Gravitational loss-cone instability

We study physical corollaries of the existing analogy between the simplest plasma traps (mirror traps) and star clusters surrounding massive black holes or dense galactic nuclei. There is a loss cone in the system through which plasma particles with low velocities transverse to the trap axis or, similarly, stars with low angular momenta (destroyed or absorbed by the central body) escape. The consequences of the “beam-like” deformation of the plasma distribution function in a trap are well known: a peculiar loss-cone instability producing a plasma flow into the loss cone develops as a result. We show that a similar gravitational loss-cone instability can also arise under certain conditions in the galactic case of interest to us. This instability is related to the slow precessional motions of highly elongated (nearly radial) stellar orbits and the main condition for its growth is that the precession of such orbits be retrograde (in the direction opposite to the orbital rotation of stars). Only under this condition do oscillations that can become unstable in the presence of a loss cone arise instead of the radial orbit instability (a variety of the Jeans instability in systems with highly elongated orbits) that takes place in the case of prograde precession. The instability produces a stream of stars onto the galactic center, i.e., serves as a mechanism of fueling the nuclear activity of galaxies. For a mathematical analysis, we have obtained relatively simple characteristic equations that describe small perturbations in a sphere of radially highly elongated stellar orbits. These characteristic equations are derived through a number of successive simplifications from a general linearized system of equations, including the collisionless Boltzmann kinetic equation and the Poisson equation (in action-angle variables). The central point of our analysis of the characteristic equations is preliminary detection of neutral modes (or proof of their absence in the case of stability).     

Flat Galaxies with Dark Matter Halos—Existence and Stability

We consider a model for a flat, disk-like galaxy surrounded by a halo of dark matter, namely a Vlasov-Poisson type system with two particle species, the stars which are restricted to the galactic plane and the dark matter particles. These constituents interact only through the gravitational potential which stars and dark matter create collectively. Using a variational approach we prove the existence of steady state solutions and their nonlinear stability under suitably restricted perturbations.     

On the Distribution of Radio Pulsars Above the Galaxy Plane

A mechanism of pulsar accumulation over the galaxy plane, caused by deceleration in the gravitational field and stopping at a certain distance of z from the plane is proposed. For pulsars with velocities close to the average observed velocity of about 300 km/s, the consideration of kinematics of such motion estimates the age of stopped pulsars of the order of ten millions years and the average distance from the galaxy plane of about 2 kpc. The consistency in the pulsar longitude distribution at |z| = 0.45–4.5 kpc and the distribution of the formation regions of massive stars in the galaxy disk was found.     

The elliptical motion of stars in close binary systems with a conservative mass exchange

The problem of the motion of a star in a close binary system with a conservative mass exchange is considered. In contrast to the well-known Paczynski-Huang model, a new model is used that defines the motion of close binary systems in the case of an elliptical orbit. The reactive forces and the force of gravity of stars by the overflowing jet are accounted for in the elliptic motion of the star. The calculations of elliptical orbits of close binary stars show that the effect of the reactive force on the evolution of the star orbit can be different. The changes of the major axis and eccentricity of the orbit of the second star are defined. The results are applied to the BF Aurigae star system and are given in the form of figures.     

Is dark matter visible by galactic gamma rays?

The EGRET excess in the diffuse galactic gamma ray data above 1 GeV shows all features expected from dark matter WIMP annihilation: (a) It is present and has the same spectrum in all sky directions, not just in the galactic plane. (b) The intensity of the excess shows the 1/r ² profile expected for a flat rotation curve outside the galactic disc with an additionally interesting substructure in the disc in the form of a doughnut-shaped ring at 14 kpc from the centre of the galaxy. At this radius a ring of stars indicates the probable infall of a dwarf galaxy, which can explain the increase in DM density. From the spectral shape of the excess the WIMP mass is estimated to be between 50 and 100 GeV, while from the intensity the halo profile is reconstructed. Given the mass and intensity of the WIMPs the mass of the ring can be calculated, which is shown to explain the peculiar change of slope in the rotation curve at about 11 kpc. These results are model-independent in the sense that only the known shapes of signal and background were fitted with free normalization factors, thus being independent of model-dependent flux calculations. The statistical significance is more than 10σ in comparison with a fit of the conventional galactic model to the EGRET data. These signals of dark matter annihilation are compatible with supersymmetry including all electroweak constraints. The statistical significance combined with all features mentioned above provide an intriguing hint that the EGRET excess is indeed a signal from dark matter annihilation.     

A linear theory of resonance structures in spiral galaxies

The resonance mechanism for the formation of galactic spirals is considered. Expressions are derived for the resonance responses of disks with circular and nearly circular stellar orbits. The spiral responses produced by the central oval-shaped structures (bars) available in many galaxies are shown to have the characteristic properties of the spirals observed in these galaxies. In the most interesting case of a quasi-steady state, the spiral responses possess a similarity property: the spiral thickness and inclination are proportional to the mean size of an epicycle (an analog of the Larmor circle in plasma).     

LAMOST medium-resolution spectroscopic survey of binarity and exotic star (LAMOST-MRS-B): Observation strategy and target selection

LAMOST-MRS-B is one of the sub-surveys of LAMOST medium-resolution ($R\sim7500$) spectroscopic survey. It aims at studying the statistical properties (e.g., binary fraction, orbital period distribution, mass ratio distribution) of binary stars and exotic stars. We intend to observe about 30000 stars ($10 {\rm mag}\leq G < 14.5$ mag) with at least 10 visits in five years. We first planned to observe 25 plates around the galactic plane in 2018. Then the plates were reduced to 12 in 2019 because of the limitation of observation. At the same time, two new plates located at the high galactic latitude were added to explore binary properties influenced by the different environments. In this survey project, we set the identified exotic and low-metallicity stars with the highest observation priorities. For the rest of the selected stars, we gave the higher priority to the relatively brighter stars in order to obtain high quality spectra as many as possible. Spectra of 49129 stars have been obtained in LAMOST-MRS-B field and released in DR8, of which 28828 and 3375 stars have been visited more than twice and ten times with $\rm SNR \geq 10$, respectively. Most of the sources are B-, A-, and F-type stars with $\rm -0.6< [Fe/H] < 0.4 $ dex. We also obtain 347 identified variable and exotic stars and about 250 stars with $\rm [Fe/H] <-1$ dex. We measure radial velocities (RVs) by using 892233 spectra of the stars. The uncertainties of RV achieve about $1$ ${\rm km \cdot s^{-1}}$and $10$ ${\rm km \cdot s^{-1}}$ for 95% of late- and early-type stars, respectively. The datasets presented in this paper are available at http://www.doi.org/10.57760/sciencedb.j00113.00035.     

共振Kuiper带天体轨道稳定性的数值模拟

对当前观测到的具有可靠轨道根数的共振Kuiper带天体的轨道未来演化进行数值模拟发现,它们的轨道在一亿年的时间演化中具有相对稳定性,即仍处于各自的共振区中,但稳定程度不同,且共振天体的轨道稳定性和其初始轨道半长径、偏心率和倾角有关.根据其轨道半长径、偏心率和倾角随时间的演化行为,这些共振天体可以分为具有"规则轨道"和"混沌轨道"两种类型.     

Finslerian post-Riemannian corrections to the equations of geodesics

The generalization of the ordinary hypothesis of Riemannian geodesics for test bodies motion to the hypothesis of Finslerian geodesies gives rise to observable consequences which can explicitly be described in the case of the static gravitational field. The Finslerian corrections prove to be those in the velocity of motion and lead, in particular, to centennial changes in the eccentricities of the planetary orbits. The residual change in the eccentricity of the Mercurian orbit unexplainable by the Riemannian post-Newtonian corrections is used to estimate the order of a characteristic Finslerian parameter.     

Quiet starts for galaxy simulations

The ability of computer simulations to reproduce the normal modes of disc galaxies is assessed. Two types of disc are studied: one in which all stars move initially on circular orbits and a second case in which stars have a broad distribution of initial velocities causing them individually to follow eccentric orbits. Quiet start procedures are developed and found to be advisable for both cases. The observed mode frequencies in the cold disc models are within 2% of the linear theory values while discrepancies of 10% arise in the warm disc models. Nonquiet starts can lead to errors in excess of 50% when the same number of particles is used. The polar grid used for the simulations is shown to have further advantages over conventional Cartesian grids.     

Galactic Metrics

The paths of stars in galaxies have circular velocity independent of their distance from the centre of the galaxy. Newtonian mechanics with a logarithmic potential has such paths. In relativity these paths can be taken to be geodesics and this requirement places a restricting equation on the spacetime metric. This equation has a non-unique spherically symmetric solution that in the Newtonian limit has a logarithmic potential. It also can be solved in terms of a conformal factor. In particular it has solutions which are conformal to the vacuum-Einstein solutions and such spacetimes are solutions to the vacuum-Bach equations. Therefore it is suggested that the Bach equations describe dynamics on galactic length scales.     

Dark matter in galaxies and the growth of giant black holes

The relationship of dark matter to giant black holes (BHs) in galactic nuclei is investigated. The simultaneous evolution of dark and baryonic matter under the effect of an averaged self-consistent gravitational field is considered. The distribution of dark matter is shown to remain spherically symmetric even if there is an appreciable asymmetry in the distribution of baryonic matter in the galaxy. A kinetic equation that describes the evolution of the distribution function for dark matter with gravitational scattering by stars is derived. A significant flux of dark matter on a seed BHe at the galactic center is shown to arise under these conditions. The law of growth of the seed BH via the absorption of dark matter has been established. The seed BH is shown to grow significantly, up to 10⁷–10⁸ M⊙, in the lifetime of the galaxy. Observational data are briefly analyzed, and the presented theory has been found to be in reasonable agreement with experimental data.

     

Hot cracks in rubber: origin of the giant toughness of rubberlike materials

We study crack propagation in rubberlike materials and show that the nonuniform temperature distribution which occurs in the vicinity of the crack tip has a profound influence on the crack propagation, and may strongly enhance the crack propagation energy G(v) for high crack velocities v. At very low crack-tip velocities, the heat produced at the crack tip can diffuse away, but already at moderate crack-tip velocities a very large temperature increase occurs close to the crack tip resulting in a "hot-crack" propagation regime. The transition between the low-speed regime and the hot-crack regime is very abrupt and may result in unstable crack motion, e.g., stick-slip motion or catastrophic failure.     

Galactic model of element formation

A cosmological model is presented that produces He, C, O, D, Li, Be, and B in their observed abundances without a Big Bang. The elements are produced during the 1.5-Gy formation period of a galaxy, with C, O, and other heavy elements produced by stars of M>12 M₃ , He by stars of 6 M_s<M<12 M_s, and D, Li, Be, and B by cosmic-ray reactions in a nearly pure H plasma halo. Thus, the model shows that the major elements used in astrophysical studies can be produced during galactic formation by exactly the same processes known to function today at much lower rates     

用面阵CCD模拟测定星光漂移的方案研究

在LAMOST焦面光纤定位系统预研中 ,在焦面板上采用面阵CCD跟踪测量亮星的位置及其漂移 ,以对焦面板进行定位。在实验室条件下 ,用光纤出射光斑代替星光 ,即在光纤一端耦合进光 ,并在另一端用面阵CCD接收光斑 ,以模拟实际中接收星光情况。并利用重心法和图像迭加技术对采集的光斑信号进行处理。结果表明 :用面阵CCD测量星光位置及其漂移具有重复精度高 ,稳定性好的特点 ,且通过图像迭加处理 ,可提高星光信号的信噪比。     

Eccentricity modulation of a close-in planet by a companion: Application to GJ 436 system

GJ 436b is a Neptune-size planet with 23.2 Earth masses in an elliptical orbit of period 2.64 days and eccentricity 0.16. With a typical tidal dissipation factor (Q′∼10⁶) as that of a giant planet with convective envelope, its orbital circularization timescale under internal tidal dissipation is around 1 Ga, at least two times less than the stellar age (> 3 Ga). A plausible mechanism is that the eccentricity of GJ 436b is modulated by a planetary companion due to their mutual perturbation. Here we investigate this possibility from the dynamical viewpoint. A general method is given to predict the possible locations of the dynamically coupled companions, including nearby/distance non-resonant or mean motion resonance orbits with the first planet. Applying the method to GJ 436 system, we find it is very unlikely that the eccentricity of GJ 436b is maintained at the present location by a nearby/distance companion through secular perturbation or mean motion resonance. In fact, in all these simulated cases, GJ 436b will undergo eccentricity damp and orbital decay, leaving the present location within the stellar age. However, these results do not rule out the possible existence of planet companions in nearby/distance orbits, although they are not able to maintain the eccentricity of GJ 436b. Supported by the National Natural Science Foundation of China (Grant Nos. 10833001 and 10778603) and the National Basic Research Program of China (Grant No. 2007CB4800)     

Charged particle trajectories in a magnetic field on a curved space-time

In this paper we have studied the motion of charged particles in a dipole magnetic field on the Schwarzscbild background geometry. A detailed analysis has been made in the equatorial plane through the study of the effective potential curves. In the case of positive canonical angular momentum the effective potential has two maxima and two minima giving rise to a well-defined potential well rear the event horizon. This feature of the effective potential categorises the particle orbits into four classes, depending on their energies. (i) Particles, coming from infinity with energy less than the absolute maximum ofV _eff, would scatter away after being turned away by the magnetic field. (ii) Whereas those with energies higher than this would go into the central star seeing no barrier. (iii) Particles initially located within the potential well are naturally trapped, and they execute Larmor motion in bound gyrating orbits. (iv) and those with initial positions corresponding to the extrema ofV _eff follow circular orbits which are stable for non-relativistic particles and unstable for relativistic ones. We have also considered the case of negative canonical angular momentum and found that no trapping in bound orbits occur for this case. In the case when particles are not confined to the equatorial plane we have found that the particles execute oscillatory motion between two mirror points if the magnetic field is sufficiently high, but would continuously fall towards the event horizon otherwise. An erratum to this article is available at .     

The high-energy heavy-particle fluences in the orbits of manned space stations

The results are presented of measurements high-energy particles in a customary manned space station orbit (a 350-450-km altitude, a 51.6 degrees inclination; Salyut-6 and 7, MIR). The particles were recorded by the chambers composed of the Lavsan (polyethyleneterephtalate) solid-state nuclear track detector layers mounted outside a spacecraft for 1-3 years. A high resolution has been attained in the charge and energy spectra of 30-200 MeV/n Fe group particles. The results of measuring the particle fluxes in the space station orbits are used to restore the initial particle energy spectra in terms of the models that describe the galactic and solar cosmic rays and their penetration to the Earth's magnetosphere. The analysis demonstrates a high effectiveness of the described methods when applied to quite a number of space physics problems.     

Dynamic Equations for Tachyon Gas

Dynamics of the tachyon gas is considered. It is interesting in the relation, that dark matter phenomenon is explained freely by existence of the tachyon gas. Tachyons have two unexpected properties: (1) a single tachyon cannot be detected and (2) the tachyon gas can be detected by its gravitational field. Although molecules (tachyons) of the tachyon gas moves with superluninal velocities, the mean motion of these molecules appears to be less, than the speed of the light. The tachyon gas properties differs from those of usual gas. The pressure of the tachyon gas is very high. It is not isotropic and depends on the gravitational potential. As a result the tachyon gas may form huge halos around galaxies. These halos have very large and almost constant density. This circumstance can explain the law of star velocities at the periphery of a galaxy. Properties of the tachyon gas admit one to consider it as a dark matter.     

ON THE NEUTRINO MASS AND THE HIDDEPI MASS IN CELESTIAL BODIES

We continually use the phenomenological of the galaxy with two constituents (v+B) as in a previous paper ^[1] and uniformly handle S galaxy, E galaxy, etc. through the normalization method. At the same time, we extend this model from degenerate condition to isoentropic condition and from low temperature to high temperature. Thus, on a much more perfect foundation it is indirectly verified that the massive neutrino can account for the missing mass hidden in different celestial scales between galaxy and galactic cluster, but it can not rule out the possibiilty that there are some new massive fermions which are lighter than neutrino. Besides, in this paper we handle 21 samples of Sc galaxy yet, and obtain the average upper limit (15 eV.) of m_v. Because the spherically symmetric model is insufficient for calculation of m_v, we will progres sively research the non-spherically symmetric model, in another paper.