average rate of spin-down. We show that this behavior of the neutron star
means that its magnetic field exceeds the quantum mechanical critical limit and it is an accretion magnetar. The system’s
evolution is explained by wind driven mass transfer without formation of an accretion disk. The constant character of the
x-ray source indicates a steady rate of accretion and raises anew the question of the stability of the boundary of the magnetosphere
of a star undergoing spherical accretion. A solution to this problem is also a key to determining the mechanism for the slowing
down of the star’s rotation. 相似文献