다중혈관 관상동맥 환자에서 y-문합을 이용하여 양쪽 내흉동맥만을 사용한 우회술의 조기 성적

抗原变异可使得多种致病微生物易于逃避宿主免疫应答。表达在感染红细胞表面的恶性疟原虫红细胞表面蛋白1（PfPMP1）与感染红细胞、内皮细胞、树突状细胞以及胎盘的单个或多个受体作用，在黏附及免疫逃避中起关键的作用。每个单倍体基因组var基因家族编码约60种成员，通过启动转录不同的var基因变异体为抗原变异提供了分子基础。

疟原虫var基因转换速率变化导致抗原变异[英]／Paul H, Robert P, Christodoulou Z, et al//Proc Natl Acad Sci U S A

Deposits of clastic carbonate-dominated (calciclastic) sedimentary slope systems in the rock record have been identified mostly as linearly-consistent carbonate apron deposits, even though most ancient clastic carbonate slope deposits fit the submarine fan systems better. Calciclastic submarine fans are consequently rarely described and are poorly understood. Subsequently, very little is known especially in mud-dominated calciclastic submarine fan systems. Presented in this study are a sedimentological core and petrographic characterisation of samples from eleven boreholes from the Lower Carboniferous of Bowland Basin (Northwest England) that reveals a >250 m thick calciturbidite complex deposited in a calciclastic submarine fan setting. Seven facies are recognised from core and thin section characterisation and are grouped into three carbonate turbidite sequences. They include: 1) Calciturbidites, comprising mostly of highto low-density, wavy-laminated bioclast-rich facies; 2) low-density densite mudstones which are characterised by planar laminated and unlaminated muddominated facies; and 3) Calcidebrites which are muddy or hyper-concentrated debrisflow deposits occurring as poorly-sorted, chaotic, mud-supported floatstones. These

Phd by thesis

This paper describes the contents of the 2016 edition of the HITRAN molecular spectroscopic compilation. The new edition replaces the previous HITRAN edition of 2012 and its updates during the intervening years. The HITRAN molecular absorption compilation is composed of five major components: the traditional line-by-line spectroscopic parameters required for high-resolution radiative-transfer codes, infrared absorption cross-sections for molecules not yet amenable to representation in a line-by-line form, collision-induced absorption data, aerosol indices of refraction, and general tables such as partition sums that apply globally to the data. The new HITRAN is greatly extended in terms of accuracy, spectral coverage, additional absorption phenomena, added line-shape formalisms, and validity. Moreover, molecules, isotopologues, and perturbing gases have been added that address the issues of atmospheres beyond the Earth. Of considerable note, experimental IR cross-sections for almost 300 additional molecules important in different areas of atmospheric science have been added to the database. The compilation can be accessed through www.hitran.org. Most of the HITRAN data have now been cast into an underlying relational database structure that offers many advantages over the long-standing sequential text-based structure. The new structure empowers the user in many ways. It enables the incorporation of an extended set of fundamental parameters per transition, sophisticated line-shape formalisms, easy user-defined output formats, and very convenient searching, filtering, and plotting of data. A powerful application programming interface making use of structured query language (SQL) features for higher-level applications of HITRAN is also provided.

/pdf/the-hitran-2008-molecular-spectroscopic-database-1ud8clpej3.pdf

The HITRAN 2008 molecular spectroscopic database

We substantially update the capabilities of the open source software package Modules for Experiments in Stellar Astrophysics (MESA), and its one-dimensional stellar evolution module, MESA star. Improvements in MESA star's ability to model the evolution of giant planets now extends its applicability down to masses as low as one-tenth that of Jupiter. The dramatic improvement in asteroseismology enabled by the space-based Kepler and CoRoT missions motivates our full coupling of the ADIPLS adiabatic pulsation code with MESA star. This also motivates a numerical recasting of the Ledoux criterion that is more easily implemented when many nuclei are present at non-negligible abundances. This impacts the way in which MESA star calculates semi-convective and thermohaline mixing. We exhibit the evolution of 3-8 M ? stars through the end of core He burning, the onset of He thermal pulses, and arrival on the white dwarf cooling sequence. We implement diffusion of angular momentum and chemical abundances that enable calculations of rotating-star models, which we compare thoroughly with earlier work. We introduce a new treatment of radiation-dominated envelopes that allows the uninterrupted evolution of massive stars to core collapse. This enables the generation of new sets of supernovae, long gamma-ray burst, and pair-instability progenitor models. We substantially modify the way in which MESA star solves the fully coupled stellar structure and composition equations, and we show how this has improved the scaling of MESA's calculational speed on multi-core processors. Updates to the modules for equation of state, opacity, nuclear reaction rates, and atmospheric boundary conditions are also provided. We describe the MESA Software Development Kit that packages all the required components needed to form a unified, maintained, and well-validated build environment for MESA. We also highlight a few tools developed by the community for rapid visualization of MESA star results.

/pdf/modules-for-experiments-in-stellar-astrophysics-mesa-planets-29j324a9bq.pdf

Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars

The IUPAC Database of Rotational-Vibrational Energy Levels and Transitions of Water Isotopologues from Experiment and Theory

We have obtained narrow-band images of the Orion Molecular Cloud OMC-1 in various infrared transitions of molecular hydrogen. The molecular emission from levels with low excitation energies (less than or similar to 15 000 K) is made up of numerous linear, jet-like structures. Their collimation factor is typically about 10 and there is no appreciable outward broadening. Most of these structures are arranged radially and seem to originate from an area close to IRc2. They however only become detectable at a projected distance of similar to 10(17) cm from the IRc2 area. The projected length of the linear features is a few times 10(17) cm. Some of the H-2 fingers seem to be associated with fast moving H2O masers.H-2 emission from higher levels (greater than or similar to 19 000 K) shows a different nebular structure: Two nebulosities, one around BN which is bipolar and the other one extending north-eastwards of IRc2 in the Peak 2 region, are detected. Images in various continuum wavelengths show the same pattern as the H-2 emission from high levels.From these images and in conjunction with long slit K and L band spectra of the Peak 2 region we obtain a map of the molecular temperature in OMC-1. The resulting temperature distribution shows little spatial structure on small or intermediate distance scales. It does not show the jet-like structures anymore but displays radial symmetry.The highly structured H-2 emission is mainly due to strong density rather than temperature variations. The observations suggest that the H-2 emission in the linear structures comes from a thin sheet with a thickness of less than one hundredth of the jet width. It is most likely due to molecular material swept up or entrained into the jet from the outside.The visual impression provided by high resolution images is that of very dynamic processes disrupting a molecular cloud. The observed structure has been described by the wakes of dense ''bullets'' ploughing through the surrounding molecular gas. The smooth and only radially variable temperature distribution can however best be interpreted in terms of instabilities in the interaction zone of a stellar wind which collides with surrounding dense molecular material. A thin layer of shocked material is subject to rapidly growing instabilities which may be responsible for the observed linear structures. We draw attention to the fact that the ''thin layer instability'' in rapidly cooling radiative shock zones may be more important than Rayleigh-Taylor instabilities.We have also obtained Fabry-perot images of OMC-1 in the light of selected K band transitions of the molecular ion H-3(+). These include 2 nu(2)(2) R(6) at 2.0933 mu m, 2 nu(2)(2) Q(4) at 2.1944 mu m, 2 nu(2)(2) R(8) at 2.1342 mu m, 2 nu(2)(2) P(5) at 2.2028 mu m and 2 nu(2)(2) P(3) at 2.2039 mu m. No H-3(+) was detected. We also observed Peak 2 spectroscopically in the L band but again without a detection of H-3(+). These observations set a probable upper limit of the H-3(+) concentration of 8.2 x 10(9) cm(-2) OMC-1.

The H-2 structure of OMC-1 (vol 318, pg 608, 1997)

A preliminary version of the line list of dipole-allowed transition of the water molecule is presented. The line lists is created on the basis of VoTe calculations (Voronin, Tennyson et al. in preparation). The cut-of values used for this line list are: 25000 cm-1 in wave number and 10-30 cm/molecule at T=296 K in intensity. Calculated line-lists are available on the site ftp://ftp.iao.ru/pub/VTT/VoTe/.

/pdf/the-vote-room-temperature-h-2-16-o-line-list-up-to-25000-cm-4zpiky6ytt.pdf

The VoTe room temperature H 2 16 O line list up to 25000 cm -1

It is now widely accepted that collisions with low-energy electrons are the major cause of radiation damage in living cells and that it is the capture of these electrons into long-lived quasi-bound states, resonances, that is responsible for this damage. We have undertaken a set of systematic calculations using the UK Molecular R-matrix codes to study electron collisions with DNA and RNA bases. Here we summarise the results of our calculations for electron collisions with adenine, guanine, uracil, cytosine and thymine. These studies aim to characterize not only low-lying shape resonances, which have been relatively well-studied, but also to detect longer-lived Feshbach resonances which are associated with simultaneous electronic excitation of the target molecule. The results of these calculations are dependent on the model chosen: only the more sophisticated, and computationally expensive, models give Feshbach resonances.

Resonances in Electron Collisions with Small Biomolecules Using the R-Matrix Method

Electron-molecule scattering calculations have been carried out using the UK Molecular R-Matrix codes on 3 neutral radicals observed in space, CN, C3N & C2H. These calculations investigate the rates of formation of the relevant molecular anions in space. It was found that all scattering resonances are of too high energy for temporary resonance states to lead to anion formation. However weakly bound anionic states may provide a possible route to formation.

https://iopscience.iop.org/article/10.1088/1742-6596/388/5/052003/pdf

Jonathan Tennyson

Papers

The IUPAC Database of Rotational-Vibrational Energy Levels and Transitions of Water Isotopologues from Experiment and Theory

The H-2 structure of OMC-1 (vol 318, pg 608, 1997)

The VoTe room temperature H 2 16 O line list up to 25000 cm -1

Resonances in Electron Collisions with Small Biomolecules Using the R-Matrix Method

Electron collsions with the interstellar molecular radicals CN, C3N & C2H using the R-Matrix method