Distribution of aliphatic amines in CO,CV, and CK carbonaceous chondrites and relation to mineralogy and processing history

The analysis of water‐soluble organic compounds in meteorites provides valuable insights into the prebiotic synthesis of organic matter and the processes that occurred during the formation of the solar system. We investigated the concentration of aliphatic monoamines present in hot acid water extracts of the unaltered Antarctic carbonaceous chondrites, Dominion Range (DOM) 08006 (CO3) and Miller Range (MIL) 05013 (CO3), and the thermally altered meteorites, Allende (CV3), LAP 02206 (CV3), GRA 06101 (CV3), Allan Hills (ALH) 85002 (CK4), and EET 92002 (CK5). We have also reviewed and assessed the petrologic characteristics of the meteorites studied here to evaluate the effects of asteroidal processing on the abundance and molecular distributions of monoamines. The CO3, CV3, CK4, and CK5 meteorites studied here contain total concentrations of amines ranging from 1.2 to 4.0 nmol g^?1 of meteorite; these amounts are 1–3 orders of magnitude below those observed in carbonaceous chondrites from the CI, CM, and CR groups. The low‐amine abundances for CV and CK chondrites may be related to their extensive degree of thermal metamorphism and/or to their low original amine content. Although the CO3 meteorites, DOM 08006 and MIL 05013, do not show signs of thermal and aqueous alteration, their monoamine contents are comparable to those observed in moderately/extensively thermally altered CV3, CK4, and CK5 carbonaceous chondrites. The low content of monoamines in pristine CO carbonaceous chondrites suggests that the initial amounts, and not asteroidal processes, play a dominant role in the content of monoamines in carbonaceous chondrites. The primary monoamines, methylamine, ethylamine, and n‐propylamine constitute the most abundant amines in the CO3, CV3, CK4, and CK5 meteorites studied here. Contrary to the predominance of n‐ω‐amino acid isomers in CO3 and thermally altered meteorites, there appears to be no preference for the larger n‐amines.     

On The Origin of The High-Perihelion Scattered Disk: The Role of The Kozai Mechanism And Mean Motion Resonances

We study the transfer process from the scattered disk (SD) to the high-perihelion scattered disk (HPSD) (defined as the population with perihelion distances q > 40 AU and semimajor axes a>50 AU) by means of two different models. One model (Model 1) assumes that SD objects (SDOs) were formed closer to the Sun and driven outwards by resonant coupling with the accreting Neptune during the stage of outward migration (Gomes 2003b, Earth, Moon, Planets 92, 29–42.). The other model (Model 2) considers the observed population of SDOs plus clones that try to compensate for observational discovery bias (Fernández et al. 2004, Icarus , in press). We find that the Kozai mechanism (coupling between the argument of perihelion, eccentricity, and inclination), associated with a mean motion resonance (MMR), is the main responsible for raising both the perihelion distance and the inclination of SDOs. The highest perihelion distance for a body of our samples was found to be q = 69.2 AU. This shows that bodies can be temporarily detached from the planetary region by dynamical interactions with the planets. This phenomenon is temporary since the same coupling of Kozai with a MMR will at some point bring the bodies back to states of lower-q values. However, the dynamical time scale in high-q states may be very long, up to several Gyr. For Model 1, about 10% of the bodies driven away by Neptune get trapped into the HPSD when the resonant coupling Kozai-MMR is disrupted by Neptune’s migration. Therefore, Model 1 also supplies a fossil HPSD, whose bodies remain in non-resonant orbits and thus stable for the age of the solar system, in addition to the HPSD formed by temporary captures of SDOs after the giant planets reached their current orbits. We find that about 12 – 15% of the surviving bodies of our samples are incorporated into the HPSD after about 4 – 5 Gyr, and that a large fraction of the captures occur for up to the 1:8 MMR (a ⋍ 120 AU), although we record captures up to the 1:24 MMR (a ≃ 260 AU). Because of the Kozai mechanism, HPSD objects have on average inclinations about 25°–50°, which are higher than those of the classical Edgeworth–Kuiper (EK) belt or the SD. Our results suggest that Sedna belongs to a dynamically distinct population from the HPSD, possibly being a member of the inner core of the Oort cloud. As regards to 2000 CR₁₀₅ , it is marginally within the region occupied by HPSD objects in the parametric planes (q,a) and (a,i), so it is not ruled out that it might be a member of the HPSD, though it might as well belong to the inner core.     

Micro-XCT chondrule classification for subsequent isotope analysis

Chondrules are microscopic, recrystallized melt droplets found in chondritic meteorites. High-resolution isotope analyses of minor elements require large enough element quantities which are obtained by dissolving entire chondrules. This work emphasizes the importance of X-ray computed tomography (XCT) to detect features that can significantly affect the bulk chondrule isotope composition. It thereby expands on other works by looking into chondrules from a wide range of chondrites including CR, CV, CB, CM, L, and EL samples before turning toward complex and time-consuming chemical processing. The features considered are metal and igneous rims, compound chondrules, matrix remnants, and metal contents. In addition to the identification of these features, computed tomography prevents the inclusion of non-chondrule samples (pure matrix or metal) as well as samples where two different chondrule fragments with potentially different isotope compositions are held together by matrix. Matrix surrounding chondrules is also easily detected and the affected chondrules can be omitted or reprocessed. The results strongly encourage to perform XCT before dissolution of chondrules for isotope analysis as a non-invasive method.     

Spatial and temporal evolution of soft and hard X-ray emission in a solar flare

We study the spatial and temporal characteristics of the 3.5 to 30.0 keV emission in a solar flare on April 10, 1980. The data were obtained by the Hard X-ray Imaging Spectrometer aboard the Solar Maximum Mission Satellite. It is complemented in our analysis with data from other instruments on the same spacecraft, in particular that of the Hard X-ray Burst Spectrometer.Key results of our investigation are: (a) Continuous energy release is needed to substain the increase of the emission through the rising phase of the flare, before and after the impulsive phase in hard X-rays. The energy release is characterized by the production of hot (5 × 10⁷ T 1.5 × 10⁸ K) thermal regions within the flare loop structures. (b) The observational parameters characterizing the impulsive burst show that it is most likely associated with non-thermal processes (particle acceleration). (c) The continuous energy release is associated with strong chromospheric evaporation, as evidenced in the spectral line behavior determined from the Bent Crystal Spectrometer data. Both processes seem to stop just before flare maximum, and the subsequent evolution is most likely governed by the radiative cooling of the flare plasma.     

The magnetic properties of solar surges

High resolution on- and off-band Hα filtergrams of disk solar surges obtained with the Vacuum Tower Telescope of the Sacramento Peak Observatory have been compared to magnetic data.

1. Surges constitute clusters of very fine dark (sometimes bright) filaments where each thread connects to an Ellerman bomb brightening. If the magnetic map reveals the existence of a satellite polarity as defined by Rust (1968), the bomb(s) lies over it.
2. Although a large fraction of surges is not associated with clearly detectable satellite polarities, events are strongly favored in regions of evolving magnetic features, characterized by dimensions of about 10 000 km and significant flux change over a period of less than a day. A flux change rate of 3 × 10¹⁵ Mx s^?1 has been measured along at least three homologous bomb-surge events in a satellite of region MW 18594. Surges appear to be related to rising flux of one polarity into a region of stronger opposite flux.
3. The trajectories of surges are matched by magnetic lines of force computed in the current-free approximation.

     

Detection of a high-confidence quasi-periodic oscillation in radio light curve of the high redshift FSRQ PKS J0805–0111

In this work,we have searched for quasi-periodic oscillations(QPOs)in the 15 GHz light curve of the FSRQ PKS J0805-0111 monitored by the Owens Valley Radio Observatory(OVRO)40 m telescope during the period from 2008 January 9 to 2019 May 9,using the weighted wavelet Z-transform(WWZ)and the Lomb-Scargle Periodogram(LSP)techniques.This is the first time to search for a periodic radio signal in the FSRQ PKS J0805-0111 by these two methods.Both methods consistently reveal a repeating signal with a periodicity of 3.38±0.8 yr(>99.7%confidence level).In order to determine the significance of the periods,the false alarm probability method was applied,and a large number of Monte Carlo simulations were performed.As possible explanations,we discuss a number of scenarios including the thermal instability of thin disks scenario,the spiral jet scenario and the binary supermassive black hole scenario.We expect that the binary black hole scenario,where the QPO is caused by the precession of binary black holes,is the most likely explanation.FSRQ PKS J0805-0111 thus could be a good binary black hole candidate.In the binary black hole scenario,the distance between the primary black hole and the secondary black hole is about 1.71×10¹⁶ cm.     

黄河口及其邻近水域强壮箭虫密度的时空分布及其与环境因子的关系

为探究强壮箭虫（Sagitta crassa）在黄河口及其邻近水域的时空分布特征及其与生物和非生物环境等因子的关系,本文依据2013—2014年在黄河口及其邻近水域6个航次的调查数据,采用丛生指标（I）、聚块性指标（A）和负二项分布参数的倒数（C_A）等聚集指标,分析了强壮箭虫的空间分布特征;应用广义可加模型（GAM）研究了强壮箭虫密度的时空分布和环境因子的关系。结果表明,黄河口及其邻近水域强壮箭虫平均密度为21.85 ind/m3,春、秋季高,冬、夏季低;其密度的空间分布以黄河入海口附近水域为密集中心,向远岸水域逐渐降低;强壮箭虫在黄河口及其邻近水域的聚集特征随密度的变化存在两次聚集和两次扩散;水深、表层水温和浮游桡足类密度是影响其密度时空分布的主要因子,总偏差解释率为55.11%,强壮箭虫密度随水深的增加而减小,随表层水温的升高先增加后减小,随桡足类密度的增加而增加。强壮箭虫密度受黄河口及其邻近水域环境因子变动的影响,具有明显的季节变化和空间分布规律。     

海南岛直尾颚足钩虾(甲壳动物:端足目,颚足钩虾科)的补充描述

颚足钩虾属 Maxillipius (端足目,颚足钩虾科 Family Maxillipiidae)中,迄今仅有2种,即直尾颚足钩虾 Maxillipius rectitelson Ledoyer和共栖颚足钩虾 Maxillipius commensalis Ledoyer。直尾颚足钩虾的模式标本采自马达加斯加,仅有雌体。虽然后来Ledoyer(1986)又进行了补充描记,但因缺乏雄体标本,使该种的描述不完善。作者在海南岛潮间带采集中,获得较多该种标本,仅雄体就有27个,并发现雄、雌第1触角形态表现为雌、雄异形(sexual dimorphism)。这与Thomas (1996)所描述的Maxillipius commensalis Ledoyer雌、雄体形态差异相似,即在雄体第1触角第3柄节上具柄突(callynophore),该柄突在 Maxillipiidae 科中为 Maxillipius 属区别于 Maxillipides 属的主要特征。 本文为直尾颚足钩虾 Maxillipius rectitelson Ledoyer 的补充描述。     

厚壳贻贝（Mytilus coruscus）McNF-κB基因的克隆及其在发育中的作用

核因子κB（Nuclear Factor kappa-B,NF-κB）具有免疫、炎症、凋亡、细胞增殖和发育的调节作用,目前NF-κB在脊椎动物和果蝇中的研究较为丰富,在贝类中的报道较少。为进一步探究NF-κB在厚壳贻贝（Mytilus coruscus）免疫和发育中的作用,本研究克隆了厚壳贻贝McNF-κB基因的序列全长,其全长为4 087 bp,开放阅读框为2 613 bp,编码871个氨基酸,具有典型的锚蛋白重复序列（ankyrinrepeat, ANK）结构域和死亡结构域。氨基酸序列分析结果发现,该基因与欧洲贻贝（Mytilus edulis）和地中海贻贝（Mytilus galloprovincialis）分别具有72.76%和66.58%同源性,且在系统进化树中与欧洲贻贝和地中海贻贝聚为一支。经实时荧光定量PCR（qRT-PCR）技术检验表明,McNF-κB基因于厚壳贻贝各组织均有分布,在鳃中表达最高;McNF-κB基因在厚壳贻贝眼点幼虫阶段和稚贝阶段均有表达,且在稚贝阶段表达量显著高于眼点幼虫阶段。利用RNA干扰技术沉默眼点幼虫McNF-κB基因后幼虫变态率显著下降,推测McNF-κB基因调控厚壳贻贝幼虫变态过程。本研究为探究McNF-κB基因如何调控厚壳贻贝发育奠定了基础。