Simulating the Background Noise in the LEGRI CZT Detectors

A Monte-Carlo model of the MINISAT 01 satellite has been built. Thismodel, based on the GEANT software suite, is used to study the backgroundnoise induced in the cadmium zinc telluride (CZT) in the LEGRI detector.We find that the background noise count rate at the poles is 50%higher than at the equator. This increase is due to the effects of geomagneticrigidity cut-off. We also simulate the effects of passages through theSouth Atlantic Anomaly (SAA) with simulations showing an increase of 0.5 counts cm^-2 sec^-1 after the SAA, in good agreement withobservational data.     

The Direct and Indirect Methods of Ionospheric TEC Predictions and Their Comparison

The direct and indirect methods for predicting the ionospheric total electron content (TEC) by using the ARIMA (p, d, q) model in the theory of time-series analysis are proposed. The direct method predicts directly the time series composed of the TECs at the every grid point. The indirect method is: at first, to fit the ionospheric TECs with the spherical harmonics and obtain the time series of the fitting coefficients; then, to predict forward the fitting coefficients with the ARIMA (p, d, q) model in the theory of time-series analysis; and finally, to calculate the TEC for the specific time and grid point. Using the ionospheric data of the International GPS Service (IGS) in the period from 1 January 2004 to 31 January 2005, the testing and comparisons on the proposed methods are performed, the results indicate that within 12 days, the results of the two methods are basically consistent, and that for the predictions longer than 12 days, the accuracy of the indirect method is higher than the direct method. In the duration of 20 days, relative to the total ionospheric grid points, the percentage of the grid points with a prediction error less than 3 TECUs is about 80%; as the duration becomes longer, compared with the indirect method, the decline of this percentage is not apparent for the direct method. Obviously, the direct method suits the prediction of regional TECs, and the indirect method suits the prediction of global TECs.     

Comparative Analysis of Prominence Magnetic Field Measurements: Differences in Results Between Zeeman and Hanle Measurements

Results of magnetic field measurements in prominences using the Zeeman and Hanle methods are discussed critically. By considering an example of three prominences, for which magnetic field data from both methods are available, the discrepancies between the methods are demonstrated. The authors believe that the existing Hanle method does not reflect adequately the actual reality. To overcome the discrepancies calls for comparative analysis of prominence magnetic field measurements by both methods.     

Estimates of Extragalactic Background and Confusion Noise Parameters for the Millimetron Telescope

Astronomy Letters - The sensitivity of future far-infrared telescopes, such as Millimetron, will be limited by the confusion noise produced by distant galaxies. We have constructed a model of the...     

Theoretical and Experimental Studies of Radiative Shocks

This paper deals with the radiative shock from both theoretical and numerical points of view. It is based on the whole experimental results obtained at Laboratoire d'Utilisation des Lasers Intenses (LULI, école Polytechnique). Radiative shocks are high-Mach number shocks with a strong coupling between radiation and hydrodynamics which leads to a structure governed by a radiative precursor. These shocks are involved in various astrophysical systems: stellar accretion shocks, pulsating stars, interaction between supernovae and the interstellar medium. In laboratory, these radiative shocks are generated using high power lasers. New diagnostics have been implemented to study the geometrical shape of the shock and the front shock density. Data were obtained varying initial conditions for different laser intensities and temperature. The modeling of these phenomena is mainly performed through numerical simulations (1D and 2D) and analytical studies. We exhibit results obtained from several radiative hydrodynamics codes. As a result, it is possible to discuss about the influence of the geometry and physical parameters introduced in the 1D and 2D models.     

On the Nature of the Object HD 209458b: Conclusions Drawn from Comparison of Experimental and Theoretical Data

The experimental data obtained in transit observations of the extrasolar planet HD 209458b and their comparison with theoretical inferences have led to the conclusions that HD 209458b (and other similar hot jupiters) is of a (mainly) hydrogen nature and that these objects probably possess strong magnetic fields. The results of the studies of HD 209458b and prospects for searches for the transits of other extrasolar planets are considered in detail.     

Relation Between Coronal Hole Areas and Solar Wind Speeds Derived from Interplanetary Scintillation Measurements

We investigate the relation between coronal hole (CH) areas and solar wind speeds during 1995?–?2011 using the potential field (PF) model analysis of magnetograph observations and interplanetary scintillation (IPS) observations by the Institute for Space-Earth Environmental Research (formerly Solar-Terrestrial Environment Laboratory) of Nagoya University. We obtained a significant positive correlation between the CH areas (\(A\)) derived from the PF model calculations and solar wind speeds (\(V\)) derived from the IPS observations. The correlation coefficients between them are usually high, but they drop significantly in solar maxima. The slopes of the \(A\)?–?\(V\) relation are roughly constant except for the period around solar maximum, when flatter or steeper slopes are observed. The excursion of the correlation coefficients and slopes at solar maxima is ascribed partly to the effect of rapid structural changes in the coronal magnetic field and solar wind, and partly to the predominance of small CHs. It is also demonstrated that \(V\) is inversely related to the flux expansion factor (\(f\)) and that \(f\) is closely related to \(A^{-1/2}\); hence, \(V \propto A^{1/2}\). A better correlation coefficient is obtained from the \(A^{1/2}\)?–?\(V\) relation, and this fact is useful for improving space weather predictions. We compare the CH areas derived from the PF model calculations with He i 1083 nm observations and show that the PF model calculations provide reliable estimates of the CH area, particularly for large \(A\).     

TM65 m射电望远镜低频段系统噪声温度测试和分析

首先介绍了天马65 m射电望远镜(简称TM65 m)接收系统,包括L、S、C、X 4个频段各部分的噪声指标.然后对系统噪声温度的几种测试方法进行了讨论;对影响系统噪声温度测量的若干关键因素进行了分析,包括非线性误差、馈源网络插入损耗和失配误差等.采用Y因子法对试验室的噪声源定标值进行了校核,校核后偏差达到0.2 K左右.最后给出了TM65 m 4个低频段系统噪声温度的实测结果,并进行了分析.     

Comparison OF Noise Properties Of GONG And MDI Time-Distance Helioseismic Data

The recently upgraded system of the ground-based Global Oscillation Network Group (GONG) network of helioseismic observatories has started to provide higher-resolution solar oscillation measurements suitable for local helioseismic studies. Selecting simultaneously observed regions on the Sun by both GONG and the space-borne Michelson Doppler Imager (MDI) instrument on board the Solar and Heliospheric Observatory (SOHO), we perform a comparative analysis of time-distance measurements focussing on the noise properties.     

New Experimental and Theoretical Techniques for Studying Photochemical reactions of Cometary Atmospheres

New experimental methods for studying photochemical reactions aregiven and the strength and weakness are briefly discussed. References and bibliographies for these photochemical studies are presented. A case study of carbon disulfide (CS₂) that uses vacuum ultraviolet lasers, time-of-flight mass spectrometry, molecular beams and ion velocity imaging to measure andcharacterize the products is described. These results are compared with previous studies and the difficulties involved in understanding these results are pointed out.     

Resolving Differences in Absolute Irradiance Measurements Between the SOHO/CELIAS/SEM and the SDO/EVE

The Solar EUV Monitor (SEM) onboard SOHO has measured absolute extreme ultraviolet (EUV) and soft X-ray solar irradiance nearly continuously since January 1996. The EUV Variability Experiment (EVE) on SDO, in operation since April of 2010, measures solar irradiance in a wide spectral range that encompasses the band passes (26?–?34 nm and 0.1?–?50 nm) measured by SOHO/SEM. However, throughout the mission overlap, irradiance values from these two instruments have differed by more than the combined stated uncertainties of the measurements. In an effort to identify the sources of these differences and eliminate them, we investigate in this work the effect of reprocessing the SEM data using a more accurate SEM response function (obtained from synchrotron measurements with a SEM sounding-rocket clone instrument taken after SOHO was already in orbit) and time-dependent, measured solar spectral distributions – i.e., solar reference spectra that were unavailable prior to the launch of the SDO. We find that recalculating the SEM data with these improved parameters reduces mean differences with the EVE measurements from about 20 % to less than 5 % in the 26?–?34 nm band, and from about 35 % to about 15 % for irradiances in the 0.1?–?7 nm band extracted from the SEM 0.1?–?50 nm channel.     

Galileo系统和区域增强导航系统的定位误差比较

采用最小二乘协方差方法分别对Galileo系统的定位误差和中国区域导航增强系统的定位误差的计算进行定义,并通过matlab编程仿真比较得出:区域增强导航系统的定位误差只有Galileo系统定位误差的三分之一。表明,如果能建立区域增强导航系统将在较大程度上提高中国区域的导航能力。     

二体问题状态转移矩阵的分析解和数值解的比较

对二体问题的状态传播问题, 以Ａｊｉｓａｉ 卫星某历元的初轨为例,考虑５ｄ （ 天） 、１０ｄ （ 天） 和１００ｄ （ 天） 间隔的弧长, 本文分别给出了它们的分析解和数值解。结果表明： 对应于５ｄ、１０ｄ、１００ｄ 间隔的弧长, 二体问题状态转移的分析解与数值解在１０－１０ 、１０ －８ 和１０－７ 以内的相对偏差下能够保持其一致性。     

Cosmic-Ray Spectrum Approximation Model: Experimental Results and Comparison with Other Models

We discuss a model which parameterizes the cosmic-ray (CR) spectrum at different physical conditions, which include the most important effects controlling the CR intensity, like convection–diffusion and energy losses. By a suitable choice of parameters the proposed model results in two approximations: one close to a “force–field” model (describing the energy losses of CRs in the inner heliosphere) and a “convection–diffusion” equation (giving the reduction of CR intensity in the outer heliosphere). The BESS (Balloon-borne Experiment with Superconducting Spectrometer) experimental spectra of galactic protons and helium nuclei are fitted by the model spectra. The calculation of the unknown parameters is performed using a constrained least squares method as an alternative to the standard chi-square minimization method, because the data contain not only random errors, but also systematic ones. The CR spectrum approximation (CRSA) model is compared to the Moscow State University (MSU) model and the Badhwar and O’Neill (Badhwar and O’Neill, Adv. Space. Res. 14, 749, 1994; Adv. Space Res. 17, 7, 1994) model; we show that depending on the choice of the model parameters it can be examined in the context of one of these two models. We derive a relation between the parameters of the CRSA and MSU models for rigidities above about 10 GV (drift effects are ignored) during periods of low to approximately average levels of solar activity. The drawbacks of the proposed approximation are that: i) the model parameters do not depend on rigidity and ii) the model does not take into account general trends in the variations of the heliospheric magnetic field; thus, the influence of the drift effects on the shape of the spectral curves for different magnetic field polarity swings is ignored.     

A Comparison of Theoretical Si VIII Emission Line Ratios with Observations from Serts

Recent R-matrix calculations of electron impact excitation rates in N-like Si VIII are used to derive theoretical emission line intensity ratios involving 2s ²2p ³–2s2p ⁴ transitions in the 216–320 Å wavelength range. A comparison of these with an extensive dataset of solar active region, quiet-Sun, sub-flare and off-limb observations, obtained during rocket flights of the Solar EUV Research Telescope and Spectrograph (SERTS), indicates that the ratio R ₁= I(216.94 Å)/I(319.84 Å) may provide a usable electron density diagnostic for coronal plasmas. The ratio involves two lines of comparable intensity, and varies by a factor of about 5 over the useful density range of 10⁸–10¹¹ cm^?3. However R ₂= I(276.85 Å)/I(319.84 Å) and R ₃=I(277.05 Å)/I(319.84 Å) show very poor agreement between theory and observation, due to the severe blending of the 276.85 and 277.05 Å lines with Si VII and Mg VII transitions, respectively, making the ratios unsuitable as density diagnostics. The 314.35 Å feature of Si VIII also appears to be blended, with the other species contributing around 20% to the total line flux.

     

A Comparison of Theoretical mgvi Emission Line Strengths with Active-Region Observations From Serts

R-matrix calculations of electron impact excitation rates in N-like Mgvi are used to derive theoretical electron-density-sensitive emission line ratios involving 2s ²2p ³–2s2p ⁴transitions in the 269–403 Å wavelength range. A comparison of these with observations of a solar active region, obtained during the 1989 flight of the Solar EUV Rocket Telescope and Spectrograph (SERTS), reveals good agreement between theory and observation for the 2s ²2p ^{3 4} S–2s2p ^{4 4} Ptransitions at 399.28, 400.67, and 403.30 Å, and the 2s ²2p ^{3 2} P–2s2p ^{4 2} Dlines at 387.77 and 387.97 Å. However, intensities for the other lines attributed to Mgvi in this spectrum by various authors do not match the present theoretical predictions. We argue that these discrepancies are not due to errors in the adopted atomic data, as previously suggested, but rather to observational uncertainties or mis-identifications. Some of the features previously identified as Mgvi lines in the SERTS spectrum, such as 291.36 and 293.15 Å, are judged to be noise, while others (including 349.16 Å) appear to be blended.     

Predictions for the frequency and orbital radii of massive extrasolar planets

We investigate the migration of massive extrasolar planets caused by gravitational interaction with a viscous protoplanetary disc. We show that a model in which planets form at 5 au at a constant rate, before migrating, leads to a predicted distribution of planets that is a steeply rising function of log( a ), where a is the orbital radius. Between 1 and 3 au, the expected number of planets per logarithmic interval in a roughly doubles. We demonstrate that, once selection effects are accounted for, this is consistent with current data, and then extrapolate the observed planet fraction to masses and radii that are inaccessible to current observations. In total, approximately 15 per cent of stars targeted by existing radial velocity searches are predicted to possess planets with masses  0.3< M _p sin( i )<10 M _J  and radii  0.1< a <5 au  . A third of these planets (around 5 per cent of the target stars) lie at the radii most amenable to detection via microlensing. A further  5–10  per cent of stars could have planets at radii of  5< a <8 au  that have migrated outwards. We discuss the probability of forming a system (akin to the Solar system) in which significant radial migration of the most massive planet does not occur. Approximately  10–15  per cent of systems with a surviving massive planet are estimated to fall into this class. Finally, we note that a smaller fraction of low-mass planets than high-mass planets is expected to survive without being consumed by the star. The initial mass function for planets is thus predicted to rise more steeply towards small masses than the observed mass function.     

Predictions on finding the SiH+ and SiH in interstellar space

Observations by Dressler are used to derive integral luminosity functions for ten rich clusters. All luminosity functions are found to consist of a linear portion and a high-luminosity toe. The size of this toe does not appear to correlate with cluster BM type. A parameterM _F (0), which has a dispersion of only 0.2 mag for the present data sample, is defined.     

用于守时工作的时间间隔计数法与双混频时差测量比对法的比较

为了比较用于守时工作的时间间隔计数法和双混频时差测量法,分析了国家授时中心时频基准实验室的两种测量比对设备(SR620时间间隔计数器和PCOMP多通道相位比较仪)对同一组原子钟进行测量时所得到的结果(钟的速率、RMS、测量精度和稳定度)。分析所得的主要结论是:双混频时差测量法具有更高的比对精度,更适用于氢原子钟短期(τ≤5 d)稳定度的测量。