纳米复合质子传导膜中温硫化氢固体氧化物燃料电池的研究

应用溶胶-凝胶法制备了中温硫化氢固体氧化物燃料电池的纳米复合质子传导膜。用SEM和EDX对纳米复合膜进行了观察和表征，并与传统工艺制备的电解膜（微米级）的性能进行了比较。探讨了微米级和纳米级的复合Li2SO4＋A12O3膜的离子传导性随温度变化规律。与传统的工艺采用相同组分制备的微米级电解膜相比，纳米复合膜的微观结构、致密性、机械强度和离子传导性均得到改善，而最显著改善是膜的离子传导性能。纳米复合Li2SO4＋Al2O3膜的中温硫化氢固体氧化物燃料电池的性能较稳定，察觉不到膜两侧的气体穿过膜扩散到另一侧。在750℃和101．13kPa下，电池的最大输出功率密度为135mW·cm^-2，最大电流密度为480mA·cm^-2。     

纳米复合质子传导膜中温硫化氢固体氧化物燃料电池的研究

应用溶胶-凝胶法制备了中温硫化氢固体氧化物燃料电池的纳米复合质子传导膜。用SEM和EDX对纳米复合膜进行了观察和表征,并与传统工艺制备的电解膜(微米级)的性能进行了比较。探讨了微米级和纳米级的复合Li2SO4 Al2O3膜的离子传导性随温度变化规律。与传统的工艺采用相同组分制备的微米级电解膜相比,纳米复合膜的微观结构、致密性、机械强度和离子传导性均得到改善,而最显著改善是膜的离子传导性能。纳米复合Li2SO4 Al2O3膜的中温硫化氢固体氧化物燃料电池的性能较稳定,察觉不到膜两侧的气体穿过膜扩散到另一侧。在750℃和101.13kPa下,电池的最大输出功率密度为135mW.cm-2,最大电流密度为480mA.cm-2。     

A turbulent wake as a tracer of 30,000 years of Mira's mass loss history

Mira is one of the first variable stars ever discovered and it is the prototype (and also the nearest example) of a class of low-to-intermediate-mass stars in the late stages of stellar evolution. These stars are relatively common and they return a large fraction of their original mass to the interstellar medium (ISM) (ref. 2) through a processed, dusty, molecular wind. Thus stars in Mira's stage of evolution have a direct impact on subsequent star and planet formation in their host galaxy. Previously, the only direct observation of the interaction between Mira-type stellar winds and the ISM was in the infrared. Here we report the discovery of an ultraviolet-emitting bow shock and turbulent wake extending over 2 degrees on the sky, arising from Mira's large space velocity and the interaction between its wind and the ISM. The wake is visible only in the far ultraviolet and is consistent with an unusual emission mechanism whereby molecular hydrogen is excited by turbulent mixing of cool molecular gas and shock-heated gas. This wind wake is a tracer of the past 30,000 years of Mira's mass-loss history and provides an excellent laboratory for studying turbulent stellar wind-ISM interactions.     

Biological scaling: does the exception prove the rule?

Reich et al. report that the whole-plant respiration rate, R, in seedlings scales linearly with plant mass, M, so that R=C(R)M(theta) when theta approximately 1, in which c(R) is the scaling normalization and theta is the scaling exponent. They also state that because nitrogen concentration (N) is correlated with c(R), variation in N is a better predictor of R than M would be. Reich et al. and Hedin incorrectly claim that these "universal" findings question the central tenet of metabolic scaling theory, which they interpret as predicting theta = (3/4), irrespective of the size of the plant. Here we show that these conclusions misrepresent metabolic scaling theory and that their results are actually consistent with this theory.     

Common genetic variants at the CRAC1 (HMPS) locus on chromosome 15q13.3 influence colorectal cancer risk

We mapped a high-penetrance gene (CRAC1; also known as HMPS) associated with colorectal cancer (CRC) in the Ashkenazi population to a 0.6-Mb region on chromosome 15 containing SCG5 (also known as SGNE1), GREM1 and FMN1. We hypothesized that the CRAC1 locus harbored low-penetrance variants that increased CRC risk in the general population. In a large series of colorectal cancer cases and controls, SNPs near GREM1 and SCG5 were strongly associated with increased CRC risk (for rs4779584, P = 4.44 x 10(-14)).     

中温质子传导膜H2S燃料电池电极催化剂

研究了基于三相边界层理论设计的中温质子传导膜H2S燃料电池的阳极与阴极催化剂.考察了3种阳极催化剂Pt、MoS2及复合金属硫化物(MoS2/N iS)电化学氧化硫化氢的性能和在硫化氢环境下的化学稳定性,发现MoS2和复合MoS2/N iS催化剂比Pt具有更好的催化活性,但MoS2在温度超过450℃时会升华,而含有Mo和过渡金属N i的复合MoS2/N iS催化剂在操作条件下很稳定.文中还研究了两种阴极催化剂Pt与复合N iO催化剂的电化学性能,发现复合N iO催化剂比Pt电极具有更低的过电位和更好的电化学性能;虽然复合电极的导电性比Pt差些,但是这一问题可以通过在电极中掺杂10%的Ag粉解决.由H2S、(MoS2 N iS Ag 电解质 淀粉)/Li2SO4-A l2O3/(N iO Ag 电解质 淀粉)、空气构成的燃料电池在101.13 kPa和600~680℃下的电化学特性研究表明,电池最大输出电流密度和功率密度在680℃时分别达到240mA/cm2和70mW/cm2.     

Optogenetic stimulation of a hippocampal engram activates fear memory recall

A specific memory is thought to be encoded by a sparse population of neurons. These neurons can be tagged during learning for subsequent identification and manipulation. Moreover, their ablation or inactivation results in reduced memory expression, suggesting their necessity in mnemonic processes. However, the question of sufficiency remains: it is unclear whether it is possible to elicit the behavioural output of a specific memory by directly activating a population of neurons that was active during learning. Here we show in mice that optogenetic reactivation of hippocampal neurons activated during fear conditioning is sufficient to induce freezing behaviour. We labelled a population of hippocampal dentate gyrus neurons activated during fear learning with channelrhodopsin-2 (ChR2) and later optically reactivated these neurons in a different context. The mice showed increased freezing only upon light stimulation, indicating light-induced fear memory recall. This freezing was not detected in non-fear-conditioned mice expressing ChR2 in a similar proportion of cells, nor in fear-conditioned mice with cells labelled by enhanced yellow fluorescent protein instead of ChR2. Finally, activation of cells labelled in a context not associated with fear did not evoke freezing in mice that were previously fear conditioned in a different context, suggesting that light-induced fear memory recall is context specific. Together, our findings indicate that activating a sparse but specific ensemble of hippocampal neurons that contribute to a memory engram is sufficient for the recall of that memory. Moreover, our experimental approach offers a general method of mapping cellular populations bearing memory engrams.     

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

The Hubble Deep Field provides one of the deepest multiwavelength views of the distant Universe and has led to the detection of thousands of galaxies seen throughout cosmic time. An early map of the Hubble Deep Field at a wavelength of 850?micrometres, which is sensitive to dust emission powered by star formation, revealed the brightest source in the field, dubbed HDF?850.1 (ref. 2). For more than a decade, and despite significant efforts, no counterpart was found at shorter wavelengths, and it was not possible to determine its redshift, size or mass. Here we report a redshift of z = 5.183 for HDF?850.1, from a millimetre-wave molecular line scan. This places HDF?850.1 in a galaxy overdensity at z?≈?5.2, corresponding to a cosmic age of only 1.1?billion years after the Big Bang. This redshift is significantly higher than earlier estimates and higher than those of most of the hundreds of submillimetre-bright galaxies identified so far. The source has a star-formation rate of 850 solar masses per year and is spatially resolved on scales of 5 kiloparsecs, with an implied dynamical mass of about 1.3?×?10(11) solar masses, a significant fraction of which is present in the form of molecular gas. Despite our accurate determination of redshift and position, a counterpart emitting starlight remains elusive.