气象防灾减灾科普栏目《风云纪录》的设计与实现

自然灾害公众教育可以提高全社会的灾害意识和忧患意识,增加公众的灾害知识,提高面对灾害的自救和互救能力,从而减少灾害的损失。为充分发挥电视在普及气象防灾减灾知识中的作用,依托已经发生或者新近发生的灾害事件,在纪实拍摄的基础上,充分利用数字媒体技术,设计了气象防灾减灾科普栏目《风云纪录》。节目采用故事化叙事手段,关注灾害事件中的受灾群体,将致灾的自然力量与社会人文因素交织在一起,把自然变化放在社会环境之中,气象专家、灾害专家和社会学者对灾害事件详细解读,使观众对灾害的认识更全面更深刻。对于抽象的知识、科学原理等,采用动画演示,以求通俗易懂。灾害纪实画面、灾害亲历者的现场采访、动画、解说、音乐、音效等表现形式经数字音视频编辑技术协调平衡,既真实生动,又具科普价值。自2003年以来,在栏目设计指导下,已经拍摄制作了200余期节目,通过各种播放,发挥了良好的科普效益,也为进一步做好气象灾害专题教育积累了经验。     

庐山2008和2009年两次冰冻天气对比分析

利用高空与地面观测资料,主要从形势场、温度层结、地理形势及地面气象要素等方面,对庐山2008年和2009年两次冰冻天气过程进行对比分析。结果表明,庐山2009年冰冻灾害与2008年初中国南方出现的大范围冰冻灾害有些不同特点,2009年冰冻灾害更具有明显的庐山局部性特征。认为庐山冰冻灾害的出现主要决定于925—850hPa层次的温度层结,当层结温度降为0℃以下并伴有较明显降水时,并不一定需要太长时间和明显逆温层的存在庐山就可以出现冰冻灾害。     

广东2008年低温雨雪冰冻灾害及气象应急响应

2008年初我国南方遭受了百年一遇低温雨雪冰冻灾害,广东的受灾程度属80年一遇,造成了重大经济损失和严重社会影响.分析发现:灾害过程在近年来最严重的一次"拉尼娜"事件背景下发生的,与欧亚地区持续大气环流异常密切相关.在"北脊南槽"和西太平洋副高偏北偏强的形势下,冷暖气流在我国南方地区频繁交汇,使对流层中低层形成逆温层和局地经向环流产生异常,造成了此次持续低温雨雪冰冻过程.面对灾害引发的公共事件,广东省气象部门打破常规、准确预警,启动预案,通过媒体和"公共事件预警信息发布平台",及时传播权威的公共预警信息,为安定民心、稳定社会、减少灾害起到积极作用.灾后反思发现,山区冰灾的监测、灾害的评估、公共信息发布等的能力和规范均亟待加强.     

濮阳高新区洪灾城市经济损失评估

根据1995--2004年濮阳高新区气象和洪灾实况资料,分析了洪灾时空分布及城市经济损失特征.采用分等级、分资源类型的参数统计、回归分析和加权平均等方法,探讨了洪灾损失的评估步骤和技术方法,建立了城市洪灾损失的定量评估系统模型.选用2005--2006年濮阳高新区典型的洪灾事例验证该方法、模型的可行性,结果表明,洪灾损失评估定量计算结果与社会经济损失调查统计数据比较接近.结论认为:洪灾损失评估模型能够快速、准确地对洪灾损失作出定量评估,技术方法是可行、可操作的,为政府指挥防洪抗灾提供理论分析有一定的使用价值.     

2008年初贵州低温雨雪凝冻灾害天气成因分析

利用NECP 2.5°×2.5°的日平均再分析资料和常规观测资料,对2008年1月12日-2月13日期间贵州省历史罕见的持续低温雨雪凝冻天气过程的环流特征及物理量进行了分析,并对中东部凝冻严重的前期和西部凝冻严重的后期做了对比.揭示了此次灾害天气的几个主要天气特征:(1)地面静止锋的位置关系着我省低温雨雪凝冻灾害的区域.(2)500 hPa环流前期和后期影响系统明显不同.过程期间欧亚大陆500 hPa高度场距平呈"北高南低"分布,亚洲区极涡南掉,面积偏大.(3)过程前期850 hPa冷舌明显,等温线密集;后期700 hPa 温降低,有冷舌活动,850 hPa冷舌明显减弱,低温维持.中东部和西部地区冷暖平流垂直方向上的配制不同.强盛的700 hPa暖湿气流是此次过程的主要水汽来源.     

Planetary transit observations at the University Observatory Jena: XO‐1b and TrES‐1

We report on observations of transit events of the transiting planets XO‐1b and TrES‐1 with a 25 cm telescope of the University Observatory Jena. With the transit timings for XO‐1b from all 50 available XO, SuperWASP, Transit Light Curve (TLC)‐Project‐ and Exoplanet Transit Database (ETD)‐data, including our own I ‐band photometry obtained in March 2007, we find that the orbital period is P = (3.941501 ± 0.000001) d, a slight change by ∼3 s compared to the previously published period. We present new ephemeris for this transiting planet. Furthermore, we present new R ‐band photometry of two transits of TrES‐1. With the help of all available transit times from literature this allows us to refine the estimate of the orbital period: P = (3.0300722 ± 0.0000002) d. Our observations will be useful for future investigations of timing variations caused by additional perturbing planets and/or stellar spots and/or moons (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Repeating microlensing events in the OGLE data

Microlensing events are usually selected among single-peaked non-repeating light curves in order to avoid confusion with variable stars. However, a microlensing event may exhibit a second microlensing brightening episode when the source or/and the lens is a binary system. A careful analysis of these repeating events provides an independent way to study the statistics of wide binary stars and to detect extrasolar planets. Previous theoretical studies predicted that 0.5–2 per cent of events should repeat due to wide binary lenses. We present a systematic search for such events in about 4000 light curves of microlensing candidates detected by the Optical Gravitational Lensing Experiment (OGLE) towards the Galactic bulge from 1992 to 2007. The search reveals a total of 19 repeating candidates, with six clearly due to a wide binary lens. As a by-product, we find that 64 events (∼2 per cent of the total OGLE-III sample) have been misclassified as microlensing; these misclassified events are mostly nova or other types of eruptive stars. The number and importance of repeating events will increase considerably when the next-generation wide-field microlensing experiments become fully operational in the future.     

On corotation torques, horseshoe drag and the possibility of sustained stalled or outward protoplanetary migration

We study the torque on low-mass protoplanets on fixed circular orbits, embedded in a protoplanetary disc in the isothermal limit. We consider a wide range of surface density distributions including cases where the surface density increases smoothly outwards. We perform both linear disc response calculations and non-linear numerical simulations. We consider a large range of viscosities, including the inviscid limit, as well as a range of protoplanet mass ratios, with special emphasis on the co-orbital region and the corotation torque acting between disc and protoplanet.
For low-mass protoplanets and large viscosity, the corotation torque behaves as expected from linear theory. However, when the viscosity becomes small enough to enable horseshoe turns to occur, the linear corotation torque exists only temporarily after insertion of a planet into the disc, being replaced by the horseshoe drag first discussed by Ward. This happens after a time that is equal to the horseshoe libration period reduced by a factor amounting to about twice the disc aspect ratio. This torque scales with the radial gradient of specific vorticity, as does the linear torque, but we find it to be many times larger. If the viscosity is large enough for viscous diffusion across the co-orbital region to occur within a libration period, we find that the horseshoe drag may be sustained. If not, the corotation torque saturates leaving only the linear Lindblad torques. As the magnitude of the non-linear co-orbital torque (horseshoe drag) is always found to be larger than the linear torque, we find that the sign of the total torque may change even for mildly positive surface density gradients. In combination with a kinematic viscosity large enough to keep the torque from saturating, strong sustained deviations from linear theory and outward or stalled migration may occur in such cases.