Equilibrium Structures of Rotationally and Tidally Distorted Polytropic Models of Stars

We propose suitable modifications in the concept of Roche equipotentials to account for the effect of mass distribution inside a star. The Kippenhahn and Thomas (1970) approach is used to incorporate the effects of rotational and tidal forces in the equations of stellar structure. The proposed method is applied to compute structures of certain rotationally and tidally distorted polytropic models.     

Convergence of Liapunov series for Huygens–Roche Figures

According to the classical theory of equilibrium figures, surfaces of equal density, potential and pressure concur (let us call them isobars). Isobars can be represented by means of Liapunov power series in small parameter q, up to the first approximation coinciding with the centrifugal to gravitational force ratio at the equator. Liapunov has proved the existence of the universal convergence domain: the above mentioned series converge for all bodies (satisfying a natural condition that the density ρ decreases from the center to the surface) if |q| < q*. Using Liapunov’s algorithm and symbolic manipulation tools, we have found q*= 0.000370916. Evidently, the convergence radius q* may be much greater in common situations. To comfirm it it is reasonable to consider two limiting and one or two intermediate cases for the density behaviour: ρ is a constant, the Dirac’s δ-function, linear function of the distance from the center, etc. And indeed, in the previous paper we find a three orders of magnitude greater value for homogeneous figures. In the present paper we find that in the opposite case of Huygens-Roche figures (a point-mass surrounded by a weightless atmosphere) the convergence radius is unexpectedly large and coincides with the well-known biggest possible value q*= 0.541115598 for such a class of figures. To ascertain it we ought to use numerical calculations, so our main result is demonstrated by means of a computer assisted proof. This revised version was published online in July 2006 with corrections to the Cover Date.     

On the nature of the radial velocity variability of Aldebaran: a search for spectral line bisector variations

The shape of the Ti  i 6303.8-Å spectral line of Aldebaran as measured by the line bisector was investigated using high signal-to-noise ratio, high-resolution data. The goal of this study was to understand the nature of the 643-d period in the radial velocity for this star reported by Hatzes & Cochran. Variations in the line bisector with the radial velocity period would provide strong evidence in support of rotational modulation or stellar pulsations as the cause of the 643-d period. A lack of any bisector variability at this period would support the planet hypothesis.
Variations in the line asymmetries are found with a period of 49.93 d. These variations are uncorrelated with the 643-d period found previously in the radial velocity measurements. It is demonstrated that this 50-d period is consistent with an m =4 non-radial sectoral g-mode oscillation. The lack of spectral variability with the radial velocity period of 643 d may provide strong evidence in support of the hypothesis that this variability stems from the reflex motion of the central star due to a planetary companion having a mass of 11 Jupiter masses. However, this long-period variability may still be the result of a low-order ( m =2) pulsation mode as these would cause bisector variations of less than the error measurement.     

On the radio spectrum of CI Cygni: a test of popular models for symbiotic stars

We have determined the spectral energy distribution at wavelengths between 6 cm and 850 μm for the prototypical S(stellar)-type symbiotic star, CI Cygni, during quiescence. Data were obtained simultaneously with the Very Large Array and the SCUBA submillimetre (sub-mm) camera on the James Clerk Maxwell Telescope. The data have allowed us to determine the free–free turnover frequency of the ionized component, facilitating a model-dependent estimate of the binary separation to compare with the known orbital parameters of CI Cyg and to critically test the known models for radio emission from symbiotic stars. In particular, our data rule out the two most popular models: ionization of the giant wind by Lyman continuum photons from its hot companion, and emission resulting from the interaction of winds from the two binary components.     

On the migration of a system of protoplanets

The evolution of a system consisting of a protoplanetary disc with two embedded Jupiter-sized planets is studied numerically. The disc is assumed to be flat and non-self-gravitating; this is modelled by the planar (two-dimensional) Navier–Stokes equations. The mutual gravitational interaction of the planets and the star, and the gravitational torques of the disc acting on the planets and the central star are included. The planets have an initial mass of one Jupiter mass M _Jup each, and the radial distances from the star are one and two semimajor axes of Jupiter, respectively.
During the evolution a joint wide annular gap is created by the planets. Both planets increase their mass owing to accretion of gas from the disc: after about 2500 orbital periods of the inner planet it has reached a mass of 2.3  M _Jup, while the outer planet has reached a mass of 3.2  M _Jup. The net gravitational torques exerted by the disc on the planets result in an inward migration of the outer planet on time-scales comparable to the viscous evolution time of the disc. The semimajor axis of the inner planet remains constant as there is very little gas left in its vicinity to induce any migration. When the distance of close approach eventually becomes smaller than the mutual Hill radius, the eccentricities increase strongly and the system may become unstable.
If disc depletion occurs rapidly enough before the planets come too close to each other, a stable system similar to our own Solar system may remain. Otherwise the orbits may become unstable and produce systems like υ And.     

On the formation of massive stars

We present a model for the formation of massive ( M ≳10 M⊙) stars through accretion-induced collisions in the cores of embedded dense stellar clusters. This model circumvents the problem of accreting on to a star whose luminosity is sufficient to reverse the infall of gas. Instead, the central core of the cluster accretes from the surrounding gas, thereby decreasing its radius until collisions between individual components become sufficient. These components are, in general, intermediate-mass stars that have formed through accretion on to low-mass protostars. Once a sufficiently massive star has formed to expel the remaining gas, the cluster expands in accordance with this loss of mass, halting further collisions. This process implies a critical stellar density for the formation of massive stars, and a high rate of binaries formed by tidal capture.     

On the effects of the stellar magnetic field on the structure of T Tauri accretion discs

The structure of accretion discs around magnetic T Tauri stars is calculated numerically using a particle hydrodynamical code, in which magnetic interaction is included in the framework of King's diamagnetic blob accretion model. Setting up the calculation so as to simulate the density structure of a quasi-steady disc in the equatorial plane of a T Tauri star, we find that the central star's magnetic field typically produces a central hole in the disc and spreads out the surface density distribution. We argue that this result suggets a promising mechanism for explaining the unusual flatness (IR excess) of T Tauri accretion disc spectra.     

基于1．2m望远镜白适应光学系统激光信标转盘式机械快门的研究

基于激光信标发射和接收共光路系统中探测器受杂散光影响的关键问题,设计了一种新型转盘式机械快门装置,对光信号进行高频率开关控制,从而对自适应光学系统的波前探测器起到彻底保护作用。设计时,分析了瑞利信标的采样厚度以及快门开关与脉冲激光器的发射、探测器探测时间的时序控制。     

基于1.2m望远镜自适应光学系统激光信标转盘式机械快门的研究

基于激光信标发射和接收共光路系统中探测器受杂散光影响的关键问题,设计了一种新型转盘式机械快门装置,对光信号进行高频率开关控制,从而对自适应光学系统的波前探测器起到彻底保护作用.设计时,分析了瑞利信标的采样厚度以及快门开关与脉冲激光器的发射、探测器探测时间的时序控制.     

Absolute Calibration of the PL-Relations for the Classical Cepheids Based on the HIPPARCOS Parallaxes and the Distances of the Magellanic Clouds

The zero points of the period-luminosity relations for the classical cepheids are calibrated based on the HIPPARCOS parallaxes of these stars. The calibrations are used to determine the distance moduli of the LMC and SMC: DM _LMC = 18^m.569 ± 0^m.117 and DM _SMC = 19^m.070 ± 0^m.119, respectively. It turns out that a calibration of the PL relations based on the distances of 25 FU classical cepheids in the galaxy by Gieren et al. yields a distance scale that is shorter by approximately 0^m.20 than the calibrations based on the HIPPARCOS parallaxes.     

Analytical solution for the evolution of a binary with stable mass transfer from a giant

We derive a simple analytical solution for the evolution of a close binary with nuclear time-scale driven mass transfer from a giant. This solution is based on the well-known fact that the luminosity and the radius of a giant scale to a good approximation as simple power laws of the mass M _c of the degenerate helium core. Comparison with results of numerical calculations by Webbink, Rappaport & Savonije show the analytical solution and the power-law approximation to be quite accurate. The analytical solution presented does also allow (in parametrized form) for non-conservative mass transfer. Furthermore, it is shown that the near constancy of the mass-transfer rate over most of the mass-transfer phase seen in the results by Webbink, Rappaport & Savonije is not a generic feature of this type of evolution but rather a consequence of a particular choice of parameters. The analytical solution also demonstrates that the level of mass transfer is largely set by the core mass of the giant at the onset of mass transfer. Finally, we show that the model is self-consistent and discuss its applicability to low-mass X-ray binaries.     

Effects of a clumpy circumstellar medium on the dynamics of stellar winds

Mass pickup from clumps resulting from previous mass loss phases by a fast stellar wind can substantially modify its behaviour, even leading to a highly supersonic wind becoming transonic before leaving the mass-loading region. The observational consequences of mass-loading on these astrophysical flows is discussed.