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绝热脉动
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  “绝热脉动”译为未确定词的双语例句
     In the quasi-adiabatic region, turbulent pressure will be to exert destabilizing influence.
     而在准绝热脉动区,湍流压起退稳定的作用.
短句来源
  相似匹配句对
     DECOUPLING TREATMENT OF LINEAR NONADIABATIC NONRADIAL PULSATIONS OF STARS
     恒星线性非绝热非径向脉动问题的退耦化处理方法
短句来源
     In the quasi-adiabatic region, turbulent pressure will be to exert destabilizing influence.
     而在准绝热脉动区,湍流压起退稳定的作用.
短句来源
     Chaotic Pulsation in Variable Stars
     变星的混沌脉动
短句来源
     THE FOAMED PLASTICS USED IN CRYOGENIC INSULATION
     低温绝热泡沫塑料
短句来源
     Adiabatic Expansion of Electron Beam
     电子束的绝热展开
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  adiabatic pulsation
Moreover, the theory predicts changes in mode frequency that may, in part, explain the discrepancy between solar observations and the adiabatic pulsation frequencies of theoretical models.
      


The dynamic behavior of turbulent convection is studied. From the dynamic- equations of correlation function, we have obtained steady component and pulsational- component of convections. The physical significance of these solutions are discussed, and main results may be summarized as follows: (1) For the steady convection, Vitense's and Opik's phenomenological theories can be recovered as special cases of present statistical theory. (2) Taking account of the dynamic process of turbulent convection, turbulent...

The dynamic behavior of turbulent convection is studied. From the dynamic- equations of correlation function, we have obtained steady component and pulsational- component of convections. The physical significance of these solutions are discussed, and main results may be summarized as follows: (1) For the steady convection, Vitense's and Opik's phenomenological theories can be recovered as special cases of present statistical theory. (2) Taking account of the dynamic process of turbulent convection, turbulent vicious forces and pulsational amplitudes of heat convection and turbulent pressure decrease, and a phase-lag arises. (3) The analysis of vibrational stability indicates that: a) The net direct effect of the energy convection (heated and mechanical) under ionizing regions of abundant elements tend to promote the pulsational instabi- lity. However, in the ionizing regions of abundant elements it may produce a damping effect. b) Turbulent viscosity always produces a damping effect. In the quasi-adiabatic region, turbulent pressure will be to exert destabilizing influence. c) The energy transferred from turbulence through moleculer stresses (gas pressure and molecular viscosity) has an effects on vibrational stability just against the turbulent Reynold's stresses. These effects might account for the location of red-edge of pulsational instability strip, and for the light variabirity of red giants and supergiants.

本文研究了湍动对流的动力学过程.从统一的关联函数的动力学方程出发,同时得到了变星脉动速度场下,对流的定常分量和脉动分量.主要结果可归结如下:(1)对于定常对流,维滕斯的混合长理论和奥比克的元胞对流公式,均可视为我们统计理论的特殊情况.(2)考虑到湍动对流建立的动力学过程,与似稳流场的混合长理论相比,湍动对流脉动分量的振幅减小了,并且出现一个相位滞后.(3)讨论了湍动对流对变星脉动稳定性的影响,它表明:a)在丰富元素的电离区之下,湍动能对流(热对流加机械能流)的直接作用是促使脉动不稳定;而在丰富元素的电离区,对流传能起稳定性作用.b)湍流粘滞性永远起阻尼作用;而在准绝热脉动区,湍流压起退稳定的作用.c)分子应力(气体压加分子粘滞应力)对湍流作功项对变星脉动稳定性的作用,正好同湍流雷诺应力的作用相反.辐射传能和湍动对流的综合作用,可以解释“造父型”变星脉动不稳定区红端边界和晚型红巨星及超巨星的光度变化.

According to the time-dependent convection theory developed in [1], the thermodynamic coupling between radial pulsations and convection is studied. The growth rate for small-amplitude pulsation has been calculated in linear nonadiabatic approximation for 11 series of RR Lyrae models. The dependence of the red edge of their instability strip on the mass, luminosity, helium abundance and convective paramater has been investigated.

本文根据依赖时间的对流统计理论,研究了对流同变星脉动的热力学耦合。对11种天琴座RR型变星模型序进行了线性非绝热脉动的计算,并探讨了脉动不稳定区红端边界对于恒星质量、光度、氦含量以及对流参数c_1=I_(el)/H_p的依赖关系.

Dephei stars are a group of short-period intrinsic variables on the upper mainsequence. Finding the excitation mechanism for them and other early-type variablesis a long standing problem. The new OPAL opacity tables show some significantenhancements with respect to the old tos Alamos opacity. The kappa-mechanism proposed long ago becomes very likely to be the driving mechanism for β Depheipulsators.In this paper, the stability of β Cephei stars are studied using linear theory ofradial non-adiabatic pulsation....

Dephei stars are a group of short-period intrinsic variables on the upper mainsequence. Finding the excitation mechanism for them and other early-type variablesis a long standing problem. The new OPAL opacity tables show some significantenhancements with respect to the old tos Alamos opacity. The kappa-mechanism proposed long ago becomes very likely to be the driving mechanism for β Depheipulsators.In this paper, the stability of β Cephei stars are studied using linear theory ofradial non-adiabatic pulsation. The opacity used here is an analytical fit to the standard OPAL opacity made by the authors, by which the opadty-mechanism is examined. However, no instability is found up to the tenth radial overtone in ourcalculation. Following this results we suspect that the K-mechanism might not bestrong enough to excite β Cephei stars. Furthermore, as the instability of β Cepheistars found by others is not confirmed by the present work, it seems to be too earlyto draw a firm conclusion to the exciation mechanism for β Cephei stars. From ourpoint of view, reexamination of K-mechanism and careful consideration of othermechanisms should be undertaken.

仙王座β型变星是一类上部主序的短周期内因变星,找到它们及其它早型变星的脉动激发机制是一个长期未能解决的问题.新发表的不透明度表格OPAL比早期的表格有显著的提高,这样不透明度机制似乎就能够解释仙王座β型变星的脉动.本文用线性径向非绝热脉动理论研究了仙王座β型星的脉动稳定性,检查了不透明度机制,用的不透明度是对OPAL表格的一种分析逼近,但计算的十阶以下脉动模式都是稳定的.由于未能证实别人得到的脉动不稳定性,所以我们怀疑不透明度机制可能还不足以激发仙王座β型星,因而给它们的激发机制下一个肯定的结论似乎还为时过早.我们认为对仙王座β型星的脉动起因,有必要进一步研究不透明度机制或别的脉动激发机制.

 
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