Dissociation of the benzene molecule by ultraviolet and soft X-rays in circumstellar environment     

H. M. Boechat-Roberty  R. Neves  S. Pilling  A. F. Lago  G. G. B. de Souza 《Monthly notices of the Royal Astronomical Society》2009,394(2):810-817

Benzene molecules, present in the proto-planetary nebula CRL 618, are ionized and dissociated by ultraviolet (UV) and X-ray photons originated from the hot central star and by its fast wind. Ionic species and free radicals produced by these processes can lead to the formation of new organic molecules. The aim of this work is to study the photoionization and photodissociation processes of the benzene molecule, using synchrotron radiation and time-of-flight mass spectrometry. Mass spectra were recorded at different energies corresponding to the vacuum UV (21.21 eV) and soft X-ray (282–310 eV) spectral regions. The production of ions from the benzene dissociative photoionization is here quantified, indicating that C₆H₆ is more efficiently fragmented by soft X-ray than UV radiation, where 50 per cent of the ionized benzene molecules survive to UV dissociation while only about 4 per cent resist to X-rays. Partial ion yields of H⁺ and small hydrocarbons, such as  C₂H⁺₂, C₃H⁺₃, C₄H⁺₂  , are determined as a function of photon energy. Absolute photoionization and dissociative photoionization cross-sections have also been determined. From these values, half-life of benzene molecule due to UV and X-ray photon fluxes in CRL 618 was obtained.  相似文献   

Formation of H₂ on an olivine surface: a computational study     

T. P. M. Goumans  C. Richard  A. Catlow  Wendy A. Brown 《Monthly notices of the Royal Astronomical Society》2009,393(4):1403-1407

The formation of H₂ on a pristine olivine surface [forsterite (010)] is investigated computationally. Calculations show that the forsterite surface catalyzes H₂ formation by providing chemisorption sites for H atoms. The chemisorption route allows for stepwise release of the reaction exothermicity and stronger coupling to the surface, which increases the efficiency of energy dissipation. This suggests that H₂ formed on a pristine olivine surface should be much less rovibrationally excited than H₂ formed on a graphite surface. Gas-phase H atoms impinging on the surface will first physisorb relatively strongly  ( E _phys= 1240 K)  . The H atom can then migrate via desorption and re-adsorption, with a barrier equal to the adsorption energy. The barrier for a physisorbed H atom to become chemisorbed is equal to the physisorption energy, therefore there is almost no gas-phase barrier to chemisorption. An impinging gas-phase H atom can easily chemisorb  ( E _chem= 12 200 K)  , creating a defect where a silicate O atom is protonated and a single electron resides on the surface above the adjacent magnesium ion. This defect directs any subsequent impinging H atoms to chemisorb strongly (39 800 K) on the surface electron site. The two adjacent chemisorbed atoms can subsequently recombine to form H₂ via a barrier (5610 K) that is lower than the chemisorption energy of the second H atom. Alternatively, the adsorbed surface species can react with another incoming H atom to yield H₂ and regenerate the surface electron site. This double chemisorption 'relay mechanism' catalyzes H₂ formation on the olivine surface and is expected to attenuate the rovibrational excitation of H₂ thus formed.  相似文献   

Is H⁺₃ cooling ever important in primordial gas?     

S. C. O. Glover  D. W. Savin 《Monthly notices of the Royal Astronomical Society》2009,393(3):911-948

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Stability of C₆₀ and C₇₀ fullerenes toward corpuscular and γ radiation     

Franco Cataldo  Giovanni Strazzulla  Susana Iglesias-Groth 《Monthly notices of the Royal Astronomical Society》2009,394(2):615-623

The stability of C₆₀ and C₇₀ fullerenes in the interstellar medium deposited on dust surface or embedded in meteorites and comets has been simulated with γ irradiation and with He⁺ ion bombardment. It is shown by vibrational spectroscopy that a γ radiation dose of 2.6 MGy (1 Gy = 1 joule absorbed energy per kilogram) causes partial oligomerization of both C₆₀ and C₇₀ fullerenes. Oligomers are made by fullerene cages chemically connected each other which can yield back free fullerenes by a thermal treatment. The amount of irreversibly polymerized fullerenes caused by 2.6 MGy as deduced as the toluene insoluble fraction has been determined as 1.7 and 15 per cent by weight, respectively, for C₆₀ and C₇₀ fullerene. The radiation dose generated by radionuclides decay and expected to be delivered to fullerenes buried at a depth of more than 20 m in comets and meteorites is about 3 MGy per 10⁹ yr. Since fullerenes are by far resistant to such radiation dose they can survive for at least some billion years inside comets and meteorites and in fact have been detected inside certain carbonaceous chondrites. On the other hand, the direct exposure of fullerenes to cosmic rays for instance when they are adsorbed or deposited on the surface of carbon dust corresponds to the delivery of a radiation dose comprised between 30 and 65 MGy per 10⁹ yr. Experimental bombardment of both C₆₀ and C₇₀ fullerenes for instance with He⁺ ions has shown that the complete amorphization occurs at about 250 MGy. Thus in ∼4 Gyr exposure to cosmic rays it is expected a complete amorphization.  相似文献   

Laboratory investigations of the interaction between benzene and bare silicate grain surfaces     

J. D. Thrower  M. P. Collings  F. J. M. Rutten  M. R. S. McCoustra 《Monthly notices of the Royal Astronomical Society》2009,394(3):1510-1518

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The total and relative contribution of the relevant absorption processes to the opacity of DB white dwarf atmospheres in the UV and VUV regions     

Lj. M. Ignjatovi&#;  A. A. Mihajlov  N. M. Sakan  M. S. Dimitrijevi&#;  A. Metropoulos 《Monthly notices of the Royal Astronomical Society》2009,396(4):2201-2210

The main aim of this work is to estimate the total contribution of the processes of     molecular ion photodissociation and     collisional absorption charge exchange to the opacity of DB white dwarf atmospheres, and compare this with the contribution of     and other relevant radiative absorption processes included in standard models.
The method for the calculations of the molecular ion     photodissociation cross-sections is based on the dipole approximation and quantum-mechanical treatment of the internuclear motion, while the quasi-classical method for describing absorption processes in     collisions is based on the quasi-static approximation.
Absorption coefficients are calculated in the region  50 nm ≤λ≤ 850 nm  and compared with the corresponding coefficients of other relevant absorption processes; the calculations of the optical depth of the atmosphere layers considered are performed in the far-UV and VUV regions; the contribution of the relevant absorption processes to the opacity of DB white dwarf atmospheres is examined.
We examined the spectral ranges in which the total     and     absorption processes dominate in particular layers of DB white dwarf atmospheres. In addition, we show that in the region of  λ≲ 70 nm  the process of     atom photoionization is also important, in spite of the fact that the ratio of hydrogen and helium abundances in the DB white dwarf atmosphere considered is  1:10⁵  .  相似文献   

Cosmogenic production as a background in searching for rare physics processes     

D.-M. Mei  Z.-B. Yin  S.R. Elliott 《Astroparticle Physics》2009,31(6):417-420

We revisit calculations of the cosmogenic production rates for several long-lived isotopes that are potential sources of background in searching for rare physics processes such as the detection of dark matter and neutrinoless double-beta decay. Using updated cosmic-ray neutron flux measurements, we use TALYS 1.0 to investigate the cosmogenic activation of stable isotopes of several detector targets and find that the cosmogenic isotopes produced inside the target materials and cryostat can result in large backgrounds for dark matter searches and neutrinoless double-beta decay. We use previously published low-background HPGe data to constrain the production of ³H on the surface and the upper limit is consistent with our calculation. We note that cosmogenic production of several isotopes in various targets can generate potential backgrounds for dark matter detection and neutrinoless double-beta decay with a massive detector, thus great care should be taken to limit and/or deal with the cosmogenic activation of the targets.  相似文献   

An economical optical cloud/fog detector     

Jacqueline H. Carrillo  Scott E. Emert  D. Eli Sherman  Pierre Herckes  Jeffrey L. Collett Jr.   《Atmospheric Research》2008,87(3-4):259

A new, relatively low cost instrument has been developed to detect the presence of fog or cloud for fog/cloud sampling applications. The instrument uses attenuation of an 880 nm light emitting diode signal to detect cloud/fog drops in the optical path between a sending and receiving arm. Laboratory and field testing under a variety of conditions and fog types were carried out to determine the ability of the optical fog detector (OFD) to accurately detect cloud/fog presence as well as to provide some measure of liquid water content. Results indicated that the OFD provided a reliable estimate of fog presence as well as a reasonable estimate of liquid water content (LWC) under several different conditions. The OFD does appear to have an interference from rain, resulting in an overestimation of LWC during rainfall. This may occasionally give a false positive indication of fog presence.  相似文献   

DS-CDMA系统中两种盲多用户检测恒模算法的比较     

周先春 《南京气象学院学报》2008,31(6):890-894

研究了线性约束恒模算法（LCCMA,linear constrained constant modulus algorithm）和线性约束差分恒模算法（LCDCMA,linear constrained differential constant modulus algorithm）,并仿真试验了在期望用户信号幅度不同情况下这两种算法的收敛性和稳定性,仿真结果与理论推导相吻合。试验表明：LCCM算法只有在满足信号幅度是A≥1/3的情况下才能完全消除多址干扰（MAI,multiac-cess interference）,而LCDCM算法不论信号幅度是在≥1/3还是在〈1/√3条件下,都能够正确收敛到目标用户,具有很好的收敛性和稳定性,优越于LCCM算法。  相似文献   

基于局部阈值插值的地基云自动检测方法   总被引：3，自引：0，他引：3  

杨俊  吕伟涛  马颖  姚雯  李清勇 《气象学报》2010,68(6):1007-1017

地基云自动化观测是当前气象业务发展的迫切需求.目前的地基云检测算法仍主要是以阈值为基础,针对固定阈值和全局阈值算法在云检测精度方面存在的不足,利用晴朗天空下天空呈蓝色、云呈白色的属件,提出了一种基于局部阈值插值的地基云自动检测方法.该方法在对云图进行重采样后,对云图蓝、红波段进行归一化差值处理,再将处理后的结果图像按空间像素位置自动分成互不重叠、大小相等的均匀子块,对每一子区域采用一定的规则并结合改进的最大类间方差自适应阈值算法计算局部阈值,然后对每一子区域形成的阈值矩阵采用双线性插值算法进行插值处理,形成与原始云图大小相等的阈值曲面,利用此阈值曲面与云图蓝、红波段归一化差值处理结果进行比较,即可完成地基云的自动检测.与固定阈值和全局阈值算法相比,局部阈值插值算法对一些细碎的云和与背景反差不大的云获得了更好的检测效果.定量的评估结果表明,固定阈值方法在正确率和精确度上都要远远低于全局阈值和局部阈值方法,而文中提出的局部阈值算法在正确率和精确度上相比全局阈值算法又有较大提高.  相似文献