Stellar wind/ISM shocks in gravitational potentials     

A. Hubbard 《Monthly notices of the Royal Astronomical Society》2007,374(3):1045-1050

  相似文献   

Self-regulated gravitational accretion in protostellar discs     

E. I. Vorobyov  Shantanu Basu 《Monthly notices of the Royal Astronomical Society》2007,381(3):1009-1017

We present a numerical model for the evolution of a protostellar disc that has formed self-consistently from the collapse of a molecular cloud core. The global evolution of the disc is followed for several million years after its formation. The capture of a wide range of spatial and temporal scales is made possible by use of the thin-disc approximation. We focus on the role of gravitational torques in transporting mass inward and angular momentum outward during different evolutionary phases of a protostellar disc with disc-to-star mass ratio of order 0.1. In the early phase, when the infall of matter from the surrounding envelope is substantial, mass is transported inward by the gravitational torques from spiral arms that are a manifestation of the envelope-induced gravitational instability in the disc. In the late phase, when the gas reservoir of the envelope is depleted, the distinct spiral structure is replaced by ongoing irregular non-axisymmetric density perturbations. The amplitude of these density perturbations decreases with time, though this process is moderated by swing amplification aided by the existence of the disc's sharp outer edge. Our global modelling of the protostellar disc reveals that there is typically a residual non-zero gravitational torque from these density perturbations, i.e. their effects do not exactly cancel out in each region. In particular, the net gravitational torque in the inner disc tends to be negative during first several million years of the evolution, while the outer disc has a net positive gravitational torque. Our global model of a self-consistently formed disc shows that it is also self-regulated in the late phase, so that it is near the Toomre stability limit, with a near-uniform Toomre parameter Q ≈ 1.5–2.0. Since the disc also has near-Keplerian rotation, and comparatively weak temperature variation, it maintains a near-power-law surface density profile proportional to r ^−3/2.  相似文献   

Interfacial instabilities driven by self-gravity: first numerical results     

R.M. Hueckstaedt  J.H. HunterJr 《Monthly notices of the Royal Astronomical Society》2001,327(4):1097-1102

The evolution of the interstellar medium (ISM) is driven by a variety of phenomena, including turbulence, shearing flows, magnetic fields and the thermal properties of the gas. Among the most important forces at work is self-gravity, which ultimately drives protostellar collapse. As part of an ongoing study of instabilities in the ISM, Hunter, Whitaker & Lovelace have discovered another process driven by self-gravity: the instability of an interface of discontinuous density. Theory predicts that this self-gravity driven interfacial instability persists in the static limit and in the absence of a constant background acceleration. Disturbances to a density interface are found to grow on a time-scale of the order of the free-fall time, even when the perturbation wavelength is much less than the Jeans length. Here we present the first numerical simulations of this instability. The theoretical growth rate is confirmed and the non-linear morphology displayed. The self-gravity interfacial instability is shown to be fundamentally different from the Rayleigh–Taylor instability, although both exhibit similar morphologies under the condition of a high density contrast, such as is commonly found in the ISM. Such instabilities are a possible mechanism by which observed features, such as the pillars of gas seen near the boundaries of interstellar clouds, are formed.  相似文献   

海冰动力学数值方法研究进展   总被引：1，自引：0，他引：1  

季顺迎  岳前进  王瑞学 《地球科学进展》2004,19(6):963-970

在海冰动力学数值模拟和预测研究中,人们将海冰视为连续介质分别建立了欧拉坐标下的有限差分（FD）方法、拉格朗日坐标下的光滑质点流体动力学（SPH）方法、欧拉和拉格朗日坐标相结合的质点网格法（PIC）,近年来又发展了基于非连续介质的颗粒流（GF）方法。对以上几种海冰动力学数值方法的特点和适用性进行了讨论,结果表明：FD、PIC和SPH方法可适用于中长期海冰动力学数值模拟,但SPH方法的计算效率需进一步提高;GF方法在不同尺度下的海冰动力学数值模拟中的计算精度均有很强的适用性,但目前较适用于小尺度下海冰动力学基本特性的数值试验研究,计算时效还不能满足实际海冰数值模拟和预测的要求。为进一步提高海冰动力学模拟的精度和适用性,在不同时空尺度下分别发展与其相适应的数值方法是必要的。  相似文献   

Analytic solutions to the accretion of a rotating finite cloud towards a central object – I. Newtonian approach     

S. Mendoza  E. Tejeda  E. Nagel † 《Monthly notices of the Royal Astronomical Society》2009,393(2):579-586

We construct a steady analytic accretion flow model for a finite rotating gas cloud that accretes material to a central gravitational object. The pressure gradients of the flow are considered to be negligible, and so the flow is ballistic. We also assume a steady flow and consider the particles at the boundary of the spherical cloud to be rotating as a rigid body, with a fixed amount of inwards radial velocity. This represents a generalization to the traditional infinite gas cloud model described by Ulrich. We show that the streamlines and density profiles obtained deviate largely from the ones calculated by Ulrich. The extra freedom in the choice of the parameters on the model can naturally account for the study of protostars formed in dense clusters by triggered mechanisms, where a wide variety of external physical mechanisms determine the boundary conditions. Also, as expected, the model predicts the formation of an equatorial accretion disc about the central object with a radius different from the one calculated by Ulrich.  相似文献   

Vortices in self-gravitating gaseous discs     

G. R. Mamatsashvili  W. K. M. Rice 《Monthly notices of the Royal Astronomical Society》2009,394(4):2153-2163

  相似文献   

Keeping the Universe ionized: photoheating and the clumping factor of the high-redshift intergalactic medium     

Andreas H. Pawlik  Joop Schaye  Eveline van Scherpenzeel 《Monthly notices of the Royal Astronomical Society》2009,394(4):1812-1824

  相似文献   

NLTE models of line-driven stellar winds – III. Influence of X-ray radiation on wind structure of O stars     

Ji&#;í Krti&#;ka  Ji&#;í Kubát 《Monthly notices of the Royal Astronomical Society》2009,394(4):2065-2079

We study the influence of X-rays on the wind structure of selected O stars. For this purpose we use our non-local thermodynamic equilibrium (NLTE) wind code with inclusion of additional artificial source of X-rays, assumed to originate in the wind shocks.
We show that the influence of shock X-ray emission on wind mass-loss rate is relatively small. Wind terminal velocity may be slightly influenced by the presence of strong X-ray sources, especially for stars cooler than   T _eff≲ 35 000 K  .
We discuss the origin of the   L _X/ L ∼ 10⁻⁷  relation. For stars with thick wind this relation can be explained assuming that the cooling time depends on wind density. Stars with optically thin winds exhibiting the 'weak wind problem' display enhanced X-ray emission which may be connected with large shock cooling length. We propose that this effect can explain the 'weak wind problem'.
Inclusion of X-rays leads to a better agreement of the model ionization structure with observations. However, we do not find any significant influence of X-rays on P  v ionization fraction implying that the presence of X-rays cannot explain the P  v problem.
We study the implications of modified ionization equilibrium due to shock emission on the line transfer in the X-ray region. We conclude that the X-ray line profiles of helium-like ions may be affected by the line absorption within the cool wind.  相似文献   

Diurnal thermal tides in a non-synchronized hot Jupiter     

Pin-Gao Gu  Gordon I. Ogilvie 《Monthly notices of the Royal Astronomical Society》2009,395(1):422-435

We perform a linear analysis to investigate the dynamical response of a non-synchronized hot Jupiter to stellar irradiation. In this work, we consider the diurnal Fourier harmonic of the stellar irradiation acting at the top of a radiative layer of a hot Jupiter with no clouds and winds. In the absence of the Coriolis force, the diurnal thermal forcing can excite internal waves propagating into the planet's interior when the thermal forcing period is longer than the sound crossing time of the planet's surface. When the Coriolis effect is taken into consideration, the latitude-dependent stellar heating can excite weak internal waves (g modes) and/or strong baroclinic Rossby waves (buoyant r modes) depending on the asynchrony of the planet. When the planet spins faster than its orbital motion (i.e. retrograde thermal forcing), these waves carry negative angular momentum and are damped by radiative loss as they propagate downwards from the upper layer of the radiative zone. As a result, angular momentum is transferred from the lower layer of the radiative zone to the upper layer and generates a vertical shear. We estimate the resulting internal torques for different rotation periods based on the parameters of HD 209458b.  相似文献   

Dual black holes in merger remnants – I. Linking accretion to dynamics     

M. Dotti  M. Ruszkowski  L. Paredi  M. Colpi  M. Volonteri  F. Haardt 《Monthly notices of the Royal Astronomical Society》2009,396(3):1640-1646

We study the orbital evolution and accretion history of massive black hole (MBH) pairs in rotationally supported circumnuclear discs up to the point where MBHs form binary systems. Our simulations have high resolution in mass and space which, for the first time, makes it feasible to follow the orbital decay of a MBH either counter- or corotating with respect to the circumnuclear disc. We show that a moving MBH on an initially counter-rotating orbit experiences an 'orbital angular momentum flip' due to the gas-dynamical friction, i.e. it starts to corotate with the disc before a MBH binary forms. We stress that this effect can only be captured in very high resolution simulations. Given the extremely large number of gas particles used, the dynamical range is sufficiently large to resolve the Bondi–Hoyle–Lyttleton radii of individual MBHs. As a consequence, we are able to link the accretion processes to the orbital evolution of the MBH pairs. We predict that the accretion rate is significantly suppressed and extremely variable when the MBH is moving on a retrograde orbit. It is only after the orbital angular momentum flip has taken place that the secondary rapidly 'lights up' at which point both MBHs can accrete near the Eddington rate for a few Myr. The separation of the double nucleus is expected to be around ≲10 pc at this stage. We show that the accretion rate can be highly variable also when the MBH is corotating with the disc (albeit to a lesser extent) provided that its orbit is eccentric. Our results have significant consequences for the expected number of observable double active galactic nuclei at separations of ≲100 pc.  相似文献