Sources and sinks of atmospheric methane   总被引：7，自引：0，他引：7  

D. H. Ehhalt  U. Schmidt 《Pure and Applied Geophysics》1978,116(2-3):452-464

In 1972 average mixing ratio of methane in the troposphere was 1.41 ppm and 1.3 ppmv for the northern and southern hemisphere, respectively, which corresponds to a total amount of 4×10¹⁵ g of CH₄ present in the atmosphere. Most is of recent biologic origin.¹⁴C analyses show that no more than 20 percent is released by fossil sources. The various ecosystems producing CH₄ are discussed and the total annual production is estimated to lie between 5.5×10¹⁴ g/yr and 11×10¹⁴ g/yr. The corresponding turnover times for atmospheric CH₄ range from 4 to 7 yrs. The destruction of CH₄ takes place mainly in the troposphere, most probably through the reaction of CH₄ + OH CH₃ + H₂O. About 10 percent of the CH₄ is destroyed in the stratosphere. The CH₄ cycle contributes on the order of 1 percent to the atmospheric carbon cycle.  相似文献   

TRAINING OF HYDROGEOLOGISTS FOR GROUND-WATER POLLUTION EVALUATIONS     

Kenneth D. Schmidt 《Ground water》1979,17(4):322-322

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The variation of the blocking temperature in models of thermoremanence (TRM)     

V.A. Schmidt 《Earth and Planetary Science Letters》1976,29(1):146-154

The simplest non-interactive forms of Néel's domain-reversal and wall-motion models are examined and the variations of their respective blocking temperatures as functions of applied field and coercivity are compared. Both models show remarkably similar blocking temperature behavior, but the remanence acquisition mechanisms are so different as to produce diametrically opposed results when the Lowrie-Fuller stability criterion is considered. In particular, in low fields the wall-motion model selectively activates high-coercivity fractions while the domain-reversal model favors the low coercivities. This results in the paradox that the wall-motion model predicts behavior experimentally associated with the single-domain and pseudo-single-domain size range while the domain-reversal model predicts behavior usually associated with the large multidomain range. The paradox can be partly resolved within the multidomain model alone, but this would not apply for the smallest grain sizes. Several alternative approaches to the problems of this size range are suggested.  相似文献   

Zur Reinigung organisch verschmutzter Abwässer im Stabilisierungsteichsystem Warnitz     

G. P. Schmidt  S. Schwarz 《洁净——土壤、空气、水》1976,4(4):345-351

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Early Mars volcanic sulfur storage in the upper cryosphere and formation of transient SO2‐rich atmospheres during the Hesperian          下载免费PDF全文

F. Schmidt  E. Chassefière  F. Tian  E. Dartois  J.‐M. Herri  O. Mousis 《Meteoritics & planetary science》2016,51(11):2226-2233

In a previous paper (Chassefière et al. 2013 ), we have shown that most volcanic sulfur released to the early Mars atmosphere could have been trapped in the upper cryosphere under the form of CO₂‐SO₂ clathrates. Huge amounts of sulfur, up to the equivalent of an ~1 bar atmosphere of SO₂, would have been stored in the Noachian upper cryosphere, then massively released to the atmosphere during the Hesperian due to rapidly decreasing CO₂ pressure. It could have resulted in the formation of the large sulfate deposits observed mainly in Hesperian terrains, whereas no or little sulfates are found at the Noachian. In the present paper, we first clarify some aspects of our previous work. We discuss the possibility of a smaller cooling effect of sulfur particles, or even of a net warming effect. We point out the fact that CO₂‐SO₂ clathrates formed through a progressive enrichment of a pre‐existing reservoir of CO₂ clathrates and discuss processes potentially involved in the slow formation of a SO₂‐rich upper cryosphere. We show that episodes of sudden destabilization at the Hesperian may generate 1000 ppmv of SO₂ in the atmosphere and contribute to maintaining the surface temperature above the water freezing point.  相似文献   

Editors' note: Astron. Nachr. 6/2010     

Wolfgang Schmidt  Rolf Schlichenmaier  Oskar von der Lühe 《Astronomische Nachrichten》2010,331(6):557-557

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Using DORIS measurements for modeling the vertical total electron content of the Earth’s ionosphere     

Denise Dettmering  Marco Limberger  Michael Schmidt 《Journal of Geodesy》2014,88(12):1131-1143

The Doppler orbitography and radiopositioning integrated by satellite (DORIS) system was originally developed for precise orbit determination of low Earth orbiting (LEO) satellites. Beyond that, it is highly qualified for modeling the distribution of electrons within the Earth’s ionosphere. It measures with two frequencies in L-band with a relative frequency ratio close to 5. Since the terrestrial ground beacons are distributed quite homogeneously and several LEOs are equipped with modern receivers, a good applicability for global vertical total electron content (VTEC) modeling can be expected. This paper investigates the capability of DORIS dual-frequency phase observations for deriving VTEC and the contribution of these data to global VTEC modeling. The DORIS preprocessing is performed similar to commonly used global navigation satellite systems (GNSS) preprocessing. However, the absolute DORIS VTEC level is taken from global ionospheric maps (GIM) provided by the International GNSS Service (IGS) as the DORIS data contain no absolute information. DORIS-derived VTEC values show good consistency with IGS GIMs with a RMS between 2 and 3 total electron content units (TECU) depending on solar activity which can be reduced to less than 2 TECU when using only observations with elevation angles higher than \(50^\circ \) . The combination of DORIS VTEC with data from other space-geodetic measurement techniques improves the accuracy of global VTEC models significantly. If DORIS VTEC data is used to update IGS GIMs, an improvement of up to 12  % can be achieved. The accuracy directly beneath the DORIS satellites’ ground-tracks ranges between 1.5 and 3.5 TECU assuming a precision of 2.5 TECU for altimeter-derived VTEC values which have been used for validation purposes.  相似文献   

Settling and compaction of chromite cumulates employing a centrifuging piston cylinder and application to layered mafic intrusions     

Shahrzad?ManoochehriEmail author  Max?W.?Schmidt 《Contributions to Mineralogy and Petrology》2014,168(6):1091

The time scales and mechanics of gravitationally driven crystal settling and compaction is investigated through high temperature (1,280–1,500 °C) centrifuge-assisted experiments on a chromite-basalt melt system at 100–1,500g (0.5 GPa). Subsequently, the feasibility of this process for the formation of dense chromite cumulate layers in large layered mafic intrusions (LMIs) is assessed. Centrifugation leads to a single cumulate layer formed at the gravitational bottom of the capsule. The experimentally observed mechanical settling velocity of a suspension of ~24 vol% chromite is calculated to be about half (~0.53) of the Stokes settling velocity, with a sedimentation exponent n of 2.35 (3). Gravitational settling leads to an orthocumulate layer with a porosity of 0.52 (all porosities as fraction). Formation times for such a layer from a magma with initial chromite contents of 0.1–1 vol% are 140–3.5 days, equal to a growth rate of 0.007–0.3 m/day for grain sizes of 1–2 mm. More compacted chromite layers form with increasing centrifugation time and acceleration through chemical compaction: An increase of grain contact areas and grain sizes together with a decrease in porosity is best explained by pressure dissolution at grain contacts, reprecipitation and grain growth into the intergranular space and a concomitant expulsion of intergranular melt. The relation between the porosity in the cumulate pile and effective pressure integrated over time (Δρ · h · a · t) is best fit with a logarithmic function, in fact confirming that a (pressure) dissolution–reprecipitation process is the dominant mechanism of compaction. The experimentally derived equation allows calculating compaction times: 70–80 % chromite at the bottom of a 1-m-thick chromite layer are reached after 9–250 years, whereas equivalent compaction times are 0.2–0.9 years for olivine (both for 2 mm grain size). The experiments allow to determine the bulk viscosities of chromite and olivine cumulates to be of magnitude 10⁹ Pa s, much lower than previously reported. As long as melt escape from the compacting cumulate remains homogeneous, fluidization does not play any role; however, channelized melt flow may lead to suspension and upward movement of cumulate crystals. In LMIs, chromitite layers are typically part of a sequence with layers of mafic minerals, compaction occurs under the additional weight of the overlying layers and can be achieved in a few years to decades.  相似文献   

Profiles of blue and infrared diffuse interstellar bands     

G. A. Galazutdinov  F. A. Musaev  M. R. Schmidt  J. Kre&#;owski 《Monthly notices of the Royal Astronomical Society》2001,323(2):293-300

The paper presents a survey of profiles of reasonably strong diffuse interstellar bands (DIBs) based on the extensive set of high-resolution spectra acquired with the aid of echelle spectrographs installed at the 2-m Terskol, 2-m Pic du Midi and 1-m SAO telescopes. The surveyed diffuse interstellar bands cover the spectral ranges of blue and near-infrared, i.e the DIBs not surveyed by Krełowski & Schmidt . The possible modifications caused by stellar and telluric lines are discussed. The very broad features such as 4430 are not discussed because the shapes of their profiles, extracted from echelle spectra, are very uncertain. The signal-to-noise (S/N) ratios of the spectra are not high enough to enable discussion of the profiles of numerous weak interstellar features discovered recently.  相似文献   

Determination of Phobos’ rotational parameters by an inertial frame bundle block adjustment     

Steffi Burmeister  Konrad Willner  Valentina Schmidt  Jürgen Oberst 《Journal of Geodesy》2018,92(9):963-973

A functional model for a bundle block adjustment in the inertial reference frame was developed, implemented and tested. This approach enables the determination of rotation parameters of planetary bodies on the basis of photogrammetric observations. Tests with a self-consistent synthetic data set showed that the implementation converges reliably toward the expected values of the introduced unknown parameters of the adjustment, e.g., spin pole orientation, and that it can cope with typical observational errors in the data. We applied the model to a data set of Phobos using images from the Mars Express and the Viking mission. With Phobos being in a locked rotation, we computed a forced libration amplitude of \(1.14^\circ \pm 0.03^\circ \) together with a control point network of 685 points.  相似文献