初至折射波静校正技术在复杂探区地震数据处理中的应用

山区及黄土塬地区近地表结构复杂，地形起伏大、低降速带横向变化剧烈，地震资料处理中的静校正难度加大。长波长静校正容易引起构造形态畸变，短波长静校正影响地震剖面信噪比。针对此类问题，从长波长静校正问题及短波长地表非一致性问题分析入手，提出部分炮检距叠加识别长波长静校正技术及分段统计逼近地表非一致性校正技术。该技术在复杂地表区与其它相关技术综合应用，可有效解决长、短波长静校正问题。     

BDS中长距离非差实时动态厘米级定位算法

针对BDS常规实时动态定位(RTK)中,随着流动站与参考站间的距离增加,大气延迟误差的空间相关性大大降低,影响了整周模糊度的快速解算和流动站位置信息的解算精度问题。该文研究了一种基于非差观测误差的BDS中长距离常规RTK定位算法,采用非差误差改正方法为流动站提供误差改正,利用参考站的非差误差改正数以单颗卫星为对象进行误差改正。对电离层延迟误差和相对天顶对流层延迟误差进行参数估计,处理电离层延迟误差和对流层延迟误差的影响。最后通过BDS实测数据对该算法进行了算法验证和结果分析。实验结果表明,该算法可以实现BDS中长距离常规RTK的快速定位,并获得厘米级定位精度。     

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中国大陆及华北地区地震资料的小波分析

基于地震活动为多尺度多活动这一观点，运用小波变换方法，以不同的小波尺度分析了中国大陆1900～2001年和华北地区1500～2001年M≥5地震的本尼奥夫应变资料，得到了各种层次地震活跃期和平静期，分析结果可信而又符合实际。对历史地震研究和地震危险性预测具有一定的参考价值。     

基于循环神经网络的重力异常数据推估研究

利用鄂尔多斯西南缘的重力观测数据对长短期记忆循环神经网络(long short-term memory,LSTM)进行训练,结果表明,该神经网络可基于有限的数据获取较好的推估结果.基于自由空气重力异常数据,对比分析长短期记忆循环神经网络和传统克里金方法的推估结果发现,神经网络的推估能力优于传统克里金方法,但运算效率低于...     

Accretion stream mapping of HU Aquarii

We present a new mapping algorithm, the Accretion Stream Mapping (ASM), which uses the full phase-coverage of a light curve to derive spatially resolved intensity distributions along the accretion stream in magnetic cataclysmic variables of AM Herculis type (polars). The surface of the accretion stream is approximated as a 12-sided (duodecadon-shaped) tube. After successfully testing this method on artificial data we applied it to emission-line light curves of H β , H γ and He  ii λ 4686 of the bright eclipsing polar HU Aqr. We find hydrogen and helium line emission bright in the threading region of the stream where the stream couples on to magnetic field lines. It is particularly interesting that the stream is bright on the irradiated side facing the white dwarf, which highlights the interplay of collisional and radiative excitation/ionization.     

Recent discoveries of supersoft X‐ray sources in M 31

Classical novae (CNe) have recently been reported to represent the major class of supersoft X‐ray sources (SSSs) in the central area of our neighbouring galaxy M 31. This paper presents a review of results from recent X‐ray observations of M 31 with XMM‐Newton and Chandra. We carried out a dedicated optical and X‐ray monitoring program of CNe and SSSs in the central area ofM 31. We discovered the first SSSs in M 31 globular clusters (GCs) and their connection to the very first discovered CN in a M 31 GC. This result may have an impact on the CN rate in GCs. Furthermore, in our optical and X‐ray monitoring data we discovered the CN M3 1N 2007‐11a, which shows a very short SSS phase of 29–52 days. Short SSS states (durations ≤ 100 days) of CNe indicate massive white dwarfs (WDs) that are candidate progenitors of supernovae type Ia. In the case of M31N 2007‐11a, the optical and X‐ray light curves suggest a binary containing a WD with M_WD > 1.0 M_⊙. Finally, we present the discovery of the SSS counterpart of the CN M31N 2006‐04a. The X‐ray light curve of M31N 2006‐04a shows short‐time variability, which might indicate an orbital period of about 2 hours (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

K-band spectroscopy of the intermediate polar XY Ari

We present the K -band infrared spectrum of the intermediate polar XY Ari. The spectrum confirms the cataclysmic binary nature of XY Ari, showing emission lines of He  i ( λ 2.0587 μm) and the Brackett and Paschen series of H  i . The broad nature of these lines suggests an origin in an accretion disc. The spectrum is strongly reddened by absorption within the molecular cloud Lynds 1457 and shows prominent absorption features from the secondary star, from which we determine a spectral type for the secondary of M0V. The secondary contributes     per cent of the K -band light. We derive a visual extinction to XY Ari of     and a distance of     , placing XY Ari behind the molecular cloud.     

The β Cephei instability strip

We carried out a series of linear stability analyses of the radial and low-degree non-radial p modes for stellar models with initial masses of     . The stellar models were computed by using convective overshoot distance     , 0.25 and 0.40  H _P. Our numerical results show that the β Cephei instability strip forms a horn-shaped region pointing upwards near the main sequence on the Hertzsprung–Russell diagram (HRD). The lower part of the instability strip for the radial modes join the zero-age main-sequence (ZAMS) at     , while the top of the instability strip extends up to     . The instability strip for the non-radial modes is even wider. The overall instability strip is dominated by the radial and non-radial fundamental modes. The first overtone (the radial-order index     is also pulsationally unstable. We have shown that the β Cephei stability is almost independent of the overshoot parameter d _over used for the stellar models, while it depends critically on the metal abundance. With decreasing metal abundance, the instability region shrinks and eventually disappears for     .     

The re-analysis of the ROSAT data of Nova Mus 1983 using white dwarf atmosphere emission models

The analyses of X-ray emission from classical novae during the outburst stage have shown that the soft X-ray emission below 1 keV, which is thought to originate from the photosphere of the white dwarf, is inconsistent with the simple blackbody model of emission. Thus, ROSAT Position Sensitive Proportional Counter (PSPC) archival data of the classical Nova Mus 1983 (GQ Mus) have been re-analysed in order to understand the spectral development in the X-ray wavelengths during the outburst stage. The X-ray spectra are fitted with the hot white dwarf (WD) atmosphere emission models developed for the remnants of classical novae near the Eddington luminosity. The post-outburst X-ray spectra of the remnant white dwarf are examined in the context of evolution on the Hertzsprung–Russell diagram using C–O enhanced atmosphere models. The data obtained in 1991 August (during the ROSAT All Sky Survey) indicate that the effective temperature is         . The 1992 February data show that the white dwarf had reached an effective temperature in the range         with an unabsorbed X-ray flux (i.e. ∼ bolometric flux) between     and     . We show that the H burning at the surface of the WD had most likely ceased at the time of the X-ray observations. Only the 1991 August data show evidence for ongoing H burning.