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521.
N. Seehafer 《Solar physics》1978,58(2):215-223
At first it is shown that a magnetic field being force-free, i.e. satisfying × B = B, with = constant ( 0) in the whole exterior of the Sun cannot have a finite energy content and cannot be determined uniquely from only one magnetic field component given at the photosphere. Then the boundary value problem for a semi-infinite column of arbitrary cross section is solved by a Green's function method. 相似文献
522.
A high-resolution (0.6 cm?1) spectrum of Jupiter at 5 μm recorded at the Kuiper Airborne Observatory is used to determine upper limits to the column density of 19 molecules. The upper limits to the mixing ratios of SiH4, H2S, HCN, and simple hydrocarbons are discussed with respect to current models of Jupiter's atmosphere. These upper limits are compared to expectations based upon the solar abundance of the elements. This analysis permits upper limit measurements (SiH4), or actual detections (GeH4), of molecules with mixing ratios with hydrogen as low as 10?9. In future observations at 5 μm the sensitivity of remote spectroscopic analyses should permit the study of constituents with mixing ratios as low as 10?10, which would include the hydrides of such elements as Sn and As as well as numerous organic molecules. 相似文献
523.
Slitless spectrograms obtained during the eclipse of 10 June 1972 have been analyzed to determine the height distribution of the D3 He line intensity.For undisturbed regions the maximum of D3 line intensity is confirmed to exist at about 1700km above the limb. Besides the above mentioned maximum, in plages a considerable intensity may be observed at low heights (h < 1000 km).An analysis of these observations for h > 1000 km has been carried out within the low temperature mechanism of triplet helium emission taking into account the helium ionization by XUV radiation. The density dependence of the 23
S level population at different XUV flux values has been calculated. Our observations give N
e 2 × 1010 cm–3 in the chromosphere at h = 2000 km. The probable coincidence of the H and He emission small filaments in the middle chromosphere is discussed. 相似文献
524.
This paper deals with inclusions, megacrysts, and nodules froma group of Stephanian and Permian vents and associated intrusiveson the Fife (Scotland) coast near Elie. The petrography andchemistry of inclusions of spinel Iherzolite, wehrlite, andclinopyroxenite are described. The Elie Ness vent contains coarse-grainedplutonic nodules (Elie type nodules) and megacrysts of pyrope,sub-calcic augite, kaersutite, and anorthoclase. Elie type nodulesare divisible into five groups: (1) kaersutite-olivine-pyroxenite,(2) type 1 +oligoclase, (3) biotite-pyroxenite, (4) sodic amphibole-biotite-albite,(5) biotite-albite. Experimental studies show that sub-calcic augite and pyropephenocrysts could have coprecipitated from an alkali basaltmagma at P > 25 kb, T = 13001450 ?C. It is proposedthat the primary alkali basalt liquid was formed by partialmelting of a vapour-free, mica-bearing garnet Iherzolite mantleat a depth of c. 100 km, with subsequent pyrope-augite phenocrystcrystallization at not less than 70 km depth. Geochemical studiesof clinopyroxenes from the Elie type nodules indicate crystallizationwithin the lower crust. It is proposed that types 1 and 2 nodulesare cumulates from the alkaline basaltic liquid, intercumuluskaersutite representing compositions of liquids intermediateon the Fife basalt trend. Type 3 nodules may represent basalticliquids at the basic end of the Fife trend, wholly crystallizedat pressure from 1015 kb. Experimental data on stabilityof anorthoclase in its host basanite show it to be present inthe basanite melting interval only at P < 9 kb (dry). Itis thought that crystallization of anorthoclase may be associatedwith formation of types 4 and 5 nodules, possibly from a trappedpocket of evolved alkaline liquid at upper crustal levels. TheElie Ness eruption must have been rapid enough to strip theaccumulated pyroxenites from the lower crust and carry unresorbedgarnet megacrysts from depths of over 70 km. Spinel-lherzoliteinclusions are found only in late stage basic sheets whose intrusionmay be unrelated to the initial violent tuff eruptions. 相似文献
525.
Grains ejected from stars at velocities of 107 cm s–1 and/or grains accelerated by the pressure of starlight in the intercloud medium to velocities in the range 2×106–107 cm s–1 are slowed to velocities of about 2×105 cm s–1 in a typical interstellar cloud. The interaction of fast grains with gas atoms as they are slowed in clouds could provide (a) the dominant heat source for interstellar clouds; (b) sites for molecule formation; and (c) a mechanism of providing a pressure balance between clouds and the intercloud medium.Paper presented at the Symposium on Solid State Astrophysics, held at the University College, Cardiff, Wales, between 9–12 July, 1974. 相似文献
526.
The work of Brown and Hoyng (1975) on the betatron acceleration of hard X-ray source electrons trapped in a vibrating flux tube is generalised to include Fermi acceleration by the varying transverse field. This development can explain the trajectory of bursts in a plot of equivalent thick-target electron flux
versus spectral index as inferred from observations obtained by ESRO TD1A. Specifically the loops observed in this
, diagram, unexplained in Brown and Hoyng's anslysis are accounted for by a changing phase relationship between the varying field strength f(t) and magnetic scale length g(t)- Application of the formalism to the detailed TD1A observations of the large events of 1972, August 4 and 7, allows inference of the evolution of f(t), g(t) in these events.Now at: Space Sciences Laboratory, University of California, Berkeley, U.S.A. 相似文献
527.
The occurrence at a heliocentric distance of 1 AU of alpha particle streaming velocities larger than proton streaming velocities,v
/v
p
>1 (Ogilvie, 1975) is investigated on the basis of the theory suggesting the existence in the solar wind of an accelerating force acting preferentially on the alpha particles.Accurate solution of the three-fluid model equations for the quiet solar wind indicates that anecessary andsufficient condition for (v
/v
p
)1 AU>1 is the presence of a relativelyweak accelerating forceacting in a limited region in the vicinity of 1 AU. If the force is effectiveonly at small heliocentric distances, the alpha particle streaming velocity excess vanishes at distances less than 1 AU, because of the (equalization) action of the dynamical friction force. 相似文献
528.
D. E. Blackwell P. A. Ibbetson C. A. Murray N. M. Pratt 《Astrophysics and Space Science》1976,43(2):469-473
A quantitative definition of limiting magnitude for stellar photographs is proposed, together with a method of measurement employing a Racine prism. Limiting magnitudes inU, B andV for the Isaac Newton telescope at Herstmonceux derived from a total of 72 prime focus photographs are presented and the results correlated with the size of the photographed image. The limiting magnitude for an extrapolated value of the seeing of 1 isB=22m.0, in good agreement with a value obtained by scaling the limiting magnitudes of the 200 inch telescope. 相似文献
529.
The July 12, 1973, occultation of Europa by Io was observed in 30 wavelength channels in the spectral region λλ3200-11, 000 Å with the 200-inch Hale telescope and a multichannel spectrometer. The data are presented in absolute units above the Earth's atmosphere. The data are analyzed to obtain the spectral reflectivity of seven localized areas on the disk of Europa centered on 324°W longitude. The equatorial material is confirmed to be darker than the eastward-skewed bright north polar cap and a hint is evident that the darker material as well may be somewhat redder than the cap material. 相似文献
530.
A.J. Kliore G. Fjeldbo B.L. Seidel D.N. Sweetnam T.T. Sesplaukis P.M. Woiceshyn S.I. Rasool 《Icarus》1975,24(4):407-410
The occultation of the Pioneer 10 spacecraft by Io (JI) provided an opportunity to obtain two S-band radio occultation measurements of its atmosphere. The dayside entry measurements revealed an ionosphere having a peak density of about 6 × 104 elcm?3 at an altitude of about 100 km. The topside scale height indicates a plasma temperature of about 406 K if it is composed of Na+ and 495 K if N2+ is principal ion. A thinner and less dense ionosphere was observed on the exit (night side), having a peak density of 9 × 103 elcm?3 at an altitude of 50 km. The topside plasma temperature is 160 K for N2? and 131 K for Na+. If the ionosphere is produced by photoionization in a manner analogous to the ionospheres of the terrestrial planets, the density of neutral particles at the surface of Io is less than 1011?1012 cm3, corresponding to a surface pressure of less than 10?8 to 10?9 bars. Two measurements of its radius were also obtained yielding a value of 1830 km for the entry and 192 km for the exit. The discrepancy between these values may indicate an ephemeris uncertainty of about 45 km. The two measurements yield an average radius of 1875 km, which is not in agreement with the results of the Beta Scorpii stellar occultation. 相似文献