The signature of hot hydrogen in the atmosphere of the extrasolar planet HD 209458b

About ten per cent of the known extrasolar planets are gas giants that orbit very close to their parent stars. The atmospheres of these 'hot Jupiters' are heated by the immense stellar irradiation. In the case of the planet HD 209458b, this energy deposition results in a hydrodynamic state in the upper atmosphere, allowing for sizeable expansion and escape of neutral hydrogen gas. HD 209458b was the first extrasolar planet discovered that transits in front of its parent star. The size of the planet can be measured using the total optical obscuration of the stellar disk during an observed transit, and the structure and composition of the planetary atmosphere can be studied using additional planetary absorption signatures in the stellar spectrum. Here we report the detection of absorption by hot hydrogen in the atmosphere of HD 209458b. Previously, the lower atmosphere and the full extended upper atmosphere of HD 209458b have been observed, whereas here we probe a layer where the escaping gas forms in the upper atmosphere of HD 209458b.     

Energetic neutral atoms as the explanation for the high-velocity hydrogen around HD 209458b

Absorption in the stellar Lyman-alpha (Lyalpha) line observed during the transit of the extrasolar planet HD 209458b in front of its host star reveals high-velocity atomic hydrogen at great distances from the planet. This has been interpreted as hydrogen atoms escaping from the planet's exosphere, possibly undergoing hydrodynamic blow-off, and being accelerated by stellar radiation pressure. Energetic neutral atoms around Solar System planets have been observed to form from charge exchange between solar wind protons and neutral hydrogen from the planetary exospheres, however, and this process also should occur around extrasolar planets. Here we show that the measured transit-associated Lyalpha absorption can be explained by the interaction between the exosphere of HD 209458b and the stellar wind, and that radiation pressure alone cannot explain the observations. As the stellar wind protons are the source of the observed energetic neutral atoms, this provides a way of probing stellar wind conditions, and our model suggests a slow and hot stellar wind near HD 209458b at the time of the observations.     

Infrared radiation from an extrasolar planet

A class of extrasolar giant planets--the so-called 'hot Jupiters' (ref. 1)--orbit within 0.05 au of their primary stars (1 au is the Sun-Earth distance). These planets should be hot and so emit detectable infrared radiation. The planet HD 209458b (refs 3, 4) is an ideal candidate for the detection and characterization of this infrared light because it is eclipsed by the star. This planet has an anomalously large radius (1.35 times that of Jupiter), which may be the result of ongoing tidal dissipation, but this explanation requires a non-zero orbital eccentricity (approximately 0.03; refs 6, 7), maintained by interaction with a hypothetical second planet. Here we report detection of infrared (24 microm) radiation from HD 209458b, by observing the decrement in flux during secondary eclipse, when the planet passes behind the star. The planet's 24-microm flux is 55 +/- 10 microJy (1sigma), with a brightness temperature of 1,130 +/- 150 K, confirming the predicted heating by stellar irradiation. The secondary eclipse occurs at the midpoint between transits of the planet in front of the star (to within +/- 7 min, 1sigma), which means that a dynamically significant orbital eccentricity is unlikely.     

A spectrum of an extrasolar planet

Of the over 200 known extrasolar planets, 14 exhibit transits in front of their parent stars as seen from Earth. Spectroscopic observations of the transiting planets can probe the physical conditions of their atmospheres. One such technique can be used to derive the planetary spectrum by subtracting the stellar spectrum measured during eclipse (planet hidden behind star) from the combined-light spectrum measured outside eclipse (star + planet). Although several attempts have been made from Earth-based observatories, no spectrum has yet been measured for any of the established extrasolar planets. Here we report a measurement of the infrared spectrum (7.5-13.2 microm) of the transiting extrasolar planet HD 209458b. Our observations reveal a hot thermal continuum for the planetary spectrum, with an approximately constant ratio to the stellar flux over this wavelength range. Superposed on this continuum is a broad emission peak centred near 9.65 microm that we attribute to emission by silicate clouds. We also find a narrow, unidentified emission feature at 7.78 microm. Models of these 'hot Jupiter' planets predict a flux peak near 10 microm, where thermal emission from the deep atmosphere emerges relatively unimpeded by water absorption, but models dominated by water fit the observed spectrum poorly.     

A stability limit for the atmospheres of giant extrasolar planets

Recent observations of the planet HD209458b indicate that it is surrounded by an expanded atmosphere of atomic hydrogen that is escaping hydrodynamically. Theoretically, it has been shown that such escape is possible at least inside an orbit of 0.1 au (refs 4 and 5), and also that H3+ ions play a crucial role in cooling the upper atmosphere. Jupiter's atmosphere is stable, so somewhere between 5 and 0.1 au there must be a crossover between stability and instability. Here we show that there is a sharp breakdown in atmospheric stability between 0.14 and 0.16 au for a Jupiter-like planet orbiting a solar-type star. These results are in contrast to earlier modelling that implied much higher thermospheric temperatures and more significant evaporation farther from the star. (We use a three-dimensional, time-dependent coupled thermosphere-ionosphere model and properly include cooling by H3+ ions, allowing us to model globally the redistribution of heat and changes in molecular composition.) Between 0.2 and 0.16 au cooling by H3+ ions balances heating by the star, but inside 0.16 au molecular hydrogen dissociates thermally, suppressing the formation of H3+ and effectively shutting down that mode of cooling.     

Water vapour in the atmosphere of a transiting extrasolar planet

Water is predicted to be among the most abundant (if not the most abundant) molecular species after hydrogen in the atmospheres of close-in extrasolar giant planets ('hot Jupiters'). Several attempts have been made to detect water on such planets, but have either failed to find compelling evidence for it or led to claims that should be taken with caution. Here we report an analysis of recent observations of the hot Jupiter HD 189733b (ref. 6) taken during the transit, when the planet passed in front of its parent star. We find that absorption by water vapour is the most likely cause of the wavelength-dependent variations in the effective radius of the planet at the infrared wavelengths 3.6 mum, 5.8 mum (both ref. 7) and 8 mum (ref. 8). The larger effective radius observed at visible wavelengths may arise from either stellar variability or the presence of clouds/hazes. We explain the report of a non-detection of water on HD 189733b (ref. 4) as being a consequence of the nearly isothermal vertical profile of the planet's atmosphere.     

L-抗坏血酸紫外分光光度法检测微量过氧化氢

建立了L-抗坏血酸（L—Aseorbieacid）紫外分光光度法测定微量过氧化氢的新方法．在pH=5．7的磷酸缓冲溶液介质中,选择273nm作为测定波长,过氧化氢的摩尔浓度在0～0．1mmol／L范围内服从比尔定律．回归方程为：y=0．0049＋4．44612x（mmol／L）,检出限为0．401μmol／L．该法用于溶液中、生物组织等样品中微量过氧化氢浓度的测定,快速简便．     

The interstellar N2 abundance towards HD 124314 from far-ultraviolet observations

The abundance of interstellar molecular nitrogen (N2) is of considerable importance: models of steady-state gas-phase interstellar chemistry, together with millimetre-wavelength observations of interstellar N2H+ in dense molecular clouds predict that N2 should be the most abundant nitrogen-bearing molecule in the interstellar medium. Previous attempts to detect N2 absorption in the far-ultraviolet or infrared (ice features) have hitherto been unsuccessful. Here we report the detection of interstellar N2 at far-ultraviolet wavelengths towards the moderately reddened star HD 124314 in the constellation of Centaurus. The N2 column density is larger than expected from models of diffuse clouds and significantly smaller than expected for dense molecular clouds. Moreover, the N2 abundance does not explain the observed variations in the abundance of atomic nitrogen (N I) towards high-column-density sightlines, implying that the models of nitrogen chemistry in the interstellar medium are incomplete.     

Towards a transgenic model of Huntington's disease in a non-human primate

Non-human primates are valuable for modelling human disorders and for developing therapeutic strategies; however, little work has been reported in establishing transgenic non-human primate models of human diseases. Huntington's disease (HD) is an autosomal dominant neurodegenerative disorder characterized by motor impairment, cognitive deterioration and psychiatric disturbances followed by death within 10-15 years of the onset of the symptoms. HD is caused by the expansion of cytosine-adenine-guanine (CAG, translated into glutamine) trinucleotide repeats in the first exon of the human huntingtin (HTT) gene. Mutant HTT with expanded polyglutamine (polyQ) is widely expressed in the brain and peripheral tissues, but causes selective neurodegeneration that is most prominent in the striatum and cortex of the brain. Although rodent models of HD have been developed, these models do not satisfactorily parallel the brain changes and behavioural features observed in HD patients. Because of the close physiological, neurological and genetic similarities between humans and higher primates, monkeys can serve as very useful models for understanding human physiology and diseases. Here we report our progress in developing a transgenic model of HD in a rhesus macaque that expresses polyglutamine-expanded HTT. Hallmark features of HD, including nuclear inclusions and neuropil aggregates, were observed in the brains of the HD transgenic monkeys. Additionally, the transgenic monkeys showed important clinical features of HD, including dystonia and chorea. A transgenic HD monkey model may open the way to understanding the underlying biology of HD better, and to the development of potential therapies. Moreover, our data suggest that it will be feasible to generate valuable non-human primate models of HD and possibly other human genetic diseases.     

Memory Chain in a Chaotic Autoassociative Neural Network

Memory chain is observed in a chaotic autoassociative neural network. The network recalls first stored pattern from a fragment of a memory, stays at this pattern for a while, transits to the second stored pattern that overlaps with the first recalled pattern.Then it stays at the second recalled pattern for a while, transits to the third stored pattern that overlaps with the second recalled pattern, and so on. Thus a memory chain is generated. The memory chain ends with the pattern that overlaps no other stored patten. This phenomenon is similar to the way of recalling process of human beings in some respects.     

A closely packed system of low-mass, low-density planets transiting Kepler-11

When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital shapes, and the fraction of transiting planets observed as multiples has implications for the planarity of planetary systems. But few stars have more than one known transiting planet, and none has more than three. Here we report Kepler spacecraft observations of a single Sun-like star, which we call Kepler-11, that reveal six transiting planets, five with orbital periods between 10 and 47?days and a sixth planet with a longer period. The five inner planets are among the smallest for which mass and size have both been measured, and these measurements imply substantial envelopes of light gases. The degree of coplanarity and proximity of the planetary orbits imply energy dissipation near the end of planet formation.     

四羧基钴酞菁催化氧化邻苯二胺测定过氧化氢

在pH值为9.0的Britton-Robinson缓冲溶液中,以四羧基钴酞菁作为过氧化物模拟酶催化过氧化氢与邻苯二胺的反应,建立一种测定微量过氧化氢的新方法。结果显示,反应的产物2,3-二氨基吩嗪在421nm处有一最大吸收峰,其吸光度值随过氧化氢加入量的增加而增加,吸光度差值与过氧化氢浓度在0～2.07×10-4mol/L范围内呈线性关系,检出限为1.36×10-5mol/L。该方法简单,适用于微量过氧化氢含量的测定。     

LaNi4.25Al0.75储氢合金的改性

为了提高LaNi4．25Al0．75合金的储氢性能,采用退火、表面镀铜和表面包覆SiO2对合金进行改性,并对处理前、后合金的微观结构和吸放氢性能的变化进行研究。研究结果表明,退火消除了LaNi4．25Al0．75合金中的偏析,减少了内应力,使合金具有平坦的吸氢平台;表面镀铜处理加快了合金的吸、放氢速度,但吸氢含量略有降低,另外,镀铜合金抗粉化性能加强,经10次吸、放氢循环后没有出现粉化现象;表面包覆SiO2前、后,合金的吸氢量变化不大,抗粉化性能加强,经10次吸、放氢循环后没有出现粉化现象。     

Hydrogen absorption-desorption cycle decay mechanism of palladium nanoparticle decorated nitrogen doped graphene

As a hydrogen storage material, palladium nanoparticle decorated nitrogen doped graphene (Pd/N-rGO) has drawn much attention owing to its high absorption capacity at moderate conditions. However, its hydrogen absorption-desorption cycle performance, which is essential for their practical application, has been rarely studied. In this paper, a simple and convenient high temperature thermal reduction method was used to synthesize nitrogen-doped graphene decorated with Pd nanoparticles (Pd/N-rGO). Taken it as a representative, the hydrogen absorption-desorption cycle performance of Pd/N-rGO was investigated. The results showed that after three cycles the hydrogen storage capacity dropped from 2.9 ​wt% to 0.8 ​wt% at 25 ​°C and 4 ​MPa pressure. It was found that the palladium nanoparticles shed from Pd/N-RGO sheet after cycle performance test, and then agglomerated. These phenomena will weaken the hydrogen spillover effect, leading to the decrease of hydrogen storage capacity. Meanwhile, decreased defects reduce the hydrogen absorption sites, which will thus deteriorate the hydrogen storage capacity.     

Observation and interpretation of a time-delayed mechanism in the hydrogen exchange reaction

Extensive theoretical and experimental studies have shown the hydrogen exchange reaction H+H2 --> H2+H to occur predominantly through a 'direct recoil' mechanism: the H--H bonds break and form concertedly while the system passes straight over a collinear transition state, with recoil from the collision causing the H2 product molecules to scatter backward. Theoretical predictions agree well with experimental observations of this scattering process. Indirect exchange mechanisms involving H3 intermediates have been suggested to occur as well, but these are difficult to test because bimolecular reactions cannot be studied by the femtosecond spectroscopies used to monitor unimolecular reactions. Moreover, full quantum simulations of the time evolution of bimolecular reactions have not been performed. For the isotopic variant of the hydrogen exchange reaction, H+D2 --> HD+D, forward scattering features observed in the product angular distribution have been attributed to possible scattering resonances associated with a quasibound collision complex. Here we extend these measurements to a wide range of collision energies and interpret the results using a full time-dependent quantum simulation of the reaction, thus showing that two different reaction mechanisms modulate the measured product angular distribution features. One of the mechanisms is direct and leads to backward scattering, the other is indirect and leads to forward scattering after a delay of about 25 femtoseconds.     

吸收性液滴的彩虹现象

提出了基于彩虹散射光吸收系数的液滴吸收率测量方法.采用基于Mie理论的改进算法进行数值模拟.研究表明,液滴的吸收性不改变彩虹光强波峰及对应频峰的位置,但改变彩虹光强强度,尤其对彩虹表面波结构及Airy结构影响较大,并因此降低了彩虹的可见度.计算发现液滴散射光吸收系数的最大值出现在彩虹区,并随液滴吸收率和粒径的增加稳定在彩虹最大波峰角位置,而且此处的吸收系数与吸收率之间有着线性关系.基于彩虹测量技术具有易检测、易标定的特点,因此有望发展为一种新的液滴吸收系数测量方法.     

Replication of the neurochemical characteristics of Huntington's disease by quinolinic acid

Huntington's disease (HD) is an autosomal dominant neurological disorder characterized by progressive chorea, cognitive impairment and emotional disturbance. The disease usually occurs in midlife and symptoms progress inexorably to mental and physical incapacitation. It has been postulated that an excitotoxin is involved in the pathogenesis of HD. Schwarcz and colleagues have shown that quinolinic acid (QA) can produce axon-sparing lesions similar to those observed in HD. The lesions result in a depletion of neurotransmitters contained within striatal spiny neurones, for example gamma-aminobutyric acid (GABA), while dopamine is unaffected. Recently, we and others have demonstrated that in HD striatum there is a paradoxical 3-5-fold increase in both somatostatin and neuropeptide Y which is attributable to selective preservation of a subclass of striatal aspiny neurones in which these peptides are co-localized. In the present study we demonstrate that lesions due to quinolinic acid closely resemble those of HD as they result in marked depletions of both GABA and substance P, with selective sparing of somatostatin/neuropeptide Y neurones. Lesions produced by kainic acid (KA), ibotenic acid (IA) and N-methyl-D-aspartate (MeAsp) were unlike those produced by QA, as they affected all cell types without sparing somatostatin/neuropeptide Y neurones. These results suggest that QA or a similar compound could be responsible for neuronal degeneration in HD.     

Demonstration by NMR of folding domains in lysozyme

Although there has been much speculation on the pathways of protein folding, only recently have experimental data on the topic been available. The study of proteins under conditions where species intermediate between the fully folded and unfolded states are stable has provided important information, for example about the disulphide intermediates in BPTI, cis/trans proline isomers of RNase A3 and the molten globule state of alpha-lactalbumin. An alternative approach to investigating folding pathways has involved detection and characterization of transient conformers in refolding studies using stopped-flow methods coupled with NMR measurements of hydrogen exchange. The formation of intermediate structures has been detected in the early stages of folding of cytochrome c, RNaseA and barnase. For alpha-lactalbumin, hydrogen exchange kinetics monitored by NMR proved to be crucial for identifying native-like structural features in the stable molten globule state. An analogous partially folded protein stable under equilibrium conditions has not been observed for the structurally homologous protein hen egg-white lysozyme, although there is evidence that a similar but transient state is formed during refolding. Here we describe NMR experiments based on competition between hydrogen exchange and the refolding process which not only support the existence of such a transient species for lysozyme, but enable its structural characteristics to be defined. The results indicate that the two structural domains of lysozyme are distinct folding domains, in that they differ significantly in the extent to which compact, probably native-like, structure is present in the early stages of folding.     

A highly polymorphic locus very tightly linked to the Huntington's disease gene

The genetic defect in Huntington's disease (HD), an inherited neuropsychiatric disorder of unknown etiology, has not been defined. The discovery of linkage between HD and the DNA marker D4S10(G8) raised the possibility of isolating the disease gene on the basis of its chromosomal location, in addition to providing a limited presymptomatic test for the late onset disorder. But it has been difficult to isolate other DNA markers nearer to the HD gene, and this has hampered attempts to identify the disease locus and limited the applicability and accuracy of predictive testing. Recently, several new DNA markers from the region of the genome near the HD gene have been isolated using a directed cloning strategy. We describe here the characterization of one of these new markers, D4S95, a highly polymorphic locus which displays no recombination with the HD gene in the families tested. The high degree of polymorphism at this locus and its proximity to the HD gene make it extremely useful for predictive testing and as a new starting point for attempts to clone the disease gene.     

氢钨青铜的微波辅助合成

氢钨青铜是一类光学和电学性能都非常优异的应用前景广阔的材料.快速简便的合成方法对其实际应用具有非常重要的意义.通过微波加热辅助合成了单相的立方相氢钨青铜H0.25WO3,其空间群和晶胞参数分别为Im-3和a=0.767 3(1) nm.样品的微观形貌为均匀的片状颗粒,厚度约50 nm,边长约100～200 nm.该纳米...