The dust envelope of R CrB in June 2001: Detection of a compact IR source

We present the results of a joint analysis of JHK interferometric and UBVJHKLM photometric observations of RCrB acquired in June 2001. The baseline for the IOTA interferometer was 21.18 m. During the observations, the star was in its bright state in the V band and near its maximum brightness in the L band. Our analysis reveals an IR source that is considerably smaller than the extended dust envelope discovered earlier. We identify this compact IR source with the emission from a group of dust clouds. The linear scale (diameter) of the IR source was d _in,c ≈ 13.5D_* (its angular diameter is θ_in,c≈6.4 mas). About 7% of the star’s radiation was obscured by this group of clouds, which contributed ～14% of the total IR excess of R CrB and ～22% of the K-band flux. The color temperature of the compact source was only ～300 K higher than the color temperature of the extended dust envelope. The inner boundary of the extended dust envelope had a diameter of d _in,e ≈ 90D_* (θ_in,e≈43 mas).     

The dust envelope of the symbiotic nova HM Sge

We have studied the brightness and color variations of the symbiotic nova HM Sge based on longterm UBVRJHKLM photometry of the star and data on its energy distribution in the middle infrared (7.7–22.7 µm) obtained with the low-resolution spectrometers of the IRAS satellite and ISO orbital observatory. We have also calculated models for the steady-state, spherically symmetrical, extended dust envelope of the star for two extreme heating cases: heating only by radiation from the cool component of the system and by the combined radiation from both components. Model fitting to the IRAS and ISO data indicates that models with a single, central Mira-type source are more appropriate. This indicates that the radiation of the hot component is largely processed by the surrounding gas, and does not substantially affect the infrared spectrum of the symbiotic nova directly. The mean spectral energy distribution based on 1983 IRAS data differs appreciably from the ISO spectrum obtained on October 1, 1996. The observed evolution of the envelope spectrum probably reflects an increase of the density and decrease of the temperature of the dust grains near the inner boundary of the envelope, related to a decrease of the luminosity and increase of the temperature of the hot component. We estimate the total mass-loss rate, velocity of gas expansion at the outer envelope boundary, and upper limit for the mass of the central source of radiation.     

The dust envelope of the symbiotic nova V1016 Cyg

Brightness and color variations of V1016 Cyg are studied using many years of UBVRJHKLM photometric observations and information about its spectral energy distribution in the intermediate IR (7.7 to 22.7 µm) obtained with the IRAS and ISO low-resolution spectrometers. Models for its stationary, spherically symmetrical, extended dust envelope are computed for two cases of heating: by the radiation of the cool component only and by the combined radiation from both components. Model fitting of the IRAS and ISO observations shows that the model with a single central source—the Mira star—provides a better fit to the data, indicating that the hot component’s radiation is appreciably reprocessed by the ambient gas medium and has almost no direct influence on the IR spectrum of the symbiotic nova. The mean spectral energy distributions measured by IRAS in 1983 and ISO on October 1, 1996, differ considerably. The observed evolution of the envelope’s spectrum probably reflects an increasing grain concentration and decreasing grain temperature at the inner edge of the envelope, associated with decreased luminosity and increased temperature of the hot component. The total mass-loss rate, gas-expansion velocity at the outer edge of the envelope, and upper limit to the mass of the central radiation source are estimated.     

Parameters of the dust envelope of the symbiotic star CH Cygni

The brightness and color variations of the symbiotic star CH Cygni are studied, and its stationary, spherically symmetric, extended dust envelope is modeled based on long-term UBVRJHKLM photometry, the mid-IR spectral energy distribution (7–23 µm), and far-IR fluxes measured by IRAS and ISO. The existence of a hot dust envelope, detected earlier in the near IR, is confirmed; the optical depth of the envelope has probably increased with time. Model fits to the IRAS and ISO data indicate that the V-band optical depth increased from 0.22 to 0.41 due to dust density enhancement during the 14 years between the observations by the two spacecraft. The mass-loss rate, gas-expansion velocity at the outer boundary of the envelope, and upper limit of the mass of the central source of emission are estimated assuming that the stellar wind of the system is driven by the pressure of the red giant's radiation on the dust, with subsequent momentum transfer to the gaseous medium.     

Models of the dust envelope of the unique object FG Sagittae

We use JHKLM photometric data obtained in 1998–2001 to model the dust envelope of the unique object FG Sge, which formed around the star after several consecutive cycles of dust condensation beginning in Autumn 1992. Models with a spherically symmetric, extended envelope consisting of a mixture of spherical particles of amorphous carbon and silicon carbide with an MRN size distribution were fitted to match the mean observed spectral energy distributions of FG Sge during brightness maximum and minimum after 1998 for two values of the luminosity and effective temperature of the central star. The stellar-wind parameters and mass-loss rate have been estimated in each case. The observational data for the brightness maximum and minimum cannot be described by models with a fixed luminosity or fixed distance to the star. This is a consequence of the object’s unusual behavior, with synchronous flux decreases in all the observed bands. The inability of the model to adequately describe the minimum-brightness state is probably associated with the abrupt disruption of the spherical symmetry of the envelope due to the formation of a small, dense dust cloud in the line of sight.     

Parameters for the dust envelope of the protoplanetary nebula IRAS 18062+2410

We have calculated a model for the dust envelope of the protoplanetary nebula IRAS 18062+2410 using observations from the ultraviolet to the far infrared. We assume that the envelope is spherically symmetrical and consists of identical silicate grains with a radius of 0.10 micron, and with the number density of the grains inversely proportional to the square of the distance. The optical depth of the envelope, whose inner boundary is 1.40×10^?3 pc from the center of the star, is 0.050 at 10 microns. At the inner envelope boundary, the temperature of the dust grains is 410 K and their density is 2.7×10^?7 cm^?3. Using calculations of stellar evolution at the stage following the exit from the asymptotic giant branch, we estimate the dust envelope’s expansion velocity to be 12 km/s. The mass-loss rate of the star preceding the ejection of the envelope was about 4.5×10^?6 M _⊙/yr. The observed excess of far-IR flux is not associated with the continuum radiation of the nebula, and may provide evidence for the presence of dust ejected by the star in earlier stages of its evolution.     

Variations of the parameters of the dust envelope of the symbiotic star CH Cygni

The results of JHKLM photometry of the symbiotic star CH Cyg are presented. These demonstrate that, in Autumn 2006, the state of maximum near-IR brightness observed in 2003–2006 was replaced by a sharp brightness decline in all wavebands. One possible explanation is a sharp increase in the density of circumstellar dust envelope. The JHKLM photometry data together with ISO far-IR flux measurements are used to calculate spherically symmetric dust-envelope models for the maximum and minimum brightness states. The optical depth, expansion rate, and mass-loss rate of the envelope are calculated for both states, as well as an upper limit for the mass of the central source. Comparison with earlier models suggests that the rate of growth of the envelope optical depth and the mass-loss rate by the star are accelerating with time.     

Dissipation of the hot dust envelope of CH Cygni (1996–2003)

Our analysis of JHKLM photometric data obtained in 1978–2003 for the CH Cyg system shows that the “local” dust envelope that formed in the system in 1986 and reached its highest column density in 1996 had largely dispersed by mid-2001, so that the observed brightness of the system’s red giant has returned to its pre-1985 level. The giant’s spectral type varied in the range M6.5–M7.5 in 2001–2003. The optical depth of the dust envelope at 1.25 µm was τ(J)≈0.83 near JD 2450090. The increase in the dust envelope’s optical depth was approximately a factor of 2.3 slower than the decrease. The envelope of CH Cyg can be pictured as a “stationary” dust cloud with an optical depth at λ=1.25 µm of ～0.4 and a dust-grain temperature of ～750–800 K. There was probably an injection of matter into this cloud toward the end of 1985, initiating the condensation of dust grains. The optical depth began to increase and, by 1991, the dust envelope was transformed from a cloud into a local, almost spherically-symmetric envelope with a grain temperature of 750–800 K. Its optical depth reached its maximum in 1996, after which the local envelope began to disperse, becoming a cloud again by 2001. The detected 4000-day variability of the JHK brightness of CH Cyg is in good agreement with a model with an eclipsing binary consisting of two cool giants with effective temperatures differing by approximately 100 K, a luminosity ratio of L(M7)/L(M6)～6.8, and a radius ratio of R(M7)/R(M6)～3.6. The orbital ephemeris is given by JD (Min I)=2444180+4000E.     

Infrared photometry of the carbon star RW LMi and an axisymmetric model for its dust envelope

We have developed an axisymmetric model for the dust envelope of the carbon star RW LMi with a density distribution typical for the superwind stage using JHKLM photometric data obtained in 1997–2003, supplemented by flux data at optical, mid-IR, and far-IR wavelengths. In contrast to earlier spherically-symmetric models, the model is able to reproduce the observed fluxes in all observed wavelength ranges, and provides a good agreement with the observational data. The estimated mass-loss rate is \(\dot M = 1.2 \times 10^{ - 5} M_ \odot /yr\). The computed brightness distribution of the envelope in the near-IR is in satisfactory agreement with high-resolution observations, while the optical size is considerably larger than is observed.     

Results of infrared photometry and a model for the dust envelope of the protoplanetary nebula candidate V1027 Cyg

Results of JHKLM photometry for the protoplanetary nebula candidate V1027 Cyg obtained in 1991–2008 are reported. In all bands, the brightness variations did not exceed 0.2 ^m . Estimated linear trends demonstrate no significant changes in the mean brightness and color indices of the object, with the possible exception of the L-M color index, which showed a small decrease. A search for possible periodicities in the brightness variations yielded the most probable period of 237^d. A model for a spherically-symmetric dust shell has been calculated based on the photometric results supplemented with data on the mid- and far-infrared fluxes. The estimated mass-loss rate of the star is 1.3 × 10⁻⁵ M _⊙/year.     

The mechanism of circumbinary envelope formation in close binaries

We consider the structure and formation of the circumbinary envelopes in semi-detached binary systems. Three-dimensional numerical simulations of the gas dynamics are used to study the flow pattern in a binary system after it has reached the steady-state accretion regime. The outer parts of the circumbinary envelope are replenished by periodic ejections from the accretion disk and circum-disk halo through the vicinity of the Lagrange point L₃. In this mechanism, the shape and position of a substantial part of the disk is specified by a precessional density wave. On timescales comparable to the orbital period, the precessional wave (and hence an appreciable fraction of the disk) will be virtually stationary in the observer’s frame, whereas the positions of other elements of the flow will vary due to the orbital rotation. The periodic variations of the positions of the disk and the bow shock formed when the inner parts of the circumbinary envelope flow around the disk result in variations in both the rate of angular-momentum transfer to the disk and the flow structure near L₃. All these factors lead to a periodic increase of the matter flow into the outer layers of the circumbinary envelope through the vicinity of L₃. The total duration of the ejection is approximately half the orbital period.     

The nature of molecular cloud material in interplanetary dust

Eight interplanetary dust particles (IDPs) exhibiting a wide range of H and N isotopic anomalies have been studied by transmission electron microscopy, x-ray absorption near-edge structure spectroscopy, and Fourier-transform infrared spectroscopy. These anomalies are believed to have originated during chemical reactions in a cold molecular cloud that was the precursor to the Solar System. The chemical and mineralogical studies reported here thus constitute direct studies of preserved molecular cloud materials. The H and N isotopic anomalies are hosted by different hydrocarbons that reside in the abundant carbonaceous matrix of the IDPs. Infrared measurements constrain the major deuterium (D) host in the D-enriched IDPs to thermally labile aliphatic hydrocarbon groups attached to macromolecular material. Much of the large variation observed in D/H in this suite of IDPs reflects the variable loss of this labile component during atmospheric entry heating. IDPs with elevated ¹⁵N/¹⁴N ratios contain N in the form of amine (-NH₂) functional groups that are likely attached to other molecules such as aromatic hydrocarbons. The host of the N isotopic anomalies is not as readily lost during entry heating as the D-rich material. Infrared analysis shows that while the organic matter in primitive anhydrous IDPs is similar to that observed in acid residues of primitive chondritic meteorites, the measured aromatic:aliphatic ratio is markedly lower in the IDPs.     

The evolution of hydrocarbon dust grains in the interstellar medium and its influence on the infrared spectra of dust

Computations of the evolution of the distributions of the size and degree of aromatization of interstellar dust grains, destruction by radiation and collisions with gas particles, and fragmentation during collisions with other grains are presented. The results of these computations are used to model dust emission spectra. The evolution of an ensemble of dust particles sensitively depends on the initial size distribution of the grains. Radiation in the considered range of fluxes mainly aromatizes grains. With the exception of the smallest grains, it is mainly erosion during collisions with gas particles that leads to the destruction of grains. In the presence of particle velocities above 50 km/s, characteristic for shocks in supernova remnants, grains greater than 20 Å in size are absent. The IR emission spectrum changes appreciably during the evolution of the dust, and depends on the adopted characteristics of the grains, in particular, the energy of their C–Cbonds (E₀). Aromatic bands are not observed in the near-IR (2–15 μm) when E₀ is low, even when the medium characteristics are typical for the average interstellarmedium in our Galaxy; this indicates a preference for high E₀ values. The influence of the characteristics of the medium on the intensity ratios for the dust emission in various photometric bands is considered. The I_3.4/I_11.3 intensity ratio is most sensitive to the degree of aromatization of small grains. The I_3.3/I₇₀₊₁₆₀ ratio is a sensitive indicator of the contribution of aromatic grains to the total mass of dust.     

The structure of the common envelope in a close binary system

As a result of the interaction between an elliptical accretion disk and gas flowing into it from the circumbinary envelope in a close binary in the course of its orbital motion, the matter of the disk and the circum-disk halo is periodically ejected from the vicinity of the Lagrange point L₃, and a common envelope is formed in the system. Three-dimensional numerical gas-dynamical modeling is used to study the structure and dynamics of the envelope and determine its basic parameters. The evolution of the envelope is followed on timescales of the order of several orbital periods. The matter flow ejected through the vicinity of L₃ displays a spiral shape. The maximum size of the forming spiral structure is restricted by the self-intersection point, and is of the order of four to five times the component separation. We consider the dynamics of the regions directly adjacent to the spiral structure: an inner, rarified and outer, fragmented region, which further makes a transition to an expanding diffuse ring.     

东北平原西部的碱性尘暴

每年冬春季节在东北平原的西部常有碱性尘暴发生。碱性尘暴是指地表碱性物质被风吹扬、在空中悬移造成的能见度低于1 000m 的灾害性天气现象。碱性尘暴以碱性物质为主, 并伴有一定的沙尘和盐尘物质, 是一种特殊类型的尘暴。碱性尘暴发生时, 白色的盐碱物质大面积地弥漫在空中随风迁移, 所到之处均披覆了一层白色的碱尘物质, 当地群众称这种碱性尘暴为∀ 刮白烟# 。早在20 世纪70 年代美国西部的Owen 和Mono 湖盆区就有关于碱性尘暴现象和其对人体健康影响的报道。碱性尘暴不仅造成土地沙化, 而且大量的碱性物质沉降在土壤表面造成了土地碱化, 使生态环境受到沙化和盐碱化的双重危害, 其对人体健康的影响更为严重。因此对碱性尘暴的成因和防治研究具有十分重要的意义。     

Physical Parameters of the Eclipsing System V1176 Cas

The first high-accuracy CCDUBV RI light curves for the recently discovered eclipsing system V1176 Cas (P = 6 _. ^d 33, V = 11 _. ^m 1) have been obtained. A photometric solution for the light curves and physical characteristics of the component stars are derived. The orbital eccentricity is negligible, e = 0.009; both components have physical parameters similar to the Sun, but they are younger and may have an overabundance of metals. The orientation of the orbital ellipse and the low eccentricity make studies of the apsidal motion difficult. Nevertheless, the high accuracy of the available measurements of the timings of minima has enabled derivation of an upper limit for the rate of apsidal rotation, which agrees with a theoretical estimate of this effect.     

兰州地区冬季非尘暴降尘通量初步观测

现代黄土高原上冬季非尘暴条件下的大气粉尘,主要由来自黄土物源区的远源粉尘和黄土高原本身的近源粉尘共同组成。它们各自的贡献如何,以往的研究均未做过明确的讨论。由于前者的浓度及其相应的降尘通量在较小空间内的分布是比较均匀的,而后者则往往存在显著的差异性,因此可以通过对某个小区域内不同地点降尘通量的比较和分析来推断其贡献的大小。若各点的通量均很接近,则当地的大气粉尘应以远源输入为主,而来源于本地的近源粉尘贡献很小,或者近源的大气粉尘在空间上的分布也是很均匀的;若各点的通量相差悬殊,则表明本地来源的粉尘对总降尘通量具有显著的影响,并且,由各观测点中的最小降尘通量还可以近似了解远源.     

黄土沉积物原生组分磁化率与风力的物质分选

本研究选取我国西北地区典型荒漠表土和黄土-古土壤序列样品为研究对象,探讨黄土沉积物及其潜在物源区表土的原生磁性矿物浓度在不同粒级间的变化规律、黄土剖面中粒度与磁化率的关系,以验证中国黄土沉积物中磁性组分在搬运过程中是否存在分选作用及其变化规律。来自西北地区表土的地质证据表明,磁性组分主要集中于>63 μm和31~63 μm粒径组分,并以后者的含量最高;与之相对应,黄土沉积中原生磁性组分主要集中于31~63 μm粒径组分,但>63 μm粒径组分不再是主要载磁组分,其磁性显著低于31~63 μm粒径组分。同时,多个剖面的证据表明黄土沉积的原生磁化率与31~63 μm粒径组分的含量是同相位变化的,进一步支持沉积物中原生组分的磁化率受到风动力的分选作用影响。需要强调的是,沉积物原生磁化率的主要载磁粒径组分为31~63 μm的颗粒物,而并非最粗粒组分。本研究结果暗示,相较于沉积物的全样粒度,干旱半干旱地区风成沉积的磁化率在指示古风场强度方面具有潜力。

     

成都经济区近地表大气尘地球化学基线

成都经济区近地表大气尘中重金属元素含量空间分布显示,经济区中东部高于西部,北部高于中南部,重工业城市高于综合性城市和旅游城市,工矿影响区元素含量总体偏高,人口密集的平原区高于山区。通过标准极限方法确定了近地表大气尘中元素的“极限浓度”,以低于“极限浓度”值统计确定了地球化学基线值：As为28.6mg/kg 、Hg 0.63mg/kg 、Cd 2.94mg/kg、Cr 110mg/kg、Pb 281mg/kg、Ni 32mg/kg、Zn 535mg/kg。近地表大气尘中元素地球化学基线与区域地质背景和矿产开发有关,矿业活动、工业活动及居民生活是造成近地表大气尘中人为扰动元素含量偏高的主要原因。     

成都经济区近地表大气尘地球化学基线

成都经济区近地表大气尘中重金属元素含量空间分布显示,经济区中东部高于西部,北部高于中南部,重工业城市高于综合性城市和旅游城市,工矿影响区元素含量总体偏高,人口密集的平原区高于山区。通过标准极限方法确定了近地表大气尘中元素的“极限浓度”,以低于“极限浓度”值统计确定了地球化学基线值：As为28.6mg/kg 、Hg 0.63mg/kg 、Cd 2.94mg/kg、Cr 110mg/kg、Pb 281mg/kg、Ni 32mg/kg、Zn 535mg/kg。近地表大气尘中元素地球化学基线与区域地质背景和矿产开发有关,矿业活动、工业活动及居民生活是造成近地表大气尘中人为扰动元素含量偏高的主要原因。