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1.
The composition of planetesimals depends upon the epoch and the location of their formation in the solar nebula. Meteorites
produced in the hot inner nebula contain refractory compounds. Volatiles were present in icy planetesimals and cometesimals
produced in the cold outer nebula. However, the mechanism responsible for their trapping is still controversial. We argue
for a general scenario valid in all regions of the turbulent nebula where water condensed as a crystalline ice (Hersant et al., 2004). Volatiles were trapped in the form of clathrate hydrates in the continuously cooling nebula. The epoch of clathration
of a given species depends upon the temperature and the pressure required for the stability of the clathrate hydrate. The
efficiency of the mechanism depends upon the local amount of ice available. This scenario is the only one so far which proposes
a quantitative interpretation of the non detection of N2 in several comets of the Oort cloud (Iro et al., 2003). It may explain the large variation of the CO abundance observed in comets and predicts an Ar/O ratio much less than
the upper limit of 0.1 times the solar ratio estimated on C/2001 A2 (Weaver et al., 2002). Under the assumption that the amount of water ice present at 5 AU was higher than the value corresponding to the
solar O/H ratio by a factor 2.2 at least, the clathration scenario reproduces the quasi uniform enrichment with respect to
solar of the Ar, Kr, Xe, C, N and S elements measured in Jupiter by the Galileo probe. The interpretation of the non-uniform
enrichment in C, N and S in Saturn requires that ice was less abundant at 10 AU than at 5 AU so that CO and N2 were not clathrated in the feeding zone of the planet while CH4, NH3 and H2S were. As a result, the 14N/15N ratio in Saturn should be intermediate between that in Jupiter and the terrestrial ratio.
Ar and Kr should be solar while Xe should be enriched by a factor 17. The enrichments in C, N and S in Uranus and Neptune
suggest that available ice was able to form clathrates of CH4, CO and the NH3 hydrate, but not the clathrate of N2. The enrichment of oxygen by a factor 440 in Neptune inferred by Lodders and Fegley (1994) from the detection of CO in the
troposphere of the planet is higher by at least a factor 2.5 than the lower limit of O/H required for the clathration of CO
and CH4 and for the hydration of NH3. If CO detected by Encrenaz et al. (2004) in Uranus originates from the interior of the planet, the O/H ratio in the envelope must be around of order of 260
times the solar ratio, then also consistent with the trapping of detected volatiles by clathration. It is predicted that Ar
and Kr are solar in the two planets while Xe would be enriched by a factor 30 to 70. Observational tests of the validity of
the clathration scenario are proposed. 相似文献
2.
This paper reviews the chemical processes responsible for fractionating deuterium in interstellar molecules. I show that this
process is intrinsically a low temperature phenomenon and discuss how the degree of enhancement of the deuterium content of
molecules is related to the physical conditions, particularly abundances, in molecular clouds. If significant amounts of abundant
species, such as CO, are frozen out on to interstellar dust grains, the resulting enhancement in H2D+ can result in its abundance being greater than that of H
3
+
at 10K. Transfer of the deuteron from H2D+ can then lead to the efficient formation of multiply deuterated species, such as NHD2 and ND3. Fractionation can also occur in grain surface reactions and some simple models are discussed.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
3.
T. Cassidy P. Coll F. Raulin R. W. Carlson R. E. Johnson M. J. Loeffler K. P. Hand R. A. Baragiola 《Space Science Reviews》2010,153(1-4):299-315
The transport and exchange of material between bodies in the outer solar system is often facilitated by their exposure to ionizing radiation. With this in mind we review the effects of energetic ions, electrons and UV photons on materials present in the outer solar system. We consider radiolysis, photolysis, and sputtering of low temperature solids. Radiolysis and photolysis are the chemistry that follows the bond breaking and ionization produced by incident radiation, producing, e.g., O2 and H2 from irradiated H2O ice. Sputtering is the ejection of molecules by incident radiation. Both processes are particularly effective on ices in the outer solar system. Materials reviewed include H2O ice, sulfur-containing compounds (such as SO2 and S8), carbon-containing compounds (such as CH4), nitrogen-containing compounds (such as NH3 and N2), and mixtures of those compounds. We also review the effects of ionizing radiation on a mixture of N2 and CH4 gases, as appropriate to Titan’s upper atmosphere, where radiolysis and photolysis produce complex organic compounds (tholins). 相似文献
4.
Thérèse Encrenaz 《Space Science Reviews》2008,135(1-4):11-23
Most of our knowledge regarding planetary atmospheric composition and structure has been achieved by remote sensing spectroscopy. Planetary spectra strongly differ from one planet to another. CO2 signatures dominate on Mars, and even more on Venus (where the thermal component is detectable down to 1 μm on the dark side). Spectroscopic monitoring of Venus, Earth and Mars allows us to map temperature fields, wind fields, clouds, aerosols, surface mineralogy (in the case of the Earth and Mars), and to study the planets’ seasonal cycles. Spectra of giant planets are dominated by H2, CH4 and other hydrocarbons, NH3, PH3 and traces of other minor compounds like CO, H2O and CO2. Measurements of the atmospheric composition of giant planets have been used to constrain their formation scenario. 相似文献
5.
Surface temperature and the available effective energy strongly influence the mass flux of H2O and minor volatiles from the nucleus. We perform computer simulations to model the gas flux from volatile, icy components
in porous ice-dust surfaces, in order to better understand results from observations of comets. Our model assumes a porous
body containing dust, one major ice component (H2O) and up to eight minor components of higher volatility (e.g. CO, CH4, CH3OH, HCN, C2H2, H2S), The body's porous structure is modeled as a bundle of tubes with a given tortuosity and an initially constant pore diameter.
Heat is conducted by the matrix and carried by the vapors. The model includes radially inward and outward flowing vapor within
the body, escape of outward flowing gas from the body, complete depletion of less volatile ices in outer layers, and recondensation
of vapor in deeper, cooler layers. From the calculations we obtain temperature profiles and changes in relative chemical abundances,
porosity and pore size distribution as a function of depth, and the gas flux into the interior and into the atmosphere for
each of the volatiles at various positions of the body in its orbit.
In this paper we relate the observed relative molecular abundances in the coma of Comet C/1995 O1 (Hale-Bopp) and of Comet
46P/Wirtanen to molecular fluxes at the surface calculated from our model.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
6.
The ISO-SWS instrument offering a large wavelength coverage and a resolution well adapted to the solid phase has changed our
knowledge of the physical-chemical properties of ices in space. The discovery of many new ice features was reported and the
comparison with dedicated laboratory experiments allowed the determination of more accurate abundances of major ice components.
The presence of CO2 ice has recently been confirmed with the SWS (Short Wavelength Spectrometer) as a dominant ice component of interstellar
grain mantles. The bending mode of CO2 ice shows a particular triple-peak structure which provides first evidence for extensive ice segregation in the line-of-sight
toward massive protostars. A comparison of interstellar and cometary ices using recent ISO data and ground-based measurements
has revealed important similarities but also indicated that comets contain, beside pristine interstellar material, admixtures
of processed material. The investigation of molecules in interstellar clouds is essential to reveal the link between dust
in the interstellar medium and in the Solar System.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
7.
Emmanuel Dartois 《Space Science Reviews》2005,119(1-4):293-310
The instruments on board the Infrared Space Observatory have for the first time allowed a complete low (PHOT, CVF) to medium
resolution (SWS) spectroscopic harvest, from 2.5 to 45 μm, of interstellar dust. Amongst the detected solids present in starless
molecular clouds surrounding recently born stellar and still embedded objects or products of the chemistry in some mass loss
envelopes, the so-called “ice mantles” are of specific interest. They represent an interface between the very refractory carbonaceous
and silicates materials that built the first grains with the rich chemistry taking place in the gas phase. Molecules condense,
react on ices, are subjected to UV and cosmic ray irradiation at low temperatures, participating efficiently to the evolution
toward more complex molecules, being in constant interaction in an ice layer. They also play an important role in the radiative
transfer of molecular clouds and strongly affect the gas phase chemistry. ISO results shed light on many other species than
H2O ice. The detection of these van der Waal's solids is mainly performed in absorption. Each ice feature observed by ISO spectrometer
is an important species, with abundance in the 10−4–10−7 range with respect to H2. Such high abundances represent a substantial reservoir of matter that, once released later on, replenishes the gas phase
and feeds the ladder of molecular complexity. Medium resolution spectroscopy also offers the opportunity to look at individual
line profiles of the ice features, and therefore to progressively reveal the interactions taking place in the mantles.
This article will give a view on selected results to avoid to overlap with the numerous reviews the reader is invited to consult
(e.g. van Dishoeck, in press; Gibb et al., 2004.).
Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries:
France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA. 相似文献
8.
V. Wakelam I. W. M. Smith E. Herbst J. Troe W. Geppert H. Linnartz K. Öberg E. Roueff M. Agúndez P. Pernot H. M. Cuppen J. C. Loison D. Talbi 《Space Science Reviews》2010,156(1-4):13-72
We survey the current situation regarding chemical modelling of the synthesis of molecules in the interstellar medium. The present state of knowledge concerning the rate coefficients and their uncertainties for the major gas-phase processes—ion-neutral reactions, neutral-neutral reactions, radiative association, and dissociative recombination—is reviewed. Emphasis is placed on those key reactions that have been identified, by sensitivity analyses, as ‘crucial’ in determining the predicted abundances of the species observed in the interstellar medium. These sensitivity analyses have been carried out for gas-phase models of three representative, molecule-rich, astronomical sources: the cold dense molecular clouds TMC-1 and L134N, and the expanding circumstellar envelope IRC +10216. Our review has led to the proposal of new values and uncertainties for the rate coefficients of many of the key reactions. The impact of these new data on the predicted abundances in TMC-1 and L134N is reported. Interstellar dust particles also influence the observed abundances of molecules in the interstellar medium. Their role is included in gas-grain, as distinct from gas-phase only, models. We review the methods for incorporating both accretion onto, and reactions on, the surfaces of grains in such models, as well as describing some recent experimental efforts to simulate and examine relevant processes in the laboratory. These efforts include experiments on the surface-catalyzed recombination of hydrogen atoms, on chemical processing on and in the ices that are known to exist on the surface of interstellar grains, and on desorption processes, which may enable species formed on grains to return to the gas-phase. 相似文献
9.
MIRO: Microwave Instrument for Rosetta Orbiter 总被引:1,自引:0,他引:1
S. Gulkis M. Frerking J. Crovisier G. Beaudin P. Hartogh P. Encrenaz T. Koch C. Kahn Y. Salinas R. Nowicki R. Irigoyen M. Janssen P. Stek M. Hofstadter M. Allen C. Backus L. Kamp C. Jarchow E. Steinmetz A. Deschamps J. Krieg M. Gheudin D. Bockelée-Morvan N. Biver T. Encrenaz D. Despois W. Ip E. Lellouch I. Mann D. Muhleman H. Rauer P. Schloerb T. Spilker 《Space Science Reviews》2007,128(1-4):561-597
The European Space Agency Rosetta Spacecraft, launched on March 2, 2004 toward Comet 67P/Churyumov-Gerasimenko, carries a
relatively small and lightweight millimeter-submillimeter spectrometer instrument, the first of its kind launched into deep
space. The instrument will be used to study the evolution of outgassing water and other molecules from the target comet as
a function of heliocentric distance. During flybys of the asteroids (2867) Steins and (21) Lutetia in 2008 and 2010 respectively,
the instrument will measure thermal emission and search for water vapor in the vicinity of these asteroids.
The instrument, named MIRO (Microwave Instrument for the Rosetta Orbiter), consists of a 30-cm diameter, offset parabolic
reflector telescope followed by two heterodyne receivers. Center-band operating frequencies of the receivers are near 190
GHz (1.6 mm) and 562 GHz (0.5 mm). Broadband continuum channels are implemented in both frequency bands for the measurement
of near surface temperatures and temperature gradients in Comet 67P/Churyumov-Gerasimenko and the asteroids (2867) Steins
and (21) Lutetia. A 4096 channel CTS (Chirp Transform Spectrometer) spectrometer having 180 MHz total bandwidth and 44 kHz
resolution is, in addition to the continuum channel, connected to the submillimeter receiver. The submillimeter radiometer/spectrometer
is fixed tuned to measure four volatile species – CO, CH3OH, NH3 and three, oxygen-related isotopologues of water, H2
16O, H2
17O and H2
18O. The basic quantities measured with the MIRO instrument are surface temperature, gas production rates and relative abundances,
and velocity and excitation temperature of each species, along with their spatial and temporal variability. This paper provides
a short discussion of the scientific objectives of the investigation, and a detailed discussion of the MIRO instrument system. 相似文献
10.
The measured D/H ratios in interstellar environments and in the solar system are reviewed. The two extreme D/H ratios in solar
system water - (720±120)×10−6 in clay minerals and (88±11)×10−6 in chondrules, both from LL3 chondritic meteorites - are interpreted as the result of a progressive isotopic exchange in
the solar nebula between deuterium-rich interstellar water and protosolar H2. According to a turbulent model describing the evolution of the nebula (Drouart et al., 1999), water in the solar system cannot be a product of thermal (neutral) reactions occurring in the solar nebula. Taking
720×10−6 as a face value for the isotopic composition of the interstellar water that predates the formation of the solar nebula, numerical
simulations show that the water D/H ratio decreases via an isotopic exchange with H2. During the course of this process, a D/H gradient was established in the nebula. This gradient was smoothed with time and
the isotopic homogenization of the solar nebula was completed in 106 years, reaching a D/H ratio of 88×10−6. In this model, cometary water should have also suffered a partial isotopic re-equilibration with H2. The isotopic heterogeneity observed in chondrites result from the turbulent mixing of grains, condensed at different epochs
and locations in the solar nebula. Recent isotopic determinations of water ice in cold interstellar clouds are in agreement
with these chondritic data and their interpretation (Texeira et al., 1999).
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
11.
Spectroscopy Between the Stars 总被引:1,自引:0,他引:1
The emission and absorption spectra of interstellar molecules are reviewed with special consideration of recent observational
and technical advances in the shorter submillimeter wave region of the electromagnetic spectrum. Single-dish observations
have contributed in the past probably most of the information about the structure of interstellar molecular clouds.
At present about 120 interstellar molecules have been identified in interstellar clouds and circumstellar envelopes, evidence
of a rich and diversified chemistry. CO, the most abundant interstellar molecule and other diatomic molecules and radicals
are found throughout molecular clouds, whereas the more complex molecules are found in high-density cores, which are often
the sites of active star formation. These locations represent prime targets for the search for larger molecules, such as glycine.
The ignition of young stars is accompanied by strong heating of the surrounding material by radiation and/or shocks, leading
to photoevaporation of molecules depleted on dust grains driving a "hot core" chemistry, traceable by its rich organic chemistry
and its prevailing high excitation conditions (up to about 2000 cm-1).
However, in the list of detected interstellar molecules many simple hydrides are still missing, e.g. SH, PH, PH2, etc., which constitute the building blocks for larger molecules. With the technological opening of the terahertz region
(ν ∼1 THz corresponds to λ ∼0.3 mm) to both laboratory and interstellar spectroscopy, great scientific advances are to be
expected. Amongst these will be the direct detection of the lowest rotational transitions of the light hydrides, the low energy
bending vibrations of larger (linear) molecules, and possibly the ring-puckering motion of larger ring molecules such as the
polycyclic (multiring) aromatic hydrocarbons.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
12.
The Neutral Mass Spectrometer on the Giotto spacecraft established that H2O is the dominant species in Comet Halley's volatiles and determined the abundance of more than 10 parent species. The instrument
discovered strong extended H2CO and CO sources in the coma of Comet Halley. Polymerized H2CO associated with the cometary dust and evaporating slowly as the monomer is most likely the extended H2CO source. Photodissociation of the H2CO into CO fully accounts for the extended CO source.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
13.
We have searched for rare molecules and radicals in the coma of P/Halley using the ion data obtained by IMS-Giotto. Whereas
our established methods were used in the ionosphere, a new model was developed for the interpretation of the ion data in the
outer coma. Ne/H2O < 1.5 × 10-3 was determined in the coma of the comet. Upper limits for the production of Na were derived from the very low abundance of
Na+. Methyl cyanide and (probably) ethyl cyanide were identified with abundances of CH3CN/H2O = (1.4 ± .6) × 10-3 and C2H5CN/H2O = (2.8 ± 1.6) × 10-4. These results and upper limits for other N-bearing species confirm that nitrogen is depleted in the Halley material. C4H was identified and a point source strength of C4H/H2O = (2.3 ± .8) × 10-3 was derived. Our upper limit for C3H is lower than the abundance of C4H. This is in agreement with the enhanced abundances of CnH species with even numbers of C-atoms found in interstellar molecular clouds, suggesting that the C4H in Halley was synthesized under molecular cloud conditions. Thus, C4H and other organics with unpaired electrons may turn out to be indicators for a molecular cloud origin of cometary constituents.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
14.
The gas flux from a volatile icy-dust mixture is computed using a comet nucleus thermal model in order to study the evolution
of CO outgassing during several apparitions from long-period Comet Hale-Bopp and short-period Comet Wirtanen. The comet model
assumes a spherical, porous body containing a dust component, one major ice component (H2O), and one minor ice component of higher volatility (CO). The initial chemical composition is assumed to be homogeneous.
The following processes are taken into account: heat and gas diffusion inside the rotating nucleus; release of outward diffusing
gas from the comet nucleus; chemical differentiation by sublimation of volatile ices in the surface layers and recondensation
of gas in deeper, cooler layers. A 2-D time dependent solution is obtained through the dependence of the boundary conditions
on the local solar illumination as the nucleus rotates. The model for Comet Hale-Bopp was compared with observational measurements
(Biver et al., 1999). The best agreement was obtained for a model with amorphous water ice and CO, assuming that a part of the latter is
trapped by the water ice, another part is condensed as an independent ice phase. The model confirms that sublimation of CO
ice at large heliocentric distance produces a gradual increase in the comet's activity as it approaches the Sun. Crystallization
of amorphous water ice begins at 7 AU from the Sun, but no outbursts were found. Seasonal effects and thermal inertia of the
nucleus material lead to larger CO outgassing rates as the comet recedes from the Sun. In the second part of this work the
model was run with the orbital parameters of Comet Wirtanen. Unlike Comet Hale-Bopp, the predicted CO outgassing from Comet
Wirtanen is almost constant throughout its orbit. Such behavior can be explained by a thermally evolved and chemically differentiated
comet nucleus.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
15.
W. B. Durham O. Prieto-Ballesteros D. L. Goldsby J. S. Kargel 《Space Science Reviews》2010,153(1-4):273-298
Laboratory measurements of physical properties of planetary ices generate information for dynamical models of tectonically active icy bodies in the outer solar system. We review the methods for measuring both flow properties and thermal properties of icy planetary materials in the laboratory, and describe physical theories that are essential for intelligent extrapolation of data from laboratory to planetary conditions. This review is structured with a separate and independent section for each of the two sets of physical properties, rheological and thermal. The rheological behaviors of planetary ices are as diverse as the icy moons themselves. High-pressure water ice phases show respective viscosities that vary over four orders of magnitude. Ices of CO2, NH3, as well as clathrate hydrates of CH4 and other gases vary in viscosity by nearly ten orders of magnitude. Heat capacity and thermal conductivity of detected/inferred compositions in outer solar system bodies have been revised. Some low-temperature phases of minerals and condensates have a deviant thermal behavior related to paramount water ice. Hydrated salts have low values of thermal conductivity and an inverse dependence of conductivity on temperature, similar to clathrate hydrates or glassy solids. This striking behavior may suit the dynamics of icy satellites. 相似文献
16.
《中国航空学报》2021,34(12):17-27
Ammonia (NH3) is considered as a potential alternative carbon free fuel to reduce greenhouse gas emission to meet the increasingly stringent emission requirements. Co-burning NH3 and H2 is an effective way to overcome ammonia’s relative low burning velocity. In this work, 3D Reynolds Averaged Navier-Stokes (RANS) numerical simulations are conducted on a premixed NH3/H2 swirling flame with reduced chemical kinetic mechanism. The effects of (A) overall equivalence ratio Φ and (B) hydrogen blended molar fraction XH2 on combustion and emission characteristics are examined. The present results show that when 100%NH3-0%H2-air are burnt, the NO emission and unburned NH3 of at the swirling combustor outlet has the opposite varying trends. With the increase of Φ, NO emission is found to be decreased, while the unburnt ammonia emission is increased. NH2 → HNO, NH → HNO and HNO → NO sub-paths are found to play a critical role in NO formation. Normalized reaction rate of all these three sub-paths is shown to be decreased with increased Φ. Hydrogen addition is shown to significantly increase the laminar burning velocity of the mixed fuel. However, adding H2 does not affect the critical equivalence ratio corresponding to the maximum burning velocity. The emission trend of NO and unburnt NH3 with increased Φ is unchanged by blending H2. NO emission with increased XH2 is increased slightly less at a larger Φ than that at a smaller Φ. In addition, reaction rates of NH2 → HNO and HNO → NO sub-paths are decreased with increased XH2, when Φ is larger. Under all tested cases, blending H2 with NH3 reduces the unburned NH3 emission, especially for rich combustion conditions. In summary, the present work provides research finding on supporting applying ammonia with hydrogen blended in low-emission gas turbine engines. 相似文献
17.
Infrared spectroscopic observations of planets and Saturn's satellite Titan with the Infrared Space Observatory led to many
significant discoveries that improved our understanding on the formation, physics and chemistry of these objects. The prime
results achieved by ISO are: (1) a new and consistent determination of the D/H ratios on the giant planets and Titan; (2)
the first precise measurement of the 15N/14N ratio in Jupiter, a valuable indicator of the protosolar nitrogen isotopic ratio; (3) the first detection of an external
oxygen flux for all giant planets and Titan; (4) the first detection of some stratospheric hydrocarbons (CH3, C2H4, CH3C2H, C4H2, C6H6); (5) the first detection of tropospheric water in Saturn; (6) the tentative detection of carbonate minerals on Mars; (7)
the first thermal lightcurve of Pluto.
Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries:
France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA. 相似文献
18.
Until pristine samples can be returned from cometary nuclei, primitive meteorites represent our best source of information
about organic chemistry in the early solar system. However, this material has been affected by secondary processing on asteroidal
parent bodies which probably did not affect the material now present in cometary nuclei. Production of meteoritic organic
matter apparently involved the following sequence of events: Molecule formation by a variety of reaction pathways in dense
interstellar clouds; Condensation of those molecules onto refractory interstellar grains; Irradiation of organic-rich interstellar-grain
mantles producing a range of molecular fragments and free radicals; Inclusion of those interstellar grains into the protosolar
nebula with probable heating of at least some grain mantles during passage through the shock wave bounding the solar accretion
disc; Agglomeration of residual interstellar grains and locally produced nebular condensates into asteroid-sized planetesimals;
Heating of planetesimals by decay of extinct radionuclides; Melting of ice to produce liquid water within asteroidal bodies;
Reaction of interstellar molecules, fragments and radicals with each other and with the aqueous environment, possibly catalysed
by mineral grains; Loss of water and other volatiles to space yielding a partially hydrated lithology containing a complex
suite of organic molecules; Heating of some of this organic matter to generate a kerogen-like complex; Mixing of heated and
unheated material to yield the meteoritic material now observed. Properties of meteoritic organic matter believed to be consistent
with this scenario include: Systematic decrease of abundance with increasing C number in homologous series of characterisable
molecules; Complete structural diversity within homologous series; Predominance of branched-chain isomers; Considerable isotopic
variability among characterisable molecules and within kerogen-like material; Substantial deuterium enrichment in all organic
fractions; Some fractions significantly enriched in nitrogen-15; Modest excesses of L-enantiomers in some racemisation-resistant
molecules but no general enantiomeric preference. Despite much speculation about the possible role of Fischer-Tropsch catalytic
hydrogenation of CO in production of organic molecules in the solar nebula, no convincing evidence for such material has been
found in meteorites. A similarity between some meteoritic organics and those produced by Miller-Urey discharge synthesis may
reflect involvement of common intermediates rather than the operation of electric discharges in the early solar system. Meteoritic
organic matter constitutes a useful, but not exact, guide to what we shall find with in situ analytical and sample-return
missions to cometary nuclei.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
19.
20.
乙醇燃烧加热空气污染物对煤油超燃的影响 总被引:1,自引:0,他引:1
在燃烧室入口来流马赫数为2.5的条件下,研究乙醇燃烧加热空气污染物对煤油超声速燃烧的影响.在加热器中,采用预混稳态燃烧火焰模型和61组分388步详细反应机理模拟乙醇燃烧加热过程,获得与实验温度条件相同的详细污染出口组分组成.其主要污染空气作为煤油超声速燃烧室的入口组分,采用17组分30步反应机理模拟煤油超声速燃烧过程,研究了污染物组分对煤油超燃室性能的影响.通过化学动力学和热力学分析,对比了地面电加热、乙醇燃烧加热和25km高空三种工况.结果表明:由于自由基作用以及平 均分子质量的减小和平均比定压热容的增加,乙醇燃烧加热污染空气造成超燃室的燃烧效率和内推力均上升. 相似文献