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1.
Light extinction by atmospheric particles is strongly dependent on their chemical composition and water content. Since light extinction directly impacts climate, optical measurements of atmospherically relevant aerosols at varying relative humidities (RH) are needed. Recent studies have highlighted the possibility that some atmospheric aerosols are glassy under ambient conditions. Here, the particle optical growth factor, fRHext, was measured for liquid and glassy particles using cavity ring-down aerosol extinction spectroscopy. The particles were composed of ammonium sulfate (AS), 1,2,6-hexanetriol, sucrose, raffinose, and mixed particles containing AS and either sucrose or raffinose. Both sucrose and raffinose can be glassy at room temperature. For the pure organics, the highly viscous sucrose and raffinose particles have similar optical growth curves to the liquid 1,2,6 hexanetriol particles. However, for particles composed of sucrose or raffinose mixed with AS, optical growth depends on the AS weight-percent, which in turn controls the phase state of the AS and ultimately the water uptake. 相似文献
2.
Share G.H. Murphy R.J. Dennis B.R. Schwartz R.A. Tolbert A.K. Lin R.P. Smith D.M. 《Solar physics》2002,210(1-2):357-372
The RHESSI high-resolution spectrometer detected γ-ray lines and continuum emitted by the Earth's atmosphere during impact
of solar energetic particles in the south polar region from 16:00–17:00 UT on 21 April 2002. The particle intensity at the
time of the observation was a factor of 10–100 weaker than previous events when gamma-rays were detected by other instruments.
This is the first high-resolution observation of atmospheric gamma-ray lines produced by solar energetic particles. De-excitation
lines were resolved that, in part, come from 14N at 728, 1635, 2313, 3890, and 5106 keV, and the 12C spallation product at ∼ 4439 keV. Other unresolved lines were also detected. We provide best-fit line energies and widths
and compare these with moderate resolution measurements by SMM of lines from an SEP event and with high-resolution measurements
made by HEAO 3 of lines excited by cosmic rays. We use line ratios to estimate the spectrum of solar energetic particles that
impacted the atmosphere. The 21 April spectrum was significantly harder than that measured by SMM during the 20 October 1989
shock event; it is comparable to that measured by Yohkoh on 15 July 2000. This is consistent with measurements of 10–50 MeV protons made in space at the time of the γ-ray observations. 相似文献
3.
Katherine?M.?PrimmEmail author Gregory?P.?Schill Daniel?P.?Veghte Miriam?Arak?Freedman Margaret?A.?Tolbert 《Journal of Atmospheric Chemistry》2017,74(1):55-69
Mineral dust particles are known to be efficient ice nuclei in the atmosphere. Previous work has probed heterogeneous ice nucleation on various laboratory dust samples including Arizona Test Dust, kaolinite, montmorillonite, and illite as atmospheric dust surrogates. However, it has recently been suggested that NX illite may be a better representation of atmospheric dust. Hiranuma et al. (2015) performed a laboratory comparison for immersion ice nucleation on NX illite, but here we focus on depositional ice nucleation because of its importance in low temperature cirrus cloud formation. A Raman microscope setup was used to examine the ice-nucleating efficiency of NX illite. Organic coatings on the NX illite particles were also investigated using a mixture of 5 dicarboxylic acids (M5). The ratio of NX illite to M5 was varied from 1:10 to 100:1. It was found that NX illite efficiently nucleates ice with Sice = 1.07 ± 0.01 at ?47 °C, with Sice slightly increasing at lower temperatures. In contrast, pure M5 is a poorer ice nucleus with Sice = 1.30 ± 0.02 at ?40 °C, relatively independent of temperature. Further, it was found that M5 coatings on the order of several monolayers thick hindered the ice nucleating ability of NX illite. Optical images suggest that at colder temperatures (< ?50 °C) 1:1 NX illite:M5 particles and pure M5 particles nucleate ice depositionally, while at warmer temperatures (> ?50 °C) subsaturated immersion ice nucleation dominates. These experiments suggest that mineral dust particles may become less active towards ice nucleation as they age in the atmosphere. 相似文献
4.
Recent detection of methane (CH4) on Mars has generated interest in possible biological or geological sources, but the factors responsible for the reported variability are not understood. Here we explore one potential sink that might affect the seasonal cycling of CH4 on Mars - trapping in ices deposited on the surface. Our apparatus consisted of a high-vacuum chamber in which three different Mars ice analogs (water, carbon dioxide, and carbon dioxide clathrate hydrates) were deposited in the presence of CH4 gas. The ices were monitored for spectroscopic evidence of CH4 trapping using transmission Fourier-Transform Infrared (FT-IR) spectroscopy, and during subsequent sublimation of the ice films the vapor composition was measured using mass spectrometry (MS). Trapping of CH4 in water ice was confirmed at deposition temperatures <100 K which is consistent with previous work, thus validating the experimental methods. However, no trapping of CH4 was observed in the ice analogs studied at warmer temperatures (140 K for H2O and CO2 clathrate, 90 K for CO2 snow) with approximately 10 mTorr CH4 in the chamber. From experimental detection limits these results provide an upper limit of 0.02 for the atmosphere/ice trapping ratio of CH4. If it is assumed that the trapping mechanism is linear with CH4 partial pressure and can be extrapolated to Mars, this upper limit would indicate that less than 1% is expected to be trapped from the largest reported CH4 plume, and therefore does not represent a significant sink for CH4. 相似文献
5.
Schwartz R.A. Csillaghy A. Tolbert A.K. Hurford G.J. Mc Tiernan J. Zarro D. 《Solar physics》2002,210(1-2):165-191
The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) performs imaging spectroscopy of the Sun with high spatial
and spectral resolution from 3 keV to 17 MeV using indirect Fourier-transform techniques. We review the rationale behind the
RHESSI data analysis software, and explain the underlying structure of the software tools. Our goal was to make the large
data set available within weeks after the RHESSI launch, and to make it possible for any member of the scientific community
to analyze it easily. This paper describes the requirements for the software and explores our decisions to use the SolarSoftWare
and Interactive Data Language programming packages, to support both Windows and Unix platforms, and to use object-oriented
programming. We also describe how the data are rapidly disseminated and how ancillary data sets are used to enhance the RHESSI
science. Finally, we give a schematic overview of some of the data flow through the high-level analysis tools. More information
on the data and analysis procedures can be found at the RHESSI Data Center website, http://hesperia.gsfc.nasa.gov/rhessidatacenter.
Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1022444531435 相似文献
6.
Gallagher Peter T. Dennis Brian R. Krucker Säm Schwartz Richard A. Tolbert A. Kimberley 《Solar physics》2002,210(1-2):341-356
Solar Physics - Observations of the X1.5 flare on 21 April 2002 are reviewed using the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and the Transition Region and Coronal Explorer... 相似文献
7.
Sui Linhui Holman Gordon D. Dennis Brian R. Krucker Säm Schwartz Richard A. Tolbert Kim 《Solar physics》2002,210(1-2):245-259
We have analyzed a C7.5 limb flare observed by RHESSI on 20 February 2002. The RHESSI images appear to show two footpoints
and a loop-top source. Our goal was to determine if the data are consistent with a simple steady-state model in which high-energy
electrons are continuously injected at the top of a semicircular flare loop. A comparison of the RHESSI images with simulated
images from the model has made it possible for us to identify spurious sources and fluxes in the RHESSI images. We find that
the RHESSI results are in many aspects consistent with the model if a thermal source is included between the loop footpoints,
but there is a problem with the spectral index of the loop-top source. The thermal source between the footpoints is likely
to be a low-lying loop interacting with the northern footpoint of a higher loop containing the loop-top source. 相似文献
8.
R.V. Gough J.J. Turley G.R. Ferrell K.E. Cordova S.E. Wood D.O. DeHaan C.P. McKay O.B. Toon M.A. Tolbert 《Planetary and Space Science》2011,59(2-3):238-246
It has been reported by several groups that methane in the Martian atmosphere is both spatially and temporally variable. Gough et al. (2010) suggested that temperature dependent, reversible physical adsorption of methane onto Martian soils could explain this variability. However, it is also useful to consider if there might be chemical destruction of methane (and compensating sources) operating on seasonal time scales. The lifetime of Martian methane due to known chemical loss processes is long (on the order of hundreds of years). However, observations constrain the lifetime to be 4 years or less, and general circulation models suggest methane destruction must occur even faster (<1 year) to cause the reported variability and rapid disappearance. The Martian surface is known to be highly oxidizing based on the Viking Labeled Release experiments in which organic compounds were quickly oxidized by samples of the regolith. Here we test if simulated Martian soil is also oxidizing towards methane to determine if this is a relevant loss pathway for Martian methane. We find that although two of the analog surfaces studied, TiO2·H2O2 and JSC-Mars-1 with H2O2, were able to oxidize the complex organic compounds (sugars and amino acids) used in the Viking Labeled Release experiments, these analogs were unable to oxidize methane to carbon dioxide within a 72 h experiment. Sodium and magnesium perchlorate, salts that were recently discovered at the Phoenix landing site and are potential strong oxidants, were not observed to directly oxidize either the organic solution or methane. The upper limit reaction coefficient, α, was found to be <4×10?17 for methane loss on TiO2·H2O2 and <2×10?17 for methane loss on JSC-Mars-1 with H2O2. Unless the depth of soil on Mars that contains H2O2 is very deep (thicker than 500 m), the lifetime of methane with respect to heterogeneous oxidation by H2O2 is probably greater than 4 years. Therefore, reaction of methane with H2O2 on Martian soils does not appear to be a significant methane sink, and would not destroy methane rapidly enough to cause the reported atmospheric methane variability. 相似文献
9.
It has been suggested that inclusions of CO2 or CO2 clathrate hydrates may comprise a portion of the polar deposits on Mars. Here we present results from an experimental study in which CO2 molecules were trapped in water ice deposited from CO2/H2O atmospheres at temperatures relevant for the polar regions of Mars. Fourier-Transform Infrared spectroscopy was used to monitor the phase of the condensed ice, and temperature programmed desorption was used to quantify the ratio of species in the generated ice films. Our results show that when H2O ice is deposited at 140-165 K, CO2 is trapped in large quantities, greater than expected based on lower temperature studies in amorphous ice. The trapping occurs at pressures well below the condensation point for pure CO2 ice, and therefore this mechanism may allow for CO2 deposition at the poles during warmer periods. The amount of trapped CO2 varied from 3% to 16% by mass at 160 K, depending on the substrate studied. Substrates studied were a tetrahydrofuran (C4H8O) base clathrate and Fe-montmorillonite clay, an analog for Mars soil. Experimental evidence indicates that the ice structures are likely CO2 clathrate hydrates. These results have implications for the CO2 content, overall composition, and density of the polar deposits on Mars. 相似文献
10.
Recent observations suggest methane in the martian atmosphere is variable on short spatial and temporal scales. However, to explain the variability by loss reactions requires production rates much larger than expected. Here, we report results of laboratory studies of methane adsorption onto JSC-Mars-1, a martian soil simulant, and suggest that this process could explain the observations. Uptake coefficient (γ) values were measured as a function of temperature using a high-vacuum Knudsen cell able to simulate martian temperature and pressure conditions. Values of γ were measured from 115 to 135 K, and the data were extrapolated to higher temperatures with more relevance to Mars. Adsorptive uptake was found to increase at lower temperatures and larger methane partial pressures. Although only sub-monolayer methane surface coverage is likely to exist under martian conditions, a very large mineral surface area is available for adsorption as atmospheric methane can diffuse meters into the regolith. As a result, significant methane may be temporarily lost to the regolith on a seasonal time scale. As this weak adsorption is fully reversible, methane will be re-released into the atmosphere when surface and subsurface temperatures rise and so no net loss of methane occurs. Heterogeneous interaction of methane with martian soil grains is the only process proposed thus far which contains both rapid methane loss and rapid methane production mechanisms and is thus fully consistent with the reported variability of methane on Mars. 相似文献