Solar flux in Saturn's atmosphere: Penetration and heating rates in the aerosol and cloud layers     

S. Pérez-Hoyos  A. Sánchez-Lavega 《Icarus》2006,180(2):368-378

In this work, we describe an analysis of the internal solar radiation fields in Saturn's atmosphere. The aim of this paper is to study how the solar radiation flux in optical wavelengths (0.25-1.0 μm) is attenuated, primarily by the effect of the aerosols located close to the tropopause level, retrieving also the corresponding solar heating rates. We use a doubling-adding method and previous results on the vertical cloud and haze structure of Saturn's atmosphere. Our study shows that the maximum penetration level (∼250 mbar) for these wavelengths is substantially higher than previously expected because of the huge optical thickness of the tropospheric haze described in all vertical cloud structure models. We compare our results with previous estimates and parameterizations for seasonal climate models and propose a new approach for future models, with an intense and concentrated heating rate close to the top level of the tropospheric haze. Given that our spectral range accounts for about the 70% of the total solar flux, and using previous estimates for the penetration levels of infrared radiation in Saturn's atmosphere, we conclude solar radiation effect is negligible at levels below 600 mbar. This result is fundamental for understanding the role of solar radiation in the general atmospheric circulation of Saturn.  相似文献   

Deuterium chemistry and airglow in the jovian thermosphere     

C.D. Parkinson  J.C. McConnell  A.Y.-T. Lee  E. Griffioen 《Icarus》2006,183(2):451-470

We present a detailed study of the distribution of key deuterated species (viz., atomic D and HD) and the associated deuterium Lyman-α airglow in the jovian thermosphere. The reactions that appear to govern the abundances of these deuterated species are used in conjunction with C₂-chemistry in a 1-D photochemical-diffusion model. While the D abundance is mainly sensitive to H densities and the vibrational temperature profile, the D vertical distribution also depends on other parameters such as eddy mixing and the uncertain values of some of the reaction rate constants. We consider different scenarios by varying several parameters controlling the D distribution in the thermosphere. A radiative transfer model with coupling of the H and D Lyman-α lines is employed to obtain line profiles and total intensities at disk center for these scenarios. This allows a comparison of the impact of various parameters on the jovian D Lyman-α emission. A consequence of these chemical processes in the jovian thermosphere is the formation of CH₂D, CH₃D, and C₂H₅D, and other deuterated species. We also discuss the source of these deuterated hydrocarbons and their abundance. We find that HD vibrational chemistry impacts D in the thermosphere, CH₃D and C₂H₅D are vibrationally enhanced in the thermosphere, and variations in abundance of CH₃D and C₂H₅D in the thermosphere may reflect dynamical activity (i.e., Kh) in the jovian upper atmosphere. An observing program dedicated to providing such measurements of these testable phenomena would provide further insight into the synergistic coupling between chemistry, energetics and airglow in the jovian upper atmosphere.  相似文献   

Atmosphere models of magnetized neutron stars: QED effects, radiation spectra and polarization signals     

M. van Adelsberg  D. Lai 《Monthly notices of the Royal Astronomical Society》2006,373(4):1495-1522

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Disc–corona energetics in the very high state of Galactic black holes     

Chris Done  Aya Kubota 《Monthly notices of the Royal Astronomical Society》2006,371(3):1216-1230

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Theoretical study of partial frequency redistribution function in irradiated, moving atmospheres of close binary components     

M. Srinivasa Rao 《Monthly notices of the Royal Astronomical Society》2006,371(1):303-311

We have studied the effects of partial frequency redistribution function with angle-averaged   R _II-A  in irradiated and moving atmospheres of close binary components. We have considered the atmospheric extension of the primary component to be twice the radius of the primary component in a close binary system. We have considered two cases: (i) when the atmosphere is at rest and (ii) when the atmosphere is moving. In both the cases, we have computed the line profiles along the line of sight for a given optical depth. The irradiation from the secondary component is assumed to be one, five and 10 times the self-radiation. The line fluxes in the line of sight are calculated by using the total source functions due to self-radiation of the primary component and due to the irradiation from the secondary component. We have noted double-peaked emission lines in the case of a static medium and a reduction of emission peaks in the case of velocity field.  相似文献   

Cosmological radiative transfer codes comparison project – I. The static density field tests     

Ilian T. Iliev  Benedetta Ciardi  Marcelo A. Alvarez  Antonella Maselli  rea Ferrara  Nickolay Y. Gnedin  Garrelt Mellema  Taishi Nakamoto  Michael L. Norman  Alexei O. Razoumov  Erik-Jan Rijkhorst  Jelle Ritzerveld  Paul R. Shapiro  Hajime Susa  Masayuki Umemura  Daniel J. Whalen 《Monthly notices of the Royal Astronomical Society》2006,371(3):1057-1086

Radiative transfer (RT) simulations are now at the forefront of numerical astrophysics. They are becoming crucial for an increasing number of astrophysical and cosmological problems; at the same time their computational cost has come within reach of currently available computational power. Further progress is retarded by the considerable number of different algorithms (including various flavours of ray tracing and moment schemes) developed, which makes the selection of the most suitable technique for a given problem a non-trivial task. Assessing the validity ranges, accuracy and performances of these schemes is the main aim of this paper, for which we have compared 11 independent RT codes on five test problems: (0) basic physics; (1) isothermal H  ii region expansion; (2) H  ii region expansion with evolving temperature; (3) I-front trapping and shadowing by a dense clump and (4) multiple sources in a cosmological density field. The outputs of these tests have been compared and differences analysed. The agreement between the various codes is satisfactory although not perfect. The main source of discrepancy appears to reside in the multifrequency treatment approach, resulting in different thicknesses of the ionized-neutral transition regions and the temperature structure. The present results and tests represent the most complete benchmark available for the development of new codes and improvement of existing ones. To further this aim all test inputs and outputs are made publicly available in digital form.  相似文献   

Wouthuysen–Field coupling strength and application to high-redshift 21-cm radiation     

Christopher M. Hirata 《Monthly notices of the Royal Astronomical Society》2006,367(1):259-274

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时间和频率技术新进展   总被引：5，自引：0，他引：5  

张昱  翟造成 《天文学进展》1997,15(4):285-292

概述了最近几年时间和频率技术的最新进展，给出了各种实用的原子频率标准的最新发展以及它们的性能指标的最新结果，介绍了国际原子时的归算方法和所达到的新水平，并对各种原子钟在归算子中的应用概况和所起的作用进行了比较，强调了氢原子钟的特殊作用和地位，同时也综述了高精度的时间同步和时频计量新技术的进展，特别是对为提高ＧＰＳ这一国际时间同步辐射技术的应用水平进行的各种实验研究工作的最新进展作了进行描述，对目前  相似文献   

Synthetic infrared images and spectral energy distributions of a young low-mass stellar cluster     

Ryuichi Kurosawa  Tim J. Harries  Matthew R. Bate  Neil H. Symington 《Monthly notices of the Royal Astronomical Society》2004,351(4):1134-1150

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一次闽南暖区暴雨的多尺度动力过程     

王美玲  梁湘三 《热带气象学报》2022,38(3):467-480

作为气象研究中的一个难点问题,暖区暴雨的动力学一直为学界所关注。基于多尺度子空间变换(MWT)以及基于MWT的局地多尺度能量学分析和正则传输理论,对2018年5月7日的一次闽南暖区暴雨进行研究以了解其多尺度动力过程。首先将原始物理量场重建到三个尺度子空间:背景流子空间、天气尺度子空间和暴雨子空间。重构场上可以很好地看出背景环流尺度的高低空急流,以及暴雨尺度上的垂直环流。以往的研究普遍认为暖区暴雨的动力过程具有弱斜压性这一特征,而就此次事件而言,正压失稳和斜压失稳都起着很关键的作用,暴雨主要落区内既发生了正压失稳,也发生了斜压失稳。研究表明,对流层不同高度上的动力学存在差异,低层主要表现为正压失稳,天气尺度子空间与背景流子空间向暴雨子空间传输的动能相当; 中层主要是混合失稳,除正压失稳外,斜压正则传输也将有效位能从背景流子空间传输到了暴雨子空间,再通过浮力转换将有效位能转为动能,从而维持暴雨在中层的动力过程; 高层则与低层相似,但只存在背景流子空间向暴雨子空间的能量传输。   相似文献