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961.
Edward C. D. Pope Georgi Pavlovski Christian R. Kaiser Hans Fangohr 《Monthly notices of the Royal Astronomical Society》2006,367(3):1121-1131
In recent years, evidence has accumulated suggesting that the gas in galaxy clusters is heated by non-gravitational processes. Here, we calculate the heating rates required to maintain a physically motivated mass flow rate, in a sample of seven galaxy clusters. We employ the spectroscopic mass deposition rates as an observational input along with temperature and density data for each cluster. On energetic grounds, we find that thermal conduction could provide the necessary heating for A2199, Perseus, A1795 and A478. However, the suppression factor of the classical Spitzer value is a different function of radius for each cluster. Based on the observations of plasma bubbles, we also calculate the duty cycles for each active galactic nucleus (AGN), in the absence of thermal conduction, which can provide the required energy input. With the exception of Hydra-A, it appears that each of the other AGNs in our sample requires duty cycles of roughly 106 –107 yr to provide their steady-state heating requirements. If these duty cycles are unrealistic, this may imply that many galaxy clusters must be heated by very powerful Hydra-A type events interspersed between more frequent smaller scale outbursts. The suppression factors for the thermal conductivity required for combined heating by AGN and thermal conduction are generally acceptable. However, these suppression factors still require 'fine-tuning' of the thermal conductivity as a function of radius. As a consequence of this work, we present the AGN duty cycle as a cooling flow diagnostic. 相似文献
962.
Enikö Regös Vernon C. Bailey Rosemary Mardling 《Monthly notices of the Royal Astronomical Society》2005,358(2):544-550
The concept of Roche lobe overflow is fundamental to the theory of interacting binaries. Based on potential theory, it is dependent on all the relevant material corotating in a single frame of reference. Therefore if the mass losing star is asynchronous with the orbital motion or the orbit is eccentric, the simple theory no longer applies and no exact analytical treatment has been found. We use an analytic approximation whose predictions are largely justified by smoothed particle hydrodynamic simulations (SPH). We present SPH simulations of binary systems with the same semi-major axis a = 5.55 R⊙ , masses M 1 = 1 M⊙ , M 2 = 2 M⊙ and radius R 1 = 0.89 R⊙ for the primary star but with different eccentricities e = 0.4, 0.5, 0.6 and 0.7. In each case the secondary star is treated as a point mass. When e = 0.4 no mass is lost from the primary while at e = 0.7 catastrophic mass transfer, partly through the L2 point, takes place near periastron. This would probably lead to common-envelope evolution if star 1 were a giant or to coalescence for a main-sequence star. In between, at e ≥ 0.5 , some mass is lost through the L1 point from the primary close to periastron. However, rather than being all accreted by the secondary, some of the stream appears to leave the system. Our results indicate that the radius of the Roche lobe is similar to circular binaries when calculated for the separation and angular velocity at periastron. Part of the mass loss occurs through the L2 point. 相似文献
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After nearly 20 years of construction,we have successfully solved a series of hydrologic sedimentaryand environment problems encountered during the construction of the big deep water harbour inLianyungang which can now accommodate ships of 50000 tonnage.With the economic development,the channel of 50000 tonnage will be built soon, and of 100000 tonnage is under planning. Theconstruction of the international container shipping hub at the harbour is being accelerated in anticipationof the opening of the second Eurasian land bridge.The future development of the harbour will givegreat impetus to the local economy of Lianyungang City and make it an international city. 相似文献
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968.
We study analytically the Rayleigh–Taylor instability in expanding supernova gas shell. The instability appears at the inner
shell surface accelerated by blowing pulsar wind. The most dangerous perturbations correspond to wavelengths comparable to
the shell thickness. We analyze the fragility of the supernova remnant shell in function of the initial perturbation amplitude
and the shell thickness. 相似文献
969.
ZHANG Junyan CHENG Genwei LI Yongfei 《山地科学学报》2006,3(2):125-130
Introduction Landscape evolution in glaciated high mountains environment in southwestern China is undergoing the coupled processes of monsoon- induced denudation and active tectonic. The debris fan development, in particular sediment transfer, is most int… 相似文献
970.