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1.
New measurements of the Herzberg I emission height profile in the night airglow are reported and indicate a peak emission height near 96 km in agreement with previous measurements. Using an atomic oxygen concentration profile determined from the oxygen green line profile measured on the same rocket it is concluded that the O2(A3Σu+) state is not excited in the direct three body recombination of atomic oxygen. It is suggested that the excitation mechanism is a two step process, similar to the Barth mechanism for the atomic oxygen green lineand that the excited intermediate state is C3Δu. 相似文献
2.
M. J. Jamieson M. Finch R. S. Friedman A. Dalgarno 《Planetary and Space Science》1992,40(12):1719-1721
Pectroscopic data on the shifts and widths of the energy levels of molecular oxygen have been used in the empirical construction of a diabatic potential matrix that characterizes the interactions of the B3∑−u state with the 5Πu, 23∑+u, 3Πu and 1Πu states. The diabatic potential matrix is u theory formulation to calculate the cross-sections for the excitation of O(1D) atoms in collisions of two O(3P) atoms. Total cross-sections are obtained by adding the excitation from the 3Πg, channel. The rate coefficient for quenching of O(1D) by O(3P) is evaluated as a function of temperature. The values conflict with a recent analysis of the emission of the oxygen red line in the upper atmosphere. 相似文献
3.
J. -C. Gerard 《Planetary and Space Science》1975,23(12):1681-1684
Measurements of the O2(A3Σ − X3Σ) Herzberg system in the night airglow have been made with the ESRO TD-1 satellite in the wavelength range 2400–3100 A. The slant emission rate varies from 3.5 to 15 kR, indicating an irregular structure of the atomic oxygen near the turbopause. A statistical maximum intensity is found near the tropic in the winter hemisphere. The intensity profile is consistent with excitation by three-body recombination of oxygen atoms. The observed total emission rate can be accounted for by reasonable atomic oxygen densities and an O2(A3Σ) production efficiency of about 20% if quenching by N2 occurs at the rate deduced from laboratory and other airglow measurements. 相似文献
4.
Absolute values of the emission cross sections for five vibrational bands in the Meinel system of N2+,A2πu to X2Σg+, excited by electron impact are presented. From these, a value was obtained for the total excitation cross section of the A2πu state at 100 eV of 26·5 × 10−18 cm2. The results are compared with those of other workers and with theory. Collisional transfer of the excitation energy from the levels of the A2πu state was also observed with a transfer cross section of approximately 10−14 cm2. 相似文献
5.
Recent rocket observations of the N2 V-K (Vegard-Kaplan) system in the aurora have been reinterpreted using an atmospheric model based on mass spectrometer measurements in an aurora of similar intensity at the same time of year. In contrast to the original interpretation, we find that population by cascade from the C3Πu and B3Πg states in the A3Σu+v=0,1 levels, as calculated using recently measured electron excitation cross sections, accurately accounts for the observed relative emission rates (IV-K/12PG0.0). In addition there is no need to change the production rate of A 3 Σ u+ molecules relative to that of C3Πuv=0 as a function of altitude in order to fit the profile of the deactivation probability to the atmospheric model. Quenching of A 3 Σ u+ molecules at high altitudes is dominated by atomic oxygen. The rate constants for the v=0 and v=1 levels are 8 × 10−11 cm3 sec−1 and 1.7 × 10−10 cm3 sec−1 respectively, as determined using the model atmosphere mentioned above. Recent observations with a helium cooled mass spectrometer suggest that conventional mass spectrometer measurements tend to underestimate the atomic oxygen relative concentration. The rate coefficients may therefore be too large by as much as a factor of 3. Below 130 Km we find that it is possible to account for the deactivation in bright auroras by invoking large nitric oxide concentrations, similar to those recently observed mass spectrometrically and using a rate constant of 8 × 10−11 cm3 sec−1 for both the v=1 levels. This rate constant is very nearly the same as that measured in the laboratory (7 × 10−11 cm3 sec−1). Molecular oxygen appears not to play a significant role in deactivating the lower A 3 Σ u+ levels. 相似文献
6.
Tom G. Slanger 《Planetary and Space Science》1983,31(12):1525-1528
Inspection of recent spectra presented by Sivjee (1983) show evidence of the 0–4 and 0–5 bands of the N2(c′41Σu+ → a1Πg) Gaydon-Herman system. In conjunction with earlier spectra, it is now possible that this band system is a significant auroral component, with an intensity approx. 7% that of the N2 2P system. The absence in aurorae of the potentially far stronger N2(c′41Σu+ → X1Πg) system is discussed. It is that the O2(A3Σu+ → X3Σg−) band system is indiscernible in Sivjee's auroral spectra, under conditio the foreground nightglow is expected to be clearly visible. On the other hand, at least one relatively strong O2(A′3Δu → a1Δg) band appears to be present in these spectra. 相似文献
7.
Rocket results are presented on the OI 6300 Å line and on the N2+ 3914 Å band in the dayglow. An altitude range of 78–335 km is covered. Theoretical interpretations are given, using results of simultaneous measurements of electron density and electron temperature. The apparent brightness of the 6300 Å line at the base of the emitting region is found to be 13 kR, of which 5.5 kR are ascribed to excitation through the Schumann-Runge dissociation of O2 by the solar UV radiations, 0.55 kR to the dissociative recombination of O2+ and NO+ ions, and 0.03 kR to the excitation of O by thermal electrons. An additional source of excitation above 280 km is suggested. The deactivation of O(1D) by O2(X3Σg−) is found to be appreciable below 200 km, and its rate coefficient is estimated to be 2 × 10−10 cm3/sec. The apparent brightness of the 3914 Å band at the base of the emitting region is found to be 6.5 kR, decreasing to 3.2 kR at 330 km. Assuming that fluorescent scattering of solar radiation is the mechanism involved the distribution of N2+ ions is calculated. The rate coefficients for the loss of these ions are hence calculated. 相似文献
8.
We analysed the emission spectra of solar prominences using the complete linearization method [5] and found simultaneously the optical depth at the line centre τ0, the doppler width of the line ΔλD and the damping width a. The results show 1) that the complete linearization method has a larger radius of convergence, 2) that we must consider the variation of the source function with depth, when determining τ0, and 3) that the calculated values of the damping constant for the H, Hβ of hydrogen and H and K lines of Calcium are all much greater than the theoretical values from doppler broadening and radiation damping, showing that other mechanisms besides these two also contribute to the broadening of prominence lines. 相似文献
9.
Charged boson stars and vacuum instabilities 总被引：1，自引：0，他引：1
We consider charged boson stars and study their effect on the structure of the vacuum. For very compact particle like “stars”, with constituent mass m* close to the Planck mass mPl, i.e. m2* = O(m2Pl), we argue that there is electric charge Zc, which, primarily, is due to the formation of a pion condensate (Zc 0.5−1e, where is the fine structure constant and e is the electric charge of the positron). If the charge of the “star” is larger than Zc we find numerical evidence for a complete screening indicating a limiting charge for a very compact object. There is also a less efficient competing charge screening mechanism due to spontaneous electron-positron pair creation in which case Zc −1e. Astrophysical and cosmological abundances of charged compact boson stars are briefly discussed in terms of dark matter. 相似文献
10.
We calculate the event rates induced by a 51Cr νe source and by a 90Sr---90Y
source in BOREXINO through elastic scattering on electrons, assuming a nonzero neutrino magnetic moment μν. We consider a source activity of about 2 MCi and estimate the solar ν (“source-off”) background for various oscillation scenarios. It is shown that values of μν as low as 0.5 × 10−10μB ( 0.2 × 10−10μB) can be proved with the 51Cr source (90Sr source) in about 100 days of data taking. 相似文献
11.
P. C. Wraight 《Planetary and Space Science》1977,25(12):1177-1181
Theoretical and experimental studies suggest that the recombination of atomic and molecular oxygen gives rise initially to ozone in the electronically excited state (11A2). Suggestions are made about the possible role of electronically excited ozone in stratospheric chemistry and in the nightglow. 相似文献
12.
Helioseismological sound-speed profiles severely constrain possible deviations from standard solar models, allowing us to derive new limits on anomalous solar energy losses by the Primakoff emission of axions. For an axion-photon coupling gay 5 × 10−10 GeV−1, the solar model is almost indistinguishable from the standard case, while gay 10 × 10−10 GeV−1 is probably excluded, corresponding to an axion luminosity of about 0.20 L. This constraint on gay is much weaker than the well-known globular-cluster limit, but about a factor of 3 more restrictive than previous solar limits. Our result is primarily of interest to the large number of current or proposed search experiments for solar axions because our limit defines the maximum gay for which it is self-consistent to use a standard solar model to calculate the axion luminosity. 相似文献
13.
Depending on such factors as (a) the probabilities of exciting the various vibrational states in ClO formed in the reaction of Cl with O3, (b) the radiative lifetime of ClO*, (c) ΔHƒ(ClO3), and (d) the rate coeffic`ient of the relevant three-body reaction, the production of ClO3 via the reaction ClO* +O2 +M→ClO3 +M may be quite substantial in the stratosphere. The significance of this result lies in the subsequent elimination (from the stratosphere) of ClO3 and its associated chlorine atom as HClO4, in the manner recently suggested by Samonaitis and Heicklen. In the stratosphere, ClO3 most probably photodissociates primarily into OClO and O. Upon photodissociation, OClO may also yield atomic oxygen. Thus the formation of ClO3 from ClO* and O2, and the above-mentioned photodissociation steps constitute an interesting, indirect mechanism of O2 dissociation into two odd oxygen species. Other aspects of ClO* chemistry, applicable in stratospheric conditions, also deserve attention in view of Nicholl's recent interpretation of the Umkehr measurements by Brewer et al. The reactions of ClO with HO2, and NO2, possess the potential of significantly obstructing the completion of the C1-ClO-Cl cycle, at least in the region below 35 km. An accurate and critical study of the chemistry of oxyacids, higher oxides, and nitrates of chlorine in the stratospheric environment is needed. Obviously, this is only a partial list of the difficult problems associated with a proper understanding of stratospheric chlorine chemistry which appears to be far more complex than what is implied in the literature. (See also notes added in proof stage.) 相似文献
14.
When the local solar zenith angle, χL, is < 105° the 6300 A line is much stronger than expected on the basis of F region ionic recombination alone. Between 95 and 105° the additional intensity is quantitatively explained by production of O(1D) from photolysis of O2 in the Schumann-Runge continuum, (λλ 1300–1750 A) using current values for solar flux, atmospheric composition and quenching of O(1D) by N2. The Schumann-Runge (SR) component exhibits a large seasonal variation with a maximum in summer. We interpret this variation as implying a seasonal change in thermospheric O2 abundance; the change seems largely to reflect a variation in O2 density at the base of the diffusive regime although some contribution may come from changes in thermospheric temperature structure. Large changes in the SR component exist from day to day and with a 27 day period following a major magnetic storm. The photodissociation source becomes inadequate when xl < 95°; at 90° more than half of the intensity comes from still another source which we identify as local photoelectron excitation of O atoms. 相似文献
15.
To study the climatological role of ozone in the Precambrian atmosphere and the consequences of its reduction for the ultraviolet environment of the early biosphere, a coupled one-dimensional radiative-convective and photochemical model has been developed. Oxygen levels between 10−5 and 1 time the present atmospheric level (PAL) are considered. It is shown that when the ice-albedo feedback is taken into account, relatively important temperature decreases are associated with the ozone changes linked to the progressive decrease of the oxygen level from 1 PAL to smaller values.
A similar study is performed for enhanced atmospheric CO2 pressures (Pco2). In these conditions, the ozone column is increased at low O2 concentrations with respect to the Pco2 = 1 PAL case. Consequently, the larger CO2 concentration in the ancient atmosphere could have contributed to strengthen the ultraviolet screening of ozone. The surface temperature response to the ozone decrease, as well as the thermal profiles are also analyzed in these CO2-rich models. A possible evolutionary scenario of atmospheric O2 and CO2 is discussed.
The consequences of these calculations for the ultraviolet environment of the primitive biosphere is discussed with a quantitative model calculating bacterial surviving rates. According to this model, the minimum ozone column being tolerable by unprotected bacteria would fall between 1 × 1018 and 4 × 1018 cm−2, depending on the bacterial species considered and corresponding to an O2 level somewhat lower than 10−2 PAL. For the coccoid blue-green alga Agmenellum quadruplicatum, this minimum ozone column would be of 4.5 × 1018, a value which is only slightly less than the presently observed column in the spring time ozone hole of Antarctica. 相似文献
16.
In the mesosphere, water vapor photolysis is the major source of odd hydrogen (H, OH and HO2) under normal conditions. The odd hydrogen produced may then be converted to H2 by the reaction H + HO2→ H2 + O2. This process is responsible for the calculated decrease in the H2O mixing ratio and accompanying increase in the H2 mixing ratio with altitude in the upper mesosphere and lower thermosphere. Charged particle precipitation events are calculated to produce the same effect, particularly in the 70–85 km region, thus temporarily resulting in enhanced conversion of H2O to H2 following such an event. Since odd hydrogen is produced predominantly by water vapor photolysis at these altitudes, decreased odd hydrogen concentrations are also anticipated. Odd hydrogen processes dominate ozone destruction in this region, and so an increase in ozone may occur if odd hydrogen concentrations decrease. We have examined the calculated time behavior of these processes in a numerical model using the August 1972 solar proton event as an example, and we present calculations indicating what might be observed in future events. 相似文献
17.
A general analysis of ionospheric conditions has been made in the light of possible ionic reactions occurring in the upper atmosphere. Data obtained on various parameters, such as ionic production and recombination, show that precise knowledge of the spectral distribution of solar radiation is needed and that other experimental determinations on dissociative recombinations are required.
The ionic complexity of the ionosphere is underlined by describing how the atomic ions O+ and N+ react with N2, O2 and NO molecules. The behavior of the molecular ions N+2, O+2and NO+depends on a group of simultaneous processes involving charge transfers and ionatom interchanges which are more important than dissociative recombinations. The altitude distribution of ions is exemplified by discussing the relative importance of various loss coefficients in the D-, E- and F-regions. It is seen that molecular nitrogen ions are subject to important charge transfer processes, that nitric oxide ions are always final products destroyed only by dissociative recombination. Additionally, the entire production of atomic oxygen ions is related to the photoionization of molecular nitrogen. Some information is also given on possible anomalies in the ratio of O+2 and NO+ densities in the lower ionosphere. From the lack of sufficient experimental information on ionic processes it is shown that a precise analysis of ionospheric behavior remains highly speculative. 相似文献
18.
R.Earl Good 《Planetary and Space Science》1976,24(4):389-395
A rocket experiment was conducted which measured the infrared bands of the excited hydroxyl radical in the night airglow. The OH emission was found in a layer centered at 87 km having a half-width of 6 km and a total emission of 1.1 MR. The atomic oxygen altitude profile, ranging from 1.3 × 1010 atoms/cm3 at 83 km to 3 × 1011 atoms/cm3 at 90 km is determined from the hydroxyl airglow measurements. This derivation is based on the steady state balance between ozone formation from atomic oxygen and its destruction by hydrogen which produces the OH infrared emission. 相似文献
19.
J.E. Frederick 《Planetary and Space Science》1979,27(12):1469-1477
The wind and temperature oscillations of internal gravity waves can cause horizontal variations of a factor of two in minor gas number densities in the lower thermosphere over length scales of several hundred kilometers. The variations are due both to vertical transport of constituents whose lifetimes are long compared to the wave period and to chemical activity driven by temperature dependent reaction rate coefficients. The nightglow emission of the hydroxyl radical provides a remote sensor of wave activity between 80 and 90 km. Theoretical calculations show that the horizontal variations in the atomic hydrogen distribution are the largest single contributor to wave structure in the nightglow followed by the effects of temperature fluctuations on the rate coefficient of the reaction H + O3 → O2 + OHv′ > 0). 相似文献
20.
We discuss the altitude and intensity of the nocturnal green line emission resulting from O2+ recombination. The Doppler profile of this emission is markedly non-thermal, the width being characteristic of the energy at which the O(1S) atoms are produced. A simple theory is formulated which predicts the profile of this line. Experimental evidence on airglow line profiles is reviewed and it is found that the effect predicted here has not yet been observed. However a deliberate search for this effect should yield immediate results. 相似文献