Occurrence of Cladosporium spp. and Alternaria spp. spores in Western, Northern and Central-Eastern Poland in 2004–2006 and relation to some meteorological factors

The concentration of airborne spores of Cladosporium spp. and Alternaria spp. has been investigated at three monitoring stations situated along the west-north and central-east transect in Poland (Szczecin, Olsztyn, Warszawa,) i.e. from a height of 100 m to 149 m above sea level. The aerobiological monitoring of fungal spores was performed by means of three Lanzoni volumetric spore traps.Cladosporium spp. spores were dominant at all the stations. The highest Cladosporium spp. and Alternaria spp. numbers of spores were observed at all the cities in July and August.Statistically significant correlations have been found between the Cladosporium spp. and Alternaria spp. concentration in the air and the mean air temperature, amount of precipitation, air pressure and relative air humidity. The spore count of Cladosporium spp. and Alternaria spp. is determined by the diversity of local flora and weather conditions, especially by the air temperature. The identification of factors, which influence and shape spore concentrations, may significantly improve the current methods of allergy prevention.     

甘肃酒泉区域风能资源评估

按照国家风电场风能资源评估方法,利用甘肃省酒泉区域6个测风塔不同高度层的资料,计算分析了该区域的各种风能参数,并给出了该区域风能的空间分布图.结果表明,按照我国学者的研究成果划分,除2号地区属于风能较丰富区以外,其他测风塔对应的区域属于风能丰富区.文章给出了酒泉地区有效风功率密度空间分布图,对进一步了解、应用甘肃酒泉区域的风能有较好的参考作用.     

河南省强对流天气诊断分析预报系统

强对流预报是天气预报的难点,为了提高预报强对流、特别是预报区域性强对流天气的预报能力,应用河南省1995—2004年的气象观测资料作分析样本,并计算多个大气动力和热力学参数。经过统计分析、诊断分析,选择预报能力强、指示性好的大气动力或热力学参数作为强对流天气的预报因子,采用加权集成建立预报方程。应用计算机技术自动实现从数据采集、物理参数计算、预报因子临界值判别、诊断预报方程运算,到以MICAPS图形方式输出预报结果,建立了河南省区域强对流天气预报系统。该系统为预报员提供了一种科学客观的参考依据,在近两年的业务运行中取得了比较理想的预报效果,提升了河南省强对流天气的预报能力。     

基于CMIP5模拟的中国区域陆气耦合强度评估及未来情景预估

基于第五次国际耦合模式比较计划(CMIP5)11个模式历史情景的模拟结果计算得到了中国区域夏季的陆气耦合强度并进行集合平均,结果表明,位于半干旱区的华北和内蒙古地区陆气耦合强度相对较强,西部干旱区的陆气耦合强度相对较弱,位于湿润区的中国东北地区东部、长江中下游和西南地区陆气耦合强度最弱。利用上述模式集合平均结果与由NCEP再分析资料和欧洲中心的中期气象预报40年再分析资料(ERA40)计算得到的陆气耦合强度相比较,结果显示这些模式的集合平均与再分析资料NCEP和ERA40的计算结果有较好的一致性。利用历史情景模拟和不同的典型排放路径(RCP),即低排放情景RCP2.6、中排放情景RCP4.5和高排放情景RCP8.5下的模拟结果预估陆气耦合强度未来变化。结果显示:与历史情景相比较,位于湿润区的中国南方地区蒸散发的主要控制因子是温度,在3种排放情景下随着温度上升引起蒸散发增加所导致陆气耦合强度升高;位于青藏高原以及半干旱区的内蒙古大部分地区蒸散发在未来的年际变化幅度减弱导致陆气耦合指数降低;位于西北干旱区陆气耦合强度在RCP2.6和RCP4.5情景上升,然而在RCP8.5情景下陆气耦合强度下降,其原因是在高排放情景下,水汽平流输送明显增强,局地蒸散发异常对空气湿度变化的贡献减弱,导致了陆气耦合强度降低。未来预估结果在中国南方可信度相对较高,从全国来看,在RCP4.5情景下可信度相对较高。     

剪切型多自由度体系瞬时输入能量的分布

通过对剪切型多自由度体系的地震能量反应分析,提出了描述多自由度体系整体脉冲能量反应的参数,瞬时输入能量等效平均速度,并在此基础上建立了瞬时输入能量分布系数的概念,提出了估计瞬时输入能量分布的方法。     

Signals from the epoch of cosmological recombination – Karl Schwarzschild Award Lecture 2008

The physical ingredients to describe the epoch of cosmological recombination are amazingly simple and well‐understood. This fact allows us to take into account a very large variety of physical processes, still finding potentially measurable consequences for the energy spectrum and temperature anisotropies of the Cosmic Microwave Background (CMB). In this contribution we provide a short historical overview in connection with the cosmological recombination epoch and its connection to the CMB. Also we highlight some of the detailed physics that were studied over the past few years in the context of the cosmological recombination of hydrogen and helium. The impact of these considerations is two‐fold: (i) The associated release of photons during this epoch leads to interesting and unique deviations of the CosmicMicrowave Background (CMB) energy spectrum from a perfect blackbody, which, in particular at decimeter wavelength and the Wien part of the CMB spectrum, may become observable in the near future. Despite the fact that the abundance of helium is rather small, it still contributes a sizeable amount of photons to the full recombination spectrum, leading to additional distinct spectral features. Observing the spectral distortions from the epochs of hydrogen and helium recombination, in principle would provide an additional way to determine some of the key parameters of the Universe (e.g. the specific entropy, the CMB monopole temperature and the pre‐stellar abundance of helium). Also it permits us to confront our detailed understanding of the recombination process with direct observational evidence. In this contribution we illustrate how the theoretical spectral template of the cosmological recombination spectrum may be utilized for this purpose. We also show that because hydrogen and helium recombine at very different epochs it is possible to address questions related to the thermal history of our Universe. In particular the cosmological recombination radiation may allow us to distinguish between Compton y ‐distortions that were created by energy release before or after the recombination of the Universe finished. (ii) With the advent of high precision CMB data, e.g. as will be available using the PLANCK Surveyor or CMBPOL, a very accurate theoretical understanding of the ionization history of the Universe becomes necessary for the interpretation of the CMB temperature and polarization anisotropies. Here we show that the uncertainty in the ionization history due to several processes, which until now were not taken in to account in the standard recombination code RECFAST, reaches the percent level. In particular He II → He I recombination occurs significantly faster because of the presence of a tiny fraction of neutral hydrogen at z ∼ 2400. Also recently it was demonstrated that in the case of H I Lyman α photons the timedependence of the emission process and the asymmetry between the emission and absorption profile cannot be ignored. However, it is indeed surprising how inert the cosmological recombination history is even at percent‐level accuracy. Observing the cosmological recombination spectrum should in principle allow us to directly check this conclusion, which until now is purely theoretical. Also it may allow to reconstruct the ionization history using observational data (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Intermediate‐term variations in solar radius during solar cycle 23

In this study, we look for the mid‐term variations in the daily average data of solar radius measurements made at the Solar Astrolabe Station of TUBITAK National Observatory (TUG) during solar cycle 23 for a time interval from 2000 February 26 to 2006 November 15. Due to the weather conditions and seasonal effect dependent on the latitude, the data series has the temporal gaps. For spectral analysis of the data series, thus, we use the Date Compensated Discrete Fourier Transform (DCDFT) and the CLEANest algorithm, which are powerful methods for irregularly spaced data. The CLEANest spectra of the solar radius data exhibit several significant mid‐term periodicities at 393.2, 338.9, 206.5, 195.2, 172.3 and 125.4 days which are consistent with periods detected in several solar time series by several authors during different solar cycles. The knowledge relating to the origin of solar radius variations is not yet present. To see whether these variations will repeat in next cycles and to understand how the amplitudes of such variations change with different phases of the solar cycles, we need more systematic efforts and the long‐term homogeneous data. Since most of the periodicities detected in the present study are frequently seen in solar activity indicators, it is thought that the physical mechanisms driving the periodicities of solar activity may also be effective in solar radius variations (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

New magnetic field measurements of β Cephei stars and slowly pulsating B stars

We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B‐type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B (hereafter SPB) stars, along with a small number of normal B‐type stars. A weak mean longitudinal magnetic field of the order of a few hundred Gauss was detected in three β Cephei stars and two stars suspected to be β Cephei stars, in five SPB stars and eight stars suspected to be SPB stars. Additionally, a longitudinal magnetic field at a level larger than 3σ has been diagnosed in two normal B‐type stars, the nitrogen‐rich early B‐type star HD 52089 and in the B5 IV star HD 153716. Roughly one third of β Cephei stars have detected magnetic fields: Out of 13 β Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected β Cephei stars two show a weak magnetic field. The fraction of magnetic SPBs and candidate SPBs is found to be higher: Roughly half of the 34 SPB stars have been found to be magnetic and among the 16 candidate SPBs eight stars possess magnetic fields. In an attempt to understand why only a fraction of pulsating stars exhibit magnetic fields, we studied the position of magnetic and non‐magnetic pulsating stars in the H‐R diagram. We find that their domains in the H‐R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence. It is possible that stronger fields tend to be found in stars with lower pulsating frequencies and smaller pulsating amplitudes. A somewhat similar trend is found if we consider a correlation between the field strength and the v sin i ‐values, i.e. stronger magnetic fields tend to be found in more slowly rotating stars (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)