太阳活动变化对东亚冬季气候的非对称影响及可能机制

基于1959～2013年的观测和再分析资料以及10.7 cm(2800 MHz)太阳射电通量资料, 本文分析了太阳活动变化与东亚冬季气候的相关关系, 分析结果表明:太阳活动变化与东亚冬季大气环流有较好的相关性, 且在太阳活动的强、弱时期该相关关系存在很大差异, 在强太阳活动时期太阳活动变化与东亚冬季气候的联系更为显著, 而在弱太阳活动时期二者之间的直接联系微弱, 这表明太阳活动变化对东亚冬季气候的影响具有非对称性特征。在太阳活动较强的时期, 随着太阳活动的增强, 东亚中高纬对流层中层的大气环流倾向纬向型, 东亚大槽减弱, 850 hPa出现异常偏南风, 地面上西伯利亚高压以及冬季风减弱, 东亚大部分地区气温显著偏高;而在太阳活动较弱的时期, 太阳活动的年际差异与东亚冬季大气环流之间几乎不存在显著联系。分析太阳活动较强和较弱时期纬向平均纬向风的差异发现, 其间平流层行星波活动、热带西北太平洋海表温度的差异可能是造成这种非对称影响的重要原因。在强太阳活动时期, 平流层行星波在太阳活动的异常增强年有异常的从极地向赤道的水平传播, 高纬地区E-P通量(Eliassen-Palm flux)异常辐散, 导致中高纬西风及北极涛动(AO)增强, 同时热带西北太平洋海温异常偏冷, 海陆热力差异缩小, 大气环流经向度减弱, 东亚冬季风偏弱。     

洛阳地区太阳能资源分析与评估

根据1981—2010年郑州辐射站太阳辐射和日照资料、洛阳地区9个气象观测站日照资料,采用气候学计算、线性趋势分析等方法和资源丰富程度、利用价值、稳定程度等指标,对洛阳地区太阳能资源进行了计算、分析和评估。结果表明:洛阳地区多年平均总辐射为4842.4MJ·m-2·a-1,总体呈显著减少趋势,减少速率为每年1.4MJ·m-2。夏季辐射丰富,冬季偏少,夏季总辐射量是冬季的2倍;月平均总辐射5月最多(569.7MJ·m-2),12月最少(241.9MJ·m-2);年总辐射孟津最高,为4922.8MJ·m-2·a-1,宜阳最少,为4681.1MJ·m-2·a-1。多年平均日照时数为2064.7h,总体呈显著减少趋势。春季日照时数多,冬季少,春季日照时数比冬季多33.37%;月平均日照时数5月最多(217.3h),2月最少(138.2h);年日照时数孟津最多(2144.9h),宜阳最少(1909.2h)。洛阳各地属太阳能资源丰富区,利用价值较高,各月日照时数6h的天数为9.8~18.1天,全年为162.7~185.3天;太阳能资源也比较稳定,月最大日照时数12月6h的天数为16.9天,是月最小日照时数7月的1.48倍,12月至次年1月不利于太阳能利用。     

Interannual and Decadal Variations of Surface Solar Radiation over East China in the First Half of the 20th Century

Variability and long-term trends of sunshine duration(SSD) and total cloud cover(TCC) were studied based on surface observations from 10 meteorological stations over East China in the first half of the 20 th century. The correlation coefficients between SSD and diurnal temperature range(DTR), as well as TCC, were analyzed. SSD experienced a significant increasing trend(0.16 h d-1 per decade) from 1908 to 1936, and the maximum brightening was in autumn(0.33 h d-1 per decade). The good agreement between the variability of SSD and DTR, supported by the correlation coefficient between them of 0.72, implies that the SSD measurements were reliable. TCC showed a decreasing trend(-0.93% per decade) and was significantly inversely related to SSD(-0.74), indicating the variation of SSD was attributable to changes in cloud cover. The result was obviously different to that since the 1960 s, when clouds could not account for the decadal trend of surface solar radiation in China.     

1961~2010年黄河中下游地区24节气气候变化特征分析

24节气是我国古代劳动人民的独特创造。全面掌握"24节气"的气候变化规律,不但有利于指导农事生产,提高气象服务质量和水平,而且在为人类预防和治疗疾病方面也有重要意义。在全球变暖的气候背景下,统计分析了1961~2010年黄河中下游地区24节气的气温、湿度、风速等6个气象要素的变化特征,得到以下结论:黄河中下游地区随节气变换气候变化显著,大暑、小暑节气高温高湿,小寒、大寒节气寒冷干燥,清明节气寒温反复大风将至,霜降节气天气渐凉秋燥加剧等。50年内,春季型节气(平均、最高、最低)气温显著升高,冬季型节气最低气温升高显著。气压随节气变化特征与气温大致相反,夏、秋季节气有升压趋势。相对湿度与降水均呈减少趋势,以秋季型节气减小趋势最明显。春季风速最大,夏、秋季风速最小,所有节气风速均呈减小趋势,冬夏季节气日照时间呈缩短趋势。     

太阳辐照的观测研究进展

太阳总辐照是指在地球大气层顶接收到的太阳总辐射照度,也叫"太阳常数",但它实际上并非常数。太阳总辐照随波长的分布即为太阳分光辐照。太阳辐照变化的研究,对理解太阳表面及内部活动的物理过程、机制,研究地球大气、日地关系,解决人类面临的全球气候变暖的挑战等,都具有重要意义。首先简单介绍了太阳辐照,回顾了太阳辐照的空间观测;接着介绍了观测数据的并合,以及对合成数据的一些研究;然后讨论了太阳辐照变化的原因,简述了太阳总辐照的重构及其在气候研究上的一些应用,并进行必要的评论;最后对未来的研究方向提出了一些看法。     

明嘉靖六年《大统历》历书的气朔推步精度

历书是历法的民用本.考察了明嘉靖六年(1527年)<大统历>历书,根据历书所颁朔日和节气时刻,以及先期恢复的<授时历>和<大统历>推步术,并利用现代天文历算结果,可考校得出:(1)历书所载朔日和节气日期、时刻确由<大统历>推得;(2)<大统历>与<授时历>推步结果存在差异,推朔平均差33.35 min或34.93 min,推气平均差86.40 min,且两者均有差1日现象;(3)<大统历>与现代推算合朔时刻的平均误差为24.50 min或44.03 min,与现代推算节气时刻的差平均为1.25 d,若扣除太阳中心差则节气推步的误差将减少到86.40 min.     

Advanced Technology Solar Telescope: A status report

Magnetic fields control the inconstant Sun. The key to understanding solar variability and its direct impact on the Earth rests with understanding all aspects of these magnetic fields. The Advanced Technology Solar Telescope (ATST) has been design specifically for magnetic remote sensing. Its collecting area, spatial resolution, scattered light, polarization properties, and wavelength performance all insure ATST will be able to observe magnetic fields at all heights in the solar atmosphere from photosphere to corona. After several years of design efforts, ATST has been approved by the U.S. National Science Foundation to begin construction with a not to exceed cost cap of approximately $298M. Work packages for major telescope components will be released for bid over the next several months. An application for a building permit has been submitted (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Structure of radio sources at wavelengths 10.5 and 12.0 cm from observations of the Solar eclipse on March 29, 2006

The eclipse observations were performed at the Laboratory of Radio Astronomy of the CrAO in Katsiveli with stationary instrumentation of the Solar Patrol at wavelengths of 10.5 and 12.0 cm. The data obtained were used to determine the brightness temperature of the undisturbed Sun at solar activity minimum between 11-year cycles 23 and 24: T _d10.5 = (43.7 ± 0.5) × 10³ K at 10.5 cm and T _d12.0 = (51.8 ± 0.5) × 10³ K at 12.0 cm. The radio brightness distribution above the limb group of sunspots NOAA 0866 was calculated. It shows that at both wavelengths the source consisted of a compact bright nucleus about 50 × 10³ km in size with temperatures T _b10.5 = 0.94 × 10⁶ K and T _b12.0 = 2.15 × 10⁶ K located, respectively, at heights h _10.5 = 33.5 × 10³ km and h _12.0 = 43.3 × 10³ km above the sunspot and an extended halo with a temperature T _b = (230–300) × 10³ K stretching to a height of 157 × 10³ km above the photosphere. The revealed spatial structure of the local source is consistent with the universally accepted assumption that the radiation from the bright part of the source is generated by electrons in the sunspot magnetic fields at the second-third cyclotron frequency harmonics and that the halo is the bremsstrahlung of thermal electrons in the coronal condensation forming an active region. According to the eclipse results, the electron density near the upper boundary of the condensation was N _e ≈ 2.3 × 10⁸ cm^?3, while the optical depth was τ ≈ 0.1 at an electron temperature T _e ≈ 10⁶ K. Thus, the observations of the March 29, 2006 eclipse have allowed the height of the coronal condensation at solar activity minimum to be experimentally determined and the physical parameters of the plasma near its upper boundary to be estimated.     

Ion acceleration and Alfvén wave generation at the Earth’s bow shock

The processes of ion acceleration and Alfvén wave generation by accelerated particles at the Earth’s bow shock are studied within a quasi-linear approach. Steady-state ion and wave spectra are shown to be established in a time of 0.3–4 h, depending on the background level of Alfvénic turbulence in the solar wind. The Alfvén waves produced by accelerated ions are confined within the frequency range 10^?2–1 Hz and their spectral peak with a wave amplitude βB ～ B comparable to the interplanetary magnetic field strength B corresponds to the frequency v = (2–3) × 10^?2 Hz. The high-frequency part of the wave spectrum (v > 0.2 Hz) undergoes damping by thermal ions. The calculated spectra of the accelerated ions and the Alfvén waves generated by them reproduce the main features observed in experiments.     

Solar cycles during the Maunder minimum

We have obtained new consistent versions of the 400-yr time series of the Wolf sunspot number W, the sunspot group number G, and the total sunspot area S (or the total sunspot magnetic flux Φ). We show that the 11-yr cycle did not cease during the Maunder minimum of solar activity. The characteristics of the extrema of individual 11-yr cycles in 1600–2005 have been determined in terms of the total sunspot area index. We provide arguments for using alternating (“magnetic”) time series of indices in investigating the solar cyclicity.