Condensed species in Titan's stratosphere: Confirmation of crystalline cyanoacetylene (HC₃N) and evidence for crystalline acetylene (C₂H₂) on Titan     

R.K. Khanna 《Icarus》2005,178(1):165-170

Infrared spectra of crystalline HC₃N and C₂H₂ were investigated at several temperatures between 15 and 150 K. The characteristics of the 505 and 753 cm⁻¹ bands of HC₃N are in complete agreement with the emission spectral data on Titan obtained by the Voyager IRIS instrument, thus confirming the identification of crystalline HC₃N on Titan. A composite spectrum in the 720-800 cm⁻¹ region, with contributions from HC₃N and C₂H₂ in crystalline phases, reproduces the Voyager emission data in that region, thus providing a suggestion for the identification of crystalline C₂H₂ on Titan.  相似文献   

Polarized radiation diagnostics of magnetohydrodynamic models of the solar atmosphere     

O. Steiner  U. Grossmann-Doerth  M. Schüssler  M. Knölker 《Solar physics》1996,164(1-2):223-242

Solar magnetic elements and their dynamical interaction with the convective surface layers of the Sun are numerically simulated. Radiation transfer in the photosphere is taken into account. A simulation run over 18.5 minutes real time shows that the granular flow is capable of moving and bending a magnetic flux sheet (the magnetic element). At times it becomes inclined by up to 30° with respect to the vertical around the level ₅₀₀₀ = 1 and it moves horizontally with a maximal velocity of 4 km/s. Shock waves form outside and within the magnetic flux sheet. The latter cause a distinctive signature in a time series of synthetic Stokes V-profiles. Such shock events occur with a mean frequency of about 2.5 minutes. A time resolution of at least 10 seconds in Stokes V recordings is needed to reveal an individual shock event by observation.The National Center for Atmospheric Research is sponsored by the National Science Foundation  相似文献   

热带平流层CO浓度准两年振荡的位相变化特征     

王春晓  田文寿 《大气科学》2017,41(2):275-288

利用2005~2014年10年的卫星微波临边探测仪（MLS）资料分析了热带平流层一氧化碳（CO）体积混合比的年际变率,发现热带平流层CO浓度的准两年振荡（QBO）在30 hPa高度附近存在明显的位相变化特征。大气化学气候模式模拟结果表明,热带平流层CO的准两年振荡信号是化学和动力过程共同作用的结果,而动力作用主要是QBO引起的次级经向环流引起的物质传输。化学和动力过程共同作用导致热带平流层CO浓度的垂直梯度在30 hPa高度处发生反转,进而产生一氧化碳QBO信号的位相变化。此外,化学气候模式模拟结果还表明,与CO有关的化学过程不但可以减弱一氧化碳QBO信号的振幅,还可以在热带30~10 hPa高度范围内造成一氧化碳QBO和纬向风QBO信号之间约3个月的时间差。  相似文献   

Atmospheric input of anthropogenic phosphorus to the northwest mediterranean under oligotrophic conditions     

C. Migon  V. Sandroni  J. -P. Bthoux 《Marine environmental research》2001,52(5):413-426

Phosphorus (P) concentration in the atmospheric aerosol was measured at a northwestern Mediterranean coastal site. Airborne P ranged between 25 and 85 ng m(-3) (geometric mean: 51 ng m(-3)). Due to a significant contribution (about 90%) of anthropogenic land-based source emissions, dry deposition velocities of 0.1-0.5 cm s(-1) were used to estimate a dry flux of 0.15-0.7 micromol P m(-2) day(-1). The theoretical impact of the dry flux on primary production (0.1-0.4 mg C m(-2) day(-1)) is 50-200-fold lower than that of a single significant wet event. The incineration plant of the Nice district is identified as a possible major source of airborne anthropogenic P. As the implementation of waste plants is currently expanding along the western European shores, the importance of the P atmospheric source to the western Mediterranean is likely to increase with time.  相似文献   

‘Pour votre tranquillité’: Ambiance,atmosphere, and surveillance     

《Geoforum》2013

This is a paper concerned with security, surveillance and notions of atmosphere and ambience. Whilst surveillance and security research has been excellent at examining socio-spatial relations drawn into the production and consumption of surveillance technologies, systems and practices, it has been far less well attuned to the material–affective relations, presences and absences it comes to constitute as the fabric of public space. Research within human geography and a broader ‘new materialism’ within the humanities and social sciences has become increasingly interested in exploring affective atmospheres, yet largely ignorant of a well established school of thought within French urban and social theory of ‘ambiance’. This paper explores the providence of considering atmospheres and ambiances for the examination of surveillance through the case study of two major railway stations in Britain and France. The paper proffers some methods and techniques for the further exploration of atmospheres/ambiances of security.  相似文献   

Production, ionization and redistribution of O₂ in Saturn's ring atmosphere     

R.E. Johnson  J.G. Luhmann  M. Bouhram  E.C. Sittler  T.W. Hill  M. Michael  M. Liu  D.T. Young 《Icarus》2006,180(2):393-402

Molecular oxygen produced by the decomposition of icy surfaces is ubiquitous in Saturn's magnetosphere. A model is described for the toroidal O₂ atmosphere indicated by the detection of and O⁺ over the main rings. The O₂ ring atmosphere is produced primarily by UV photon-induced decomposition of ice on the sunlit side of the ring. Because O₂ has a long lifetime and interacts frequently with the ring particles, equivalent columns of O₂ exist above and below the ring plane with the scale height determined by the local ring temperature. Energetic particles also decompose ice, but estimates of their contribution over the main rings appear to be very low. In steady state, the O₂ column density over the rings also depends on the relative efficiency of hydrogen to oxygen loss from the ring/atmosphere system with oxygen being recycled on the grain surfaces. Unlike the neutral density, the ion densities can differ on the sunlit and shaded sides due to differences in the ionization rate, the quenching of ions by the interaction with the ring particles, and the northward shift of the magnetic equator relative to the ring plane. Although O⁺ is produced with a significant excess energy, is not. Therefore, should mirror well below those altitudes at which ions were detected. However, scattering by ion-molecule collisions results in much larger mirror altitudes, in ion temperatures that go through a minimum over the B-ring, and in the redistribution of both molecular hydrogen and oxygen throughout the magnetosphere. The proposed model is used to describe the measured oxygen ion densities in Saturn's toroidal ring atmosphere and its hydrogen content. The oxygen ion densities over the B-ring appear to require either significant levels of UV light scattering or ion transmission through the ring plane.  相似文献   

Principal components analysis of Mars in the near-infrared     

David R. Klassen 《Icarus》2009,204(1):32-47

Principal components analysis and target transformation are applied to near-infrared image cubes of Mars in a study to disentangle the spectra into a small number of spectral endmembers and characterize the spectral information. The image cubes are ground-based telescopic data from the NASA Infrared Telescope Facility during the 1995 and 1999 near-aphelion oppositions when ice clouds were plentiful [ [Clancy et al., 1996] and [56]], and the 2003 near-perihelion opposition when ice clouds are generally limited to topographically high regions (volcano cap clouds) but airborne dust is more common [Martin, L.J., Zurek, R.W., 1993. J. Geophys. Res. 98 (E2), 3221-3246]. The heart of the technique is to transform the data into a vector space along the dimensions of greatest spectral variance and then choose endmembers based on these new “trait” dimensions. This is done through a target transformation technique, comparing linear combinations of the principal components to a mineral spectral library. In general Mars can be modeled, on the whole, with only three spectral endmembers which account for almost 99% of the data variance. This is similar to results in the thermal infrared with Mars Global Surveyor Thermal Emission Spectrometer data [Bandfield, J.L., Hamilton, V.E., Christensen, P.R., 2000. Science 287, 1626-1630]. The globally recovered surface endmembers can be used as inputs to radiative transfer modeling in order to measure ice abundance in martian clouds [Klassen, D.R., Bell III, J.F., 2002. Bull. Am. Astron. Soc. 34, 865] and a preliminary test of this technique is also presented.  相似文献   

Evidence for condensed-phase methane enhancement over Xanadu on Titan     

M. Ádámkovics  I. de Pater  J.W. Barnes 《Planetary and Space Science》2009,57(13):1586-1595

We present evidence for condensed-phase methane precipitation near Xanadu using nine nights of observations from the SINFONI integral-field spectrograph at the Very Large Telescope and imaging analysis with empirical surface subtraction. Radiative transfer models are used to support the imaging technique by simulating the spectrometer datacubes and testing for variations in both the surface reflectivity spectrum and atmospheric opacity. We use the models and observations together to argue against artifacts that may arise in the image analysis. High phase angle observations from Cassini/VIMS are used to test against surface scattering artifacts that may be confused with sources of atmospheric opacity. Although changes in the surface reflectivity spectrum can reproduce observations from a particular viewing geometry on a given night, multiple observations are best modeled by condensed-phase methane opacity near the surface. These observations and modeling indicate that the condensed-phase methane opacity observed with this technique occurs predominantly near Xanadu and is most likely due to precipitation.  相似文献   

Kronos: exploring the depths of Saturn with probes and remote sensing through an international mission     

《Experimental Astronomy》2009,23(3):947-976

Kronos is a mission aimed to measure in situ the chemical and isotopic compositions of the Saturnian atmosphere with two probes and also by remote sensing, in order to understand the origin, formation, and evolution of giant planets in general, including extrasolar planets. The abundances of noble gases, hydrogen, carbon, nitrogen, oxygen, sulfur and their compounds, as well as of the D/H, ⁴He/³He, ²²Ne/²¹Ne/²⁰Ne, ³⁶Ar/³⁸Ar, ¹³C/¹²C, ¹⁵N/¹⁴N, ¹⁸O/(¹⁷O)/¹⁶O, ¹³⁶Xe/¹³⁴Xe/¹³²Xe/¹³⁰Xe/¹²⁹Xe isotopic ratios will be measured by mass spectrometry on two probes entering the atmosphere of Saturn at two different locations near mid-latitudes, down to a pressure of 10 Bar. The global composition of Saturn will be investigated through these measurements, together with microwave radiometry determination of H₂O and NH₃ and their 3D variations. The dynamics of Saturn’s atmosphere will be investigated from: (1) measurements of pressure, temperature, vertical distribution of clouds and wind speed along the probes’ descent trajectories, and (2) determination of deep winds, differential rotation and convection with combined probe, gravity and radiometric measurements. Besides these primary goals, Kronos will also measure the intensities and characteristics of Saturn’s magnetic field inside the D ring as well as Saturn’s gravitational field, in order to constrain the abundance of heavy elements in Saturn’s interior and in its central core. Depending on the preferred architecture (flyby versus orbiter), Kronos will be in a position to measure the properties of Saturn’s innermost magnetosphere and to investigate the ring structure in order to understand how these tiny structures could have formed and survived up to the present times. An erratum to this article can be found at  相似文献   

What makes a planet habitable?     

H. Lammer  J. H. Bredehöft  A. Coustenis  M. L. Khodachenko  L. Kaltenegger  O. Grasset  D. Prieur  F. Raulin  P. Ehrenfreund  M. Yamauchi  J.-E. Wahlund  J.-M. Grießmeier  G. Stangl  C. S. Cockell  Yu. N. Kulikov  J. L. Grenfell  H. Rauer 《Astronomy and Astrophysics Review》2009,17(2):181-249

This work reviews factors which are important for the evolution of habitable Earth-like planets such as the effects of the host star dependent radiation and particle fluxes on the evolution of atmospheres and initial water inventories. We discuss the geodynamical and geophysical environments which are necessary for planets where plate tectonics remain active over geological time scales and for planets which evolve to one-plate planets. The discoveries of methane–ethane surface lakes on Saturn’s large moon Titan, subsurface water oceans or reservoirs inside the moons of Solar System gas giants such as Europa, Ganymede, Titan and Enceladus and more than 335 exoplanets, indicate that the classical definition of the habitable zone concept neglects more exotic habitats and may fail to be adequate for stars which are different from our Sun. A classification of four habitat types is proposed. Class I habitats represent bodies on which stellar and geophysical conditions allow Earth-analog planets to evolve so that complex multi-cellular life forms may originate. Class II habitats includes bodies on which life may evolve but due to stellar and geophysical conditions that are different from the class I habitats, the planets rather evolve toward Venus- or Mars-type worlds where complex life-forms may not develop. Class III habitats are planetary bodies where subsurface water oceans exist which interact directly with a silicate-rich core, while class IV habitats have liquid water layers between two ice layers, or liquids above ice. Furthermore, we discuss from the present viewpoint how life may have originated on early Earth, the possibilities that life may evolve on such Earth-like bodies and how future space missions may discover manifestations of extraterrestrial life.  相似文献