尘埃等离子体的引力非稳定性与凝聚效应

从尘埃等离子体的基本方程出发，采用非平衡态动力学方法，研究了尘埃粒子的引力（重力）对尘埃等离子体宏观动力学的影响，具体分析了产生凝聚效应的条件及其相关性质。结果表明，尘埃等离子体中存在一种由引力非稳定性产生的凝聚效应，从而导致局域密度增大。这种效应可能与星际介质分子云及原始恒星的形成有关，也同样会影响在实验室中等离子体加工的质量。     

暗分子云核L183的射电观测和尘气相互作用

利用青海德令哈观测站13.7m射电望远镜对暗分子云核L183作成图观测,选用的谱线为C18O(J=1-0).与Swade利用NH3(1,1)谱线所作的等积分强度图比较,发现NH3图中的2个极值位置位于C18O密度分布的低密度谷区.由于NH3的辐射与尘埃的红外辐射分布相关,所以C18O分子密度的减少是因为尘埃吸附.因此利用CO分子无法观测到恒星形成早期处于坍缩边缘的暗分子云核.     

早型旋涡星系M81(NGC 3031)光谱能量分布的空间解析研究

文章利用光谱能量分布(Spectral Energy Distribution, SED)拟合对近邻早型旋涡星系M81(NGC 3031)的整体和局部区域进行从远紫外到远红外光谱的建模,旨在探究M81星系中的星族和尘埃性质以及它们的空间分布。研究中,收集了来自包括GALEX、Swift、SDSS、2MASS、WISE、Spitzer和Herschel的空间及地面望远镜/巡天获得的一共27个波段的图像数据,并且将所有数据统一成相同的分辨率。通过对M81整体和每个像素进行SED拟合,得到了M81中的星族和尘埃等物理参数及其空间分布。发现M81是一个整体年龄约为9.5 Gyr(十亿年),恒星总质量约为3.54×10¹¹ M_☉(太阳质量),整体恒星形成率约为0.29 M_⊙/yr,光度约4.26×10¹¹ L_⊙(太阳光度),以年老恒星为主的星系。M81的内部区域(主要由核球主导),包含了星系中最年老星族,其年龄大约为10 Gyr,恒星形成率低,尘埃消光小;外部区域(盘主导)年龄约为1 G...     

两个乌桕新品种苗木光合特性比较

【目的】探讨两个乌桕新品种‘海滨绯红’、‘海滨紫晶’夏季光合特性并进行比较,为乌桕新品种的栽培与推广应用提供理论依据。【方法】盆栽条件下测定2年生嫁接苗叶片光合色素含量、光合日变化、光响应曲线以及CO₂响应曲线,并进行灰色关联分析。【结果】① ‘海滨紫晶’的叶绿素a(Chla)、叶绿素b(Chlb)、类胡萝卜素(Car)含量以及叶绿素a/b(Chla/b)均高于‘海滨绯红’,其中叶绿素a、叶绿素b和类胡萝卜素含量存在显著性差异;② 两个品种8月光合日变化曲线皆为典型的单峰型,无“午休”现象,‘海滨紫晶’净光合速率(P_n)、气孔导度(G_s)和蒸腾速率(T_r)的日均值和峰值均显著高于‘海滨绯红’,而胞间CO₂浓度(C_i)则相反;灰色关联分析表明,影响两个品种P_n的主要环境因子是大气温度(T_a)和光合有效辐射(PAR)。与‘海滨绯红’相比,‘海滨紫晶’的P_n与T_a的关联度更大,而与大气CO₂浓度(C_a)关联度较小;③ ‘海滨紫晶’的最大净光合速率(P_n,max)、光饱和点(LSP)、暗呼吸速率(R_d)和光补偿点(LCP)均高于‘海滨绯红’,表观量子效率(AQY)低于‘绯红’,其中P_n,max、LSP和R_d存在显著性差异;④ ‘海滨紫晶’的最大光合能力(A_n,max)、CO₂饱和点(CSP)、羧化效率(CE)和光呼吸速率(R_p)大于‘海滨绯红’,CO₂补偿点(CCP)小于‘海滨绯红’,其中A_n,max、CSP存在显著性差异。【结论】两个乌桕新品种在光合特性上均表现出较强的夏季生长适应性。与‘海滨绯红’相比,‘海滨紫晶’光合性能较优,对高温及强光的适应性更强。其较强的光合能力与其在高温强光下所受的非气孔限制相对较小有关,较高的羧化效率和1,5-二磷酸核酮糖(RUBP)再生能力可能是‘海滨紫晶’改善非气孔限制的主要原因,光呼吸可能是其在高温强光下避免光抑制和光破坏的一种机制。     

美科学家发现天然激光

美科学家发现天然激光美国科学家借助机载天文台上安装的红外线望远镜，对准天鹅星座内一颗诞生时间不久、温度极高、十分明亮的恒星，首次发现了存在于太空环境中的天然激光光源。天然激光的发现为科学家研究尚属年轻的恒星周围的气体和尘埃云盘状况提供了强有力的工具。...     

沟眶象发育起点温度和有效积温测定

为进一步了解沟眶象生物生态学特性,在室内自然变温条件下,对其发育起点温度和有效积温进行测定,并得出相应各虫态的历期预测式。结果表明:沟眶象卵(egg)、幼虫(larval)、蛹(pupae)发育起点温度分别为8.84、15.37、5.95 ℃,各发育期有效积温分别为190.50、667.06、322.50 ℃·d。沟眶象各虫态历期预测式分别为:N_egg=(190.50±27.81)/T-(8.84±0.66),N_larval=(667.06±92.29)/T-(15.37±1.4),N_pupae=(322.50±32.37)/T-(5.95±1.63)。经林间验证,各预测式在沟眶象卵期、蛹期较为可行,幼虫期虽有一定偏差,但可以为预测预报提供指导。     

基于核磁共振技术的硫酸盐侵蚀下混凝土孔隙率发展规律分析

针对不同浓度硫酸盐侵蚀下混凝土损伤过程中孔结构退化规律问题,对混凝土进行不同质量分数硫酸盐的冻融循环试验。采用核磁共振技术对混凝土损伤过程中的孔结构变化以及试验过程中的质量和相对动弹性模量变化进行分析。结果表明:不同质量分数硫酸盐侵蚀下T₂谱中第一峰变化明显,且同时期随着硫酸盐质量分数的增加,T₂谱第一峰变化幅度增大;盐冻环境下T₂谱第一峰面积与冻融循环次数之间符合指数关系,水冻环境下T₂谱第一峰面积与冻融循环次数之间符合线性关系;微小孔隙率发展与冻融循环次数之间符合线性关系;孔隙率与冻融循环次数、硫酸盐质量分数之间符合显著的线性关系;混凝土的质量和相对动弹性模量损失随着硫酸盐质量分数的增加而增加。     

联苯型聚芳醚砜醚酮酮共聚物的合成与表征

以无水AlCl₃/二氯乙烷(DCE)/N,N-二甲基甲酰胺(DMF)为复合溶剂体系,在低温条件下,以4,4’-二苯氧基二苯砜(DPODPS)、对苯二甲酰氯(TPC)、4,4’-联苯二甲酰氯(BPPC)为原料通过亲电共缩聚反应制得一系列聚芳醚砜醚酮酮(PESEKKs),用FT-IR、DSC、TG、WAXD等技术对聚合物做了表征.结果表明:随着BPPC含量的增加,共聚物的T_g从194 ℃上升到210 ℃,T_m从223 ℃增加到238 ℃,热分解温度均大于550 ℃,聚合物的耐热性能得到显著提升.经过检测,共聚物的溶解性能良好.     

银河系发现5000个宇宙气泡

据物珲学家组织网站报道，一组志愿者日前借助美国宇航局进行斯皮策空间望远镜数据的榆杏，在我们的银河系银蕊结构中发现了超过5000个“气泡”结构。这是年轻高温的恒星“吹出”的尘埃和气体气泡结构，这些气泡说明这些位置正有新生的恒星诞生。     

大花序桉群体适应性相关的SSR位点

【目的】检测大花序桉群体与环境适应性相关的基因组位点,为种质资源保护和利用提供分子生物学信息。【方法】利用84个SSR标记(包括29个基因组SSR 和55个EST-SSR)分析引种到广西,来源于澳大利亚昆土兰州北部和南部各7个大花序桉群体,通过Mantel 检验确定群体间是否存在地理隔离;检测群体间分化系数(F_st)离群值的受选择位点;并基于空间分析法检测与群体气候因子显著相关的等位片段,将显著相关位点的序列与NCBI数据库比对进行功能注释。【结果】大花序桉北部与南部群体间存在地理隔离,基于19个气候因子的聚类分析将北方与南方群体分为独立的组,这表明气候因子亦驱动了群体的分化。共检测到F_st离群值的受选择SSR位点39个(46.4%),其中,LOSITAN软件检测到12个正向选择位点和17个平衡选择位点。5个F_st离群值位点的6个等位片段与1个或多个气候因子显著相关(P<0.001),其等位频率在北部与南部群体间差异明显,其中,Embra6-118 bp与最冷月最低气温(T_mcm)显著相关,位点DNA序列的功能注释为碱性螺旋-环-螺旋(basic helix-loop-helix, bHLH)转录因子bHLH155;Embra20-121 bp与最暖季度降水量(P_wq)显著相关,位点的功能注释为蔗糖转运蛋白(sucrose transporters);EUCeSSR676-168 bp与T_mcm、P_wq、年均气温(T_ma)和最暖月最高气温(T_mwm)均显著相关,位点的功能注释为光系统Ⅱ稳定性/组装因子HCF136 (photosystem II stability/assembly factor HCF136);另外两个显著相关位点EUCeSSR298和EUCeSSR1009的功能未知。【结论】大花序桉北部与南部群体的显著分化受长期气候的影响,在第四纪大冰期可能存在北部和南部避难所。与气候因子显著相关的SSR位点在北部和南部群体间的等位频率差异为基于正向选择的气候适应性提供了分子证据。     

Detection of water masers in a sample of 84 IRAS sources

Using a newly installed system on the 25 m telescope of Urumqi Observatory, we searched for H20 maser emission towards 84 IRAS sources including young stellar objects （YSOs） and candidates for OFUIR stars. Water masers were detected in four star formation regions and one envelope of late type of stars for the first time. New water maser components were measured in two sources. In a maser source with no water maser emission detected six years ago, strong maser emission was found at different velocities, showing that there was a new explosion of water maser in this source.     

星际C60

C60的发现起源于人们对星际尘埃的探索,肇始于1985年由Kroto等人首次在实验室合成,25年后最终于2010年在星际空间被探测到．近几年天文工作者在多种星周、星际环境观测到C60．本文综述了与天文观测和理论密切相关的C60的有关物理性质;介绍了C60在星际空间中的观测特性;最后讨论了C60在星际空间的形成与激发机制．     

外向流喷流驱动的模型研究进展

按喷流与周围介质的相互作用过程把外向流的喷流驱动模型分为2大类,对其中几个作了较为细致的分析和比较,最后提出了今后模型发展的方向。     

Extreme collisions between planetesimals as the origin of warm dust around a Sun-like star

The slow but persistent collisions between asteroids in our Solar System generate a tenuous cloud of dust known as the zodiacal light (because of the light the dust reflects). In the young Solar System, such collisions were more common and the dust production rate should have been many times larger. Yet copious dust in the zodiacal region around stars much younger than the Sun has rarely been found. Dust is known to orbit around several hundred main-sequence stars, but this dust is cold and comes from a Kuiper-belt analogous region out beyond the orbit of Neptune. Despite many searches, only a few main-sequence stars reveal warm (> 120 K) dust analogous to zodiacal dust near the Earth. Signs of planet formation (in the form of collisions between bodies) in the regions of stars corresponding to the orbits of the terrestrial planets in our Solar System have therefore been elusive. Here we report an exceptionally large amount of warm, small, silicate dust particles around the solar-type star BD+20,307 (HIP 8920, SAO 75016). The composition and quantity of dust could be explained by recent frequent or huge collisions between asteroids or other 'planetesimals' whose orbits are being perturbed by a nearby planet.     

晚期演化星辐射流量的简化计算模型

本文提出了计算AGB末期到PPN阶段恒星辐射流量的简化模型,并由此得出了包括散射在内的光谱流量的解析表达式。该模型可较为方便地分析晚型星光谱流量的现测数据并得到有关晚型星的物理结构和状态的一些特点和参数。作为本模型的一个例子,我们得出了源OH/IR 17.7-2.0具有双壳层结构的特点,其中一个尘埃壳层的温度约为800K(内壳层),另一个壳层的温度约为110K(外壳层)。     

Water vapour and hydrogen in the terrestrial-planet-forming region of a protoplanetary disk

Planetary systems (ours included) formed in disks of dust and gas around young stars. Disks are an integral part of the star and planet formation process, and knowledge of the distribution and temperature of inner-disk material is crucial for understanding terrestrial planet formation, giant planet migration, and accretion onto the central star. Although the inner regions of protoplanetary disks in nearby star-forming regions subtend only a few nano-radians, near-infrared interferometry has recently enabled the spatial resolution of these terrestrial zones. Most observations have probed only dust, which typically dominates the near-infrared emission. Here I report spectrally dispersed near-infrared interferometric observations that probe the gas (which dominates the mass and dynamics of the inner disk), in addition to the dust, within one astronomical unit (1 au, the Sun-Earth distance) of the young star MWC 480. I resolve gas, including water vapour and atomic hydrogen, interior to the edge of the dust disk; this contrasts with results of previous spectrally dispersed interferometry observations. Interactions of this accreting gas with migrating planets may lead to short-period exoplanets like those detected around main-sequence stars. The observed water vapour is probably produced by the sublimation of migrating icy bodies, and provides a potential reservoir of water for terrestrial planets.     

Low-temperature crystallization of silicate dust in circumstellar disks.

Silicate dust in the interstellar medium is observed to be amorphous, yet silicate dust in comets and interplanetary dust particles is sometimes partially crystalline. The dust in disks that are thought to be forming planets around some young stars also appears to be partially crystalline. These observations suggest that as the dust goes from the precursor clouds to a planetary system, it must undergo some processing, but the nature and extent of this processing remain unknown. Here we report observations of highly crystalline silicate dust in the disks surrounding binary red-giant stars. The dust was created in amorphous form in the outer atmospheres of the red giants, and therefore must be processed in the disks to become crystalline. The temperatures in these disks are too low for the grains to anneal; therefore, some low-temperature process must be responsible. As the physical properties of the disks around young stars and red giants are similar, our results suggest that low-temperature crystallization of silicate grains also can occur in protoplanetary systems.     

Reflected light from sand grains in the terrestrial zone of a protoplanetary disk

In the standard model of terrestrial planet formation, the first step in the process is for interstellar dust to coagulate within a protoplanetary disk surrounding a young star, forming large grains that settle towards the disk plane. Interstellar grains of typical size approximately 0.1 microm are expected to grow to millimetre- (sand), centimetre- (pebble) or even metre-sized (boulder) objects rather quickly. Unfortunately, such evolved disks are hard to observe because the ratio of surface area to volume of their constituents is small. We readily detect dust around young objects known as 'classical' T Tauri stars, but there is little or no evidence of it in the slightly more evolved 'weak-line' systems. Here we report observations of a 3-Myr-old star, which show that grains have grown to about millimetre size or larger in the terrestrial zone (within approximately 3 au) of this star. The fortuitous geometry of the KH 15D binary star system allows us to infer that, when both stars are occulted by the surrounding disk, it appears as a nearly edge-on ring illuminated by one of the central binary components. This work complements the study of terrestrial zones of younger disks that have been recently resolved by interferometry.     

A young massive planet in a star-disk system

There is a general consensus that planets form within disks of dust and gas around newly born stars. Details of their formation process, however, are still a matter of ongoing debate. The timescale of planet formation remains unclear, so the detection of planets around young stars with protoplanetary disks is potentially of great interest. Hitherto, no such planet has been found. Here we report the detection of a planet of mass (9.8+/-3.3)M(Jupiter) around TW Hydrae (TW Hya), a nearby young star with an age of only 8-10 Myr that is surrounded by a well-studied circumstellar disk. It orbits the star with a period of 3.56 days at 0.04 au, inside the inner rim of the disk. This demonstrates that planets can form within 10 Myr, before the disk has been dissipated by stellar winds and radiation.     

Substantial reservoirs of molecular hydrogen in the debris disks around young stars

Circumstellar accretion disks transfer matter from molecular clouds to young stars and to the sites of planet formation. The disks observed around pre-main-sequence stars have properties consistent with those expected for the pre-solar nebula from which our own Solar System formed 4.5 Gyr ago. But the 'debris' disks that encircle more than 15% of nearby main-sequence stars appear to have very small amounts of gas, based on observations of the tracer molecule carbon monoxide: these observations have yielded gas/dust ratios much less than 0.1, whereas the interstellar value is about 100 (ref. 9). Here we report observations of the lowest rotational transitions of molecular hydrogen (H2) that reveal large quantities of gas in the debris disks around the stars beta Pictoris, 49 Ceti and HD135344. The gas masses calculated from the data are several hundreds to a thousand times greater than those estimated from the CO observations, and yield gas/dust ratios of the same order as the interstellar value.