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1.
The Narmada-Son lineament (NSL) forms a major tectonic feature on the Indian subcontinent. The importance of this lineament lies in its evolution as well as its tectonic history. The lineament seems to have been active since Precambrian times. In order to understand the history of its evolution, it is necessary to know what igenous activity has been taking place along this lineament, and how the Deccan trap volcanics, which cover large areas along this lineament, have erupted.For the study of this problem an analysis of the aeromagnetic anomaly map lying between 76°15 to 77°30E and 21°45 to 22°50N has been carried out. Four different profiles (B 1 B 1,B 2 B 2,B 3 B 3 andB 4 B 4) have been drawn in N-S direction over this area and interpreted in terms of the intrusive bodies present within or below the surface of Deccan trap exposures. Inversion and forward modelling techniques have been adopted for interpretation purposes. An analysis of frequency spectra along the profiles has also been carried out to estimate the average depth of the different magnetic bodies. These results have been correlated with the available geological information. It has been found that most of the small wavelength anomalies are caused by dyke-like bodies within or below the Deccan trap at a depth of less than 0.5 km.  相似文献   

2.
Summary The derivatives of the harmonicsP n (k) (sin O)cos kTO andP n (k) (sin O)sin kTO, occurring in the development of the lunar disturbing potential, are derived upto n=4 and for k== 0, 1, ..., n. The equatorial co-ordinates OTO are referred to the Moon's mass centre; the procedure for the solar disturbing potential is formally identical.  相似文献   

3.
Summary Speeded-up magnetic tape recordings of earthquake signals can be analyzed by means of an electronic sound spectrograph. The time-dependent spectrum of body waves obtained through transient analysis provides some insight into the physical properties of the earth's interior. In the short-period arrivals traveling through the outer core and inner core dispersion has been observed. A group velocity maximum has been found forP at periods between 1 and 2 seconds. The direct rayPand the surface reflected phasePP convey more energy than the arrivalsP 2 andPcPP which, firstly, enter the outer core at incidence far from vertical, and secondly spend more time in the outer part of the fluid core.
Zusammenfassung Magnetbandaufzeichnungen von Erdbebensignalen können, mit vervielfachter Geschwindigkeit wiedergegeben, mittels eines elektronischen Schallspektrographen analysiert werden. Das zeitabhängige Raumwellenspektrum, das man aus einer solchen Analyse nichtstationärer Vorgänge erhält, gibt einen gewissen Einblick in die physikalischen Eigenschaften des Erdinnern. So wurde im kurzperiodischen Anteil der Raumwellen, die durch den äusseren und inneren Erdkern gelaufen sind, Dispersion beobachtet. BeiP wurde im Periodenbereich zwischen 1 und 2 Sekunden ein Gruppengeschwindigkeitsmaximum gefunden. Der direkte StrahlP und die einmal an der Erdoberfläche reflektiertePP-Welle transportieren mehr Energie als die WellenphasenP 2 undPcPP, die erstens in den äusseren Erdkern unter einem sehr grossen Inzidenzwinkel eindringen und zweitens eine längere Zeit benötigen, um den äusseren Teil des flüssigkeitsähnlichen Kerns zu durchlaufen.

Lamont Geological Observatory Contribution No. 558.  相似文献   

4.
Summary An explicit solution is obtained for the system of equations describing the spheroidal motion in a homogeneous, isotropic, gravitating, elastic medium possessing spherical symmetry. This solution is used to derive the Green's dyad for a homogeneous gravitating sphere. The Green's dyad is then employed to obtain the displacement field induced by tangential and tensile dislocations of arbitrary orientation and depth within the sphere.Notation G Gravitational constant - a Radius of the earth - A o =4/3 G - Perturbation of the gravitational potential - Circular frequency - V p ,V s Compressional and shear wave velocities - k p =/V p - k s =/V s - k p [(2.8)] - , [(2.17)] - f l + Spherical Bessel function of the first kind - f l – Spherical Hankel function of the second kind - x =r - y =r - x o =r o - y o =ro - x =r k s - y =r k p - x o =r o k s - y o =r o k p - =a - =a - [(5.17)] - m, l   相似文献   

5.
The relationships between the linearized meteorological variables as expressed in geometric height and in log-pressure coordinates are derived from the assumptions of classical atmospheric tidal theory. While the horizontal velocity components are the same to first-order in the two coordinate systems, a linearized vertical velocity differencew-H 0 occurs because of the periodic vertical displacement of the constant pressure surfaces due to time-dependent, hydrostatic density perturbations; a linearized temperature differenceT- also results when these displacements occur in the presence of a zero-order vertical gradient of temperature. Both of these differences can be expressed in terms of the tidal geopotential field. For a given tidal mode, both differences are generally proportional to the square root of the ratio of the tidal mode's equivalent depth and the atmospheric scale height; the temperature difference is also proportional to the background temperature lapse rate. It is further shown that the two classical tidal vertical structure equations commonly derived in their respective geometric height and log-pressure coordinate systems are in fact identical to first-orderas long as the same thermotidal forcing function is used. Expressions for the zonal-mean components of the tidal bilinear fluxes, formed by zonally averaging the product of two longitudinally varying, linearized tidal fields, are also derived for the two coordinate systems. For the bilinear fields the largest relative differences (a few tens of percent) are for the tidal zonal-mean forcing per unit mass of the zonal wind. For Earth and Mars, differences between the tidal vertical velocity fields are generally less than 25% but may be significantly larger in the Martian atmosphere during one of its episodic planetary-scale dust storms. Tidal temperature differences are generally smaller.  相似文献   

6.
Summary The variations of the initialh E s height are investigated in the solar cycle 1957–1968, deriving the regressive dependency:h E s =121.4–6·10–2 R referring to the median monthly values at a solar zenith angle =75°. The similar variations ofh E s (R) during the day and night are interpreted as a domination of the sporadic layer formation from a redistribution of the day-time ionization and secondary participation of nightly ionizing sources. The analogous cyclich E s andh E variations confirm this conclusion while the seasonal variations in the state of the sporadic layer show outlined dynamical effects. The comparatively not big cyclic variation in the spatial state of theE-region are considered to confirm the predominating ionizing action of the ultraviolet range (933–1038 Å) in the lower part of theE-region, while the soft X-radiation influences mainly the near maximum part of this region.  相似文献   

7.
The nightglow OH(9,4) and O2 atmospheric (0,1) band emission intensities and their rotational temperatures T(OH) and T(O2), respectively, observed at Cachoeira Paulista (23° S, 45°W), Brazil, during the period from October 1989 to December 1990, have been analyzed to study the nighttime mesospheric energy loss rates through the radiations from the vibrationally excited OH* and electronically excited O*2 bands. The total emission rates of the OH Meinel bands, O2 atmospheric (0,0) and O2 infrared atmospheric (1g) bands were calculated using reported data for the relative band intensities and . It was found that there is a minimum in equivalent energy loss rate by the OH* Meinel bands during December/January (equivalent energy loss rate of 0.39 K/day*, where day* means averaged over the night) and maximum in equivalent energy loss rate during September (equivalent energy loss rate of 0.98 K/day*). Energy loss rate by the O*2 radiation, on the other hand, is weaker than that by the OH* Meinel bands, showing equivalent energy loss rates of 0.12 K/day* and 0.22 K/day* during January and September, respectively.  相似文献   

8.
Summary A preliminary observation has been made of the magnetic fabric in 14 specimens of undeformed sediment which exhibit repeatable principal orientation in undemagnetized state as well as after some steps of thermal demagnetization. They were chosen from 2000 specimens of the Tertiary formations of inland fluvio-lacustrine facies in the Qaidam basin, NW China. It was found that no large changes in magnetic fabric occur after stepwise thermal demagnetization up to 300°C, but some significant changes take place after treatment at higher temperature (500° up to 750°C). It is shown that the orientations of the 3 principal axes remain unchanged after each demagnetization step, whereas the differences between the principal values (L=K1–K2 and F=K2–K3) are greatly enhanced after high temperatures have been applied. The enhancement of L and F with no change in principal orientations facilitates the determination of the principal orientations. In our case one may easily measure the thermally enhanced magnetic lineation to estimate the palaeocurrent direction.Presented at 2nd conference on New Trends in Geomagnetism, Bechyn Castle, Czechoslovakia, September 24–29, 1990.  相似文献   

9.
Zusammenfassung Es wird die Gleichung für die Elektronenproduktionq(z) abgeleitet, die die meteorologischen Elemente der Mesosphäre berücksichtigt. Nach Angaben über die mit Satelliten und Raketen gemessene Röntgenstrahlung mit 8 Å wird das Differentialspektrum des ionisierenden Energieflusses für eine mittlere Sonnenaktivität konstruiert. Auf dieser Grundlage und nach der bekannten Intensität der Strahlung Ly- sowie nach Angaben über dieElektronenproduktion der kosmischen Strahlung werden die Profileq Rö(z),q Ly-(z) undq CR(z) für mittlere geographische Breiten und Standardatmosphäre entwickelt. Nach eingehender Analyse der vollständigen Gleichung für den effektiven Rekombinationskoeffizienten wird für die Verhältnisse in der tiefen Ionosphäre der Beitrag jeder einzelnen Komponente der Gleichung bestimmt. ist eine recht veränderliche Grösse, die von den aeronomischen und meteorologischen Verhältnissen und der Sonnenzenitdistanz abhängt. Aus den fürq(z) und (z) erhaltenen Angaben werden zwei ElektronendichteprofileN(z) für =30° und 75° erhalten. Das ProfilN(z) bei =30° wird mit dem gemittelten Profil einer umfangreichen Gruppe experimentell gefundener VerteilungenN(z) verglichen; das Profil bei =75° wird durch Messung der deviativen und nondeviativen Absorption für eine längere Zeitperiode überprüft. In beiden Fällen hat sich die Richtigkeit der theoretisch erhaltenen Profile bestätigt. Die jahreszeitlichen Variationen der nondeviativen Absorption in derD-Region sind ausschliesslich durch die Variationen der meteorologischen Parameter im Bereich der Mesopause bei konstantem Energiefluss der ionisierenden Strahlung bedingt.
Summary An equation about the electron production is deduced in which the meteorological elements of the mesosphere are taken into account. The differential spectrum of the ionizing energy flux with 3 Å for average solar activity is constructed on evidence from rocket and satelitc measurements. The profilesq Rö(z),q Ly-(z) andq CR(z) for mean geographical latitudes and standard atmosphere are plotted on that basis as well as on data fot the known intensity of the Ly- emission and the electron production of the cosmic rays. An exhaustive analysis is made of the full equation for the effective recombination coefficient and the contribution of all its components at lower ionosphere conditions is determined. is a rather variable quantity, dependent on the aeronomical and meteorological condition of the area under consideration, as well as on the solar zenith angle. Two profiles for the electron concentrationN(z) at =30° and 75° are drawn on the basis of data forq(z) and (z). The profileN(z) at =30° is compared with the averaged profile of a large group experimentally obtained distributionsN(z); the profile at =75° is checked by measurements of the deviative and nondeviative absorption taken for a lengthy period. Both checks are in good agreement with the theoretically obtained profiles. The seasonal variations of the nondeviative absorption in theD region could be completely explained with the variations of the meteorological parameters in the mesopause area at constant energy flux of the ionizing radiation.
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10.
Summary Utilising two years data collected at two tropical coastal stations, Madras (13°04N, 80°15E) and Waltair (17°42N, 83°18E) and for one tropical continental station, Nagpur (21°09N, 79°07E), the authors have re-evaluated the constants ofBrunt's regression equation. Analyses of the observations for Waltair and Nagpur show good correlation coefficients (r) between the values of the effective emissivity of the atmosphere (the effective emissivity is the ratio of incoming long-wave sky radiation at the surfaceR s , to black body radiation T 4) and the square root values of surface vapour pressuree (mb). The value ofr for Waltair from radiometer observations is 0.98. It is also determined for Waltair and Nagpur from Ångström compensation pyrgeometer observations as 0.83 and 0.91 respectively. A low correlation co-efficient 0.56 is obtained for Madras. It might be due to higher surface vapour pressure values at Madras than at Waltair and Nagpur. The applicability of the reduced regression equations are examined for different years for the different stations. The agreement between the computed values with the new regression equations and the observed long-wave sky radiation at the surface seems to be quite good.  相似文献   

11.
Summary Echo soundings of the U.S. Cruiser Milwaukee in the Puerto Rico Trough in 1939 are briefly discussed, and two depths of 30246 feet or 9219 m, found at 19° 36 N, 68° 20.5 W and at 19° 35N, 68° 8.75W, are stated to be the greatest depths which are known so far in the Atlantic Ocean.  相似文献   

12.
Zusammenfassung Aus der schon früher bewiesenen Eindeutigkeit des Dichtegesetzes der sphäroidischen Gleichgewichtsfiguren ergibt sich die Möglichkeit, aus einer gegebenen Gleichgewichtsfigur durch «Entblätterung» eine unendliche Reihe neuer Gleichgewichtsfiguren derselben Rotationsgeschwindigkeit mit ständig abnehmender Größe und Masse zu bilden. Auf diese Weise kann man jede beliebige innere Niveaufläche der ursprünglichen Figur bloßlegen und aus der von ihr umschlossenen TeilmasseE, der Rotationsgeschwindigkeit , der Äquatorachsea und der Äquatorachsea h des homogenen Ausgangsellipsoides der zugehörigen Figurenreihe (,C) die Abplattung berechnen und gewinnt so die Abplattungsfunktion im Innern einer Gleichgewichtsfigur gänzlich unabhängig von derClairautschen Differentialgleichung. Die Methode der Entblätterung ist auch auf höherparametrige Gleichgewichtsfiguren mit unstetigem Dichtegesetz anwendbar; sie liefert für dasWiechertsche Modell die Kernoberfläche in einer Tiefe von 3864.75 km und einen Dichtesprung von 17.84.
Summary In a previous paper I have shown, that the law of density of the spheroidal figures of equilibrium is strictly individual. This makes it possible from a given figure of equilibrium by the so called method of «stripping of leaves» to gain an infinite series of new figures of equilibrium with permanently decreasing size and mass. In this manner any inner level surface of the given figure can be laid bare and its flattening can be calculated from the enclosed part of massE, the rotation velocity , the equator axisa and from the equator axisa h of theMacLaurin ellipsoid in the beginning of the series (,C) belonging to the seeked figure. So the function of flattening in the interior of any equilibrium figure is gained totally independant fromClairaut's differential equation. The method of «stripping of leaves» also can be used for figures of equilibrium with more than one form-parameter and with discontinual density distribution. It yields forWiechert's model the surface of the core in a depth of 3864.75 km and a discontinuity of 17.84 in density.
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13.
Résumé La première partie de l'article contient les résultats des mesures magnétiques, effectuées à Kaboul par Monsieur D.S.A.Adams et par l'auteur indépendamment. À cause du manque des instruments magnétiques de campagne, nous avons exécuté les mesures au moyen des appareils de laboratoire. On a obtenu les valeurs approximatives suivantes pour l'époque 1948.0 à Kaboul: et une variation séculaire de la déclinaison magnétique de—3 par an. Dans la deuxième partie l'auteur discute les mesures magnétiques exécutées dans la Province du Nord de l'Afghanistan et publiées parWeinberg etZimmermann. Les chiffres en question montrent une variation annuelle de la déclinaison magnétique en Turkestan Afghan de +1.0 jusqu'à –0.6, de 4.9 jusqu'à 6.0 pour l'inclinaison, et de –37 jusqu'à –52 pour la composante horizontale. L'auteur suppose que le terrain afghan soit anomral au point de vue magnétique et mentionne que certaines anomalies magnétiques ont été découvertes près d'Achkhabad, au voisinage de la frontière d'Iran, par les géologues Russes.  相似文献   

14.
The authors conducted a Rn222 survey in wells of the Larderello geothermal field (Italy) and observed considerable variations in concentrations. Simple models show that flow-rate plays an important part in the Rn222 content of each well, as it directly affects the fluid transit time in the reservoirs. Rn222 has been sampled from two wells of the Serrazzano area during flow-rate drawdown tests. The apparent volume of the steam reservoir of each of these two wells has been estimated from the Rn222 concentration versus flow-rate curves.List of symbols Q Flow-rate (kg h–1) - Decay constant of Rn222 (=7.553×10–3 h–1) - Porosity of the reservoir (volume of fluid/volume of rock) - 1 Density of the fluid in the reservoir (kg m–3) - 2 Density of the rock in the reservoir (kg m–3) - M Stationary mass of fluid filling the reservoir (kg). - E Emanating power of the rock in the reservoir (nCi kg rock –1 h–1). - P Production rate of Rn222 in the reservoir: number of atoms of Rn222 (divided by 1.764×107) transferred by the rock to the mass unit of fluid per unit time (nCi kg fluid –1 h–1). - N Specific concentration of Rn222 in the fluid (nCi kg–1) - Characteristic time of the steam reservoir at maximum flow-rate (=M/Q)  相似文献   

15.
Janle  P.  Meissner  R. 《Surveys in Geophysics》1986,8(2):107-186
Geo-scientific planetary research of the last 25 years has revealed the global structure and evolution of the terrestrial planets Moon, Mercury, Venus and Mars. The evolution of the terrestrial bodies involves a differentiation into heavy metallic cores, Fe-and Mg-rich silicate mantles and light Ca, Al-rich silicate crusts early in the history of the solar system. Magnetic measurements yield a weak dipole field for Mercury, a very weak field (and local anomalies) for the Moon and no measurable field for Venus and mars. Seismic studies of the Moon show a crust-mantle boundary at an average depth of 60 km for the front side, P- and S-wave velocities around 8 respectively 4.5 km s–1 in the mantle and a considerable S-wave attenuation below a depth of 1000 km. Satellite gravity permits the study of lateral density variations in the lithosphere. Additional contributions come from photogeology, orbital particle, x-and -ray measurements, radar and petrology.The cratered surfaces of the smaller bodies Moon and Mercury have been mainly shaped by meteorite impacts followed by a period of volcanic flows into the impact basins until about 3×109 yr before present. Mars in addition shows a more developed surface. Its northern half is dominated by subsidence and younger volcanic flows. It even shows a graben system (rift) in the equatorial region. Large channels and relics of permafrost attest the role of water for the erosional history. Venus, the most developed body except Earth, shows many indications of volcanism, grabens (rifts) and at least at northern latitudes collisional belts, i.e. mountain ranges, suggesting a limited plate tectonic process with a possible shallow subduction.List of Symbols and Abbreviations a=R e mean equatorial radius (km) - A(r, t) heat production by radioactive elements (W m–3) - A, B equatorial moments of inertia - b polar radius (km) - complex amplitude of bathymetry in the wave number (K) domain (m) - C polar moment of inertia - C Fe moment of inertia of metallic core - C Si moment of inertia of silicate mantle - C p heat capacity at constant pressure (JK–1 mole–) - C nm,J nm,S nm harmonic coefficients of degreen and orderm - C/(MR e 2 ) factor of moment of inertia - d distance (km) - d nondimensional radius of disc load of elastic bending model - D diameter of crater (km) - D flexural rigidity (dyn cm) - E Young modulus (dyn cm–2) - E maximum strain energy - E energy loss during time interval t - f frequency (Hz) - f flattening - F magnetic field strength (Oe) (1 Oe=79.58A m–1) - g acceleration or gravity (cms–2) or (mGal) (1mGal=10–3cms–2) - mean acceleration - g e equatorial surface gravity - complex amplitude of gravity anomaly in the wave number (K) domain - g free air gravity anomaly (FAA) - g Bouguer gravity anomaly - g t gravity attraction of the topography - G gravitational constant,G=6.67×10–11 m3kg–1s–2 - GM planetocentric gravitational constant - h relation of centrifugal acceleration (2 R e ) to surface acceleration (g e ) at the equator - J magnetic flux density (magnetic field) (T) (1T=109 nT=109 =104G (Gauss)) - J 2 oblateness - J nm seeC nm - k (0) (zero) pressure bulk modulus (Pa) (Pascal, 1 Pa=1 Nm–2) - K wave number (km–1) - K * thermal conductivity (Jm–1s–1K–1) - L thickness of elastic lithosphere (km) - M mas of planet (kg) - M Fe mass of metallic core - M Si mass of silicate mantle - M(r) fractional mass of planet with fractional radiusr - m magnetic dipole moment (Am2) (1Am2=103Gcm3) - m b body wave magnitude - N crater frequency (km–2) - N(D) cumulative number of cumulative frequency of craters with diameters D - P pressure (Pa) (1Pa=1Nm–2=10–5 bar) - P z vertical (lithostatic) stress, see also z (Pa) - P n m (cos) Legendre polynomial - q surface load (dyn cm–2) - Q seismic quality factor, 2E/E - Q s ,Q p seismic quality factor derived from seismic S-and P-waves - R=R 0 mean radius of the planet (km) (2a+b)/3 - R e =a mean equatorial radius of the planet - r distance from the center of the planet (fractional radius) - r Fe radius of metallic core - S nm seeC nm - t time and age in a (years), d (days), h (hours), min (minutes), s (seconds) - T mean crustal thickness from Airy isostatic gravity models (km) - T temperature (°C or K) (0°C=273.15K) - T m solidus temperature - T sideral period of rotation in d (days), h (hours), min (minutes), s (seconds), =2/T - U external potential field of gravity of a planet - V volume of planet - V p ,V s compressional (P), shear (S) wave velocity, respectively (kms–1) - w deflection of lithosphere from elastic bending models (km) - z, Z depth (km) - z (K) admittance function (mGal m–1) - thermal expansion (°C–1) - viscosity (poise) (1 poise=1gcm–1s–1) - co-latitude (90°-) - longitude - Poisson ratio - density (g cm–3) - mean density - 0 zero pressure density - m , Si average density of silicate mantle (fluid interior) - average density of metallic core - t , top density of the topography - density difference between crustal and mantle material - electrical conductivity (–1 m–1) - r , radial and azimuthal surface stress of axisymmetric load (Pa) - z vertical (lithostatic) stress (seeP z ) - II second invariant of stress deviation tensor - latitude - angular velocity of a planet (=2/T) - ages in years (a), generally 0 years is present - B.P. before present - FAA Free Air Gravity Anomaly (see g - HFT High Frequency Teleseismic event - LTP Lunar Transient Phenomenon - LOS Line-Of-Sight - NRM Natural Remanent Magnetization Contribution No. 309, Institut für Geophysik der Universität, Kiel, F.R.G.  相似文献   

16.
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17.
nuam aau ¶rt; amu a um ¶rt; ¶rt;a uauu. ¶rt; ¶rt;a, ¶rt;mu auumu m mnam u nu mum ¶rt;a, umam m ¶rt;u z aa n¶rt; uuu, a aau. u¶rt; auum ¶rt;au z naa m mauu ¶rt; amu, naam, m ¶rt;au ¶rt;z naa zauuam u amu ¶rt;.
Summary A formation of ice particles on artificial deposition INis described. INacting in dependence on the temperature and supersaturation over the ice are considered in the 1 D SSconvection cloud model with detailed microphysics including freezing. The limiting influence of the water vapour pressure upon the concentration of active INis shown resulting from the dependence of water vapour pressure on the ice particle concentration.
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18.
Zusammenfassung In der modernen Registriertechnik strebt man immer mehr danach mittels elektrischer Übertragungsanlagen (Verstärker) geophysikalische Vorgänge sofort sichtbar aufzuzeichnen. Bei der Erdmagnetik konnte die photographische Aufzeichnung wegen ihrer Genauigkeit durch keine andere Methode ersetzt werden. Eine elektrische Übertragung auf P. Schreiber ist nur mit Hilfe von Differential-Photozellen möglich. Am obigen Observatorium läuft seit Oktober 1953 eine Anlage für die Deklination und Horizontalintensität. DasH-Variometer (einTöpfer-Instrument) ist temperaturkompensiert; dasD-Variometer wurde am Observatorium hergestellt und besitzt ein Plexiglas-Gehäuse. Die mit besonderen Blenden ausgestatteten Projektoren beleuchten die Variometer, die gleichmäßig ausgeleuchtete Lichtrechtecke auf die Zellen werfen. — Die Skalenwerte betragen inD: 0.70±0.03, inH: 4.2±0.05 Gamma pro pars. Die Anlage erweist sich als sehr praktisch für die Prognose ionosphärischer Störungen.
Summary In modern technique for recordings the directly visible drawing of geophysical processes is more and more used by means of electrical arrangements of transmission (amplifier). The photographic recording in the research of earth-magnetism could not be substituted with another method on account of its exactness. An electrical transmission at point-writers is only possible with differential-photocells. At the Observatory in Fürstenfeldbruck an arrangement for declination and horizontalintensity is now working since October 1953. TheH-variometer (byTöpfer) is compensated for temperature; theD-variometer was constructed at the Observatory and has a case of plexigum. The projecters furnished with special diaphragm lights up the variometers which throw equal clear rectangles of light at the cells. — The scalevalues are inD 0.70±0.03, inH: 4.2±0.05 Gamma per pars. The arrangement is very usefull for prognosis of ionospheric disturbances.
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19.
n¶rt;m u u¶rt; umnu n-a nmam, ma ¶rt;mm n¶rt; u (auum m um ¶rt;uam, aum ua¶rt;m umnua uu). ¶rt;a nu¶rt;um nmu u¶rt; ma umnu u m ma.  相似文献   

20.
Summary The optimization of the method of determining the addition constant of an EDM is discussed. The advantages of the optimization procedure from the point of view of efficiency and improvement of accuracy are reported.
nuuu ¶rt; n¶rt;u a¶rt;¶rt;uu n ¶rt;. u nu n u uu u nu u.
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