流体及磁流体力学在天体物理中的应用
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摘要
流体力学和磁流体力学在天体物理中的应用是十分广泛的。AGN中超大质量黑洞的吸积过程,星系旋臂的密度波,恒星及行星形成的吸积过程,太阳的日冕物质爆发等动力学过程的讨论都离不开流体和磁流体力学。本文着重讨论了流体和磁流体力学在日震学方面和恒星形成中吸积和外流这两方面的应用。
日震学研究中人们对g模式振荡的搜寻一直抱有极大的兴趣。如果g模式确实存在,那么它就会引起太阳内部的密度,压强和温度的周期性变化。这个变化的时间尺度和g模式振荡周期相同。这种周期性的变化会导致太阳内部声速的周期性变化。声速的周期性变化会使得太阳p模式振荡频率也产生周期性变化。本文利用变分原理探讨了通过这种g模式振荡引起的p模式调频现象来寻找太阳g模式振荡的的方法。除了磁场,较差自转和随机激发外,太阳内部的g模式振荡会引起太阳p模式功率谱谱线的分裂。我们发现只有当p模式和g模式的量子数满足一定的匹配关系时,它们之间才能发生相互作用。分析表明我们有可能从足够高的频率分辨率的p模式振荡的功率谱观测资料中找到g模式振荡的。
在本文的另一个工作中,我们考察了准球对称等温自引力系统的自相似磁流体动力学过程。推广了Shu(1977)提出的恒星形成中的自相似核膨胀波坍缩解(EWCS),提出了磁化的外壳膨胀内核收缩解(mEECC)。这些解呈现出各种不同的物理行为,如核坍缩,自相似振荡,外流以及激波。我们还详细分析了在磁声速临界点处的拓扑行为。当描述磁场的参数λ越大的时候,磁化EWCS的吸积率越大。在磁冻结的近似下,外壳膨胀部分的磁场的行为遵从B ∝ r~(-1)的变化规律,内核坍缩时的磁场行为遵从B ∝ r~(-1/2)的变化规律。我们还注意到除了恒星形成外,这些解还可以运用到连接AGB阶段和行星状星云的原行星状星云阶段的某些物理过程中,超新星遗迹和星系团的某些演化阶段中。
Hydrodynamics and magnetohydrodynamics have wide applications in astrophysics. Accretion processes and jets in supermassvie black hole in AGNs, density waves in spiral arms of spiral galaxies, accretion processes and outflows in star and planet formation, stellar oscillations as well as coronal mass ejections are all related to hydrodynamics and magnetohydrodynamics. This paper focuses on the application of hydrodynamics and magnetohydrodynamics to solar oscillations and accretion process and outflow in star formation.Searching g-mode oscillation has generated great interests among helioseismologists. If g-mode oscillations do exist, they would give rise to periodic variation of solar interior temperatures, pressures and densities. Accordingly, periodic variations of these thermodynamic quantities would lead to the periodic variations of solar sound speed. Thus the periodic behavior of sound speed would cause the frequencies of solar p-mode oscillation to change periodically on the time scale of g-mode oscillations. Frequency modulations (FMs) of solar p-modes of shorter periods may occur owing to the simultaneous presence of solar interior g-modes of longer periods and with sufficient strengths. Besides effects of differential rotation, stochastic excitation and magnetic fields, FMs of p-modes by interior g-modes would give rise to organized fine spectral fine structures in the form of frequency splitting intervals of the order of g-mode frequencies. We discuss such an approach to use frequency modulations of solar p-mode by g-modes to search solar g-modes. Analysis shows that it is possible for us to use high frequency resolution p-mode power spectrum data to search solar g-modes.In another work in this thesis, we investigate self-similar magnetohydrodynamics processes in an isothermal self-gravitating fluid with quasi-sphercial symmetry and extend the envelope expansion with core collapse solutions of Lou & Shen by incorporating magnetic fields. Magnetized expansion wave collapse solutions can be constructed as a special case. This inside-out MHD collapse occurs at the magnetosonic speed. Magnetized EECC solutions are also found. These similarity solutions can show various physical processes, such as radial inflow, core collapse, oscillations, outflow as well as shocks. We carefully address the question concerning magnetosonic critical line and topological property of magnetosonic critical points. When the parameter X is larger, the core accretion rate appropriate for magnetized EWCS is larger. In the frozen-in approximation, the magnetic fields in envelope expansion portion would behave as B ∝ r~(-1), while in core collapse portion they would behave as B ∝ r~(-1/2). We note the potential astrophysical application of EECC similarity solutions to star and planet formation processes, to the formation process of proto-planetary nebulae connecting the AGB phase and the planetary nebula phase, to supernova remnants, and to certain evolution stage of galaxy clusters.
日震学研究中人们对g模式振荡的搜寻一直抱有极大的兴趣。如果g模式确实存在,那么它就会引起太阳内部的密度,压强和温度的周期性变化。这个变化的时间尺度和g模式振荡周期相同。这种周期性的变化会导致太阳内部声速的周期性变化。声速的周期性变化会使得太阳p模式振荡频率也产生周期性变化。本文利用变分原理探讨了通过这种g模式振荡引起的p模式调频现象来寻找太阳g模式振荡的的方法。除了磁场,较差自转和随机激发外,太阳内部的g模式振荡会引起太阳p模式功率谱谱线的分裂。我们发现只有当p模式和g模式的量子数满足一定的匹配关系时,它们之间才能发生相互作用。分析表明我们有可能从足够高的频率分辨率的p模式振荡的功率谱观测资料中找到g模式振荡的。
在本文的另一个工作中,我们考察了准球对称等温自引力系统的自相似磁流体动力学过程。推广了Shu(1977)提出的恒星形成中的自相似核膨胀波坍缩解(EWCS),提出了磁化的外壳膨胀内核收缩解(mEECC)。这些解呈现出各种不同的物理行为,如核坍缩,自相似振荡,外流以及激波。我们还详细分析了在磁声速临界点处的拓扑行为。当描述磁场的参数λ越大的时候,磁化EWCS的吸积率越大。在磁冻结的近似下,外壳膨胀部分的磁场的行为遵从B ∝ r~(-1)的变化规律,内核坍缩时的磁场行为遵从B ∝ r~(-1/2)的变化规律。我们还注意到除了恒星形成外,这些解还可以运用到连接AGB阶段和行星状星云的原行星状星云阶段的某些物理过程中,超新星遗迹和星系团的某些演化阶段中。
Hydrodynamics and magnetohydrodynamics have wide applications in astrophysics. Accretion processes and jets in supermassvie black hole in AGNs, density waves in spiral arms of spiral galaxies, accretion processes and outflows in star and planet formation, stellar oscillations as well as coronal mass ejections are all related to hydrodynamics and magnetohydrodynamics. This paper focuses on the application of hydrodynamics and magnetohydrodynamics to solar oscillations and accretion process and outflow in star formation.Searching g-mode oscillation has generated great interests among helioseismologists. If g-mode oscillations do exist, they would give rise to periodic variation of solar interior temperatures, pressures and densities. Accordingly, periodic variations of these thermodynamic quantities would lead to the periodic variations of solar sound speed. Thus the periodic behavior of sound speed would cause the frequencies of solar p-mode oscillation to change periodically on the time scale of g-mode oscillations. Frequency modulations (FMs) of solar p-modes of shorter periods may occur owing to the simultaneous presence of solar interior g-modes of longer periods and with sufficient strengths. Besides effects of differential rotation, stochastic excitation and magnetic fields, FMs of p-modes by interior g-modes would give rise to organized fine spectral fine structures in the form of frequency splitting intervals of the order of g-mode frequencies. We discuss such an approach to use frequency modulations of solar p-mode by g-modes to search solar g-modes. Analysis shows that it is possible for us to use high frequency resolution p-mode power spectrum data to search solar g-modes.In another work in this thesis, we investigate self-similar magnetohydrodynamics processes in an isothermal self-gravitating fluid with quasi-sphercial symmetry and extend the envelope expansion with core collapse solutions of Lou & Shen by incorporating magnetic fields. Magnetized expansion wave collapse solutions can be constructed as a special case. This inside-out MHD collapse occurs at the magnetosonic speed. Magnetized EECC solutions are also found. These similarity solutions can show various physical processes, such as radial inflow, core collapse, oscillations, outflow as well as shocks. We carefully address the question concerning magnetosonic critical line and topological property of magnetosonic critical points. When the parameter X is larger, the core accretion rate appropriate for magnetized EWCS is larger. In the frozen-in approximation, the magnetic fields in envelope expansion portion would behave as B ∝ r~(-1), while in core collapse portion they would behave as B ∝ r~(-1/2). We note the potential astrophysical application of EECC similarity solutions to star and planet formation processes, to the formation process of proto-planetary nebulae connecting the AGB phase and the planetary nebula phase, to supernova remnants, and to certain evolution stage of galaxy clusters.
引文
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