Essentials of physical geography | R.E. Gabler,R.J. Sager,S. Brazier,and J. Pourciau, 1977. Holt-Saunders,Eastbourne, 511 pp     

E.F. Chiburis 《Earth》1978,14(2):201-202

  相似文献   

Photoelectron fluxes in cometary atmospheres     

O. Ashihara 《Icarus》1978,35(3):369-384

The photoelectron fluxes in cometary atmospheres are calculated by a Monte Carlo method. This is the first quantitative model calculation of this kind. A pure H₂O atmosphere is assumed with a sublimation rate of 10³⁰ molecules sec^?1 at 1 AU. Discussions of the energetics of electron gas and of the elementary collisional processes in determining the fluxes largely concern this water atmosphere. Influences on the photoelectron fluxes are also investigated for CO, another possible constituent. The excitation rate of the ${}^1\text{D}$ level of atomic oxygen in electron impacts is evaluated. It is highly improbable that the photoelectrons are responsible for the observed 6300 Å emission of the order of 1 kR at a heliocentric distance of 1 AU. The structure of the heat equation for thermal electrons is analyzed and a drastic change of the plasma behavior within the coma region is expected.  相似文献   

A trigger mechanism for the emerging flux model of solar flares     

T. J. Tur  E. R. Priest 《Solar physics》1978,58(1):181-200

The energetics of a current sheet that forms between newly emerging flux and an ambient field are considered. As more and more flux emerges, so the sheet rises in the solar atmosphere. The various contributions to the thermal energy balance in the sheet are approximated and the resulting equation solved for the internal temperature of the sheet. It is found that, for certain choices of the ambient magnetic field strength and velocity, the internal temperature increases until, when the sheet reaches some critical height, no neighbouring equilibrium state exists. The temperature then increases rapidly, seeking a hotter branch of the solution curve. During this dynamic heating, the threshold temperature for the onset of plasma microinstabilities may be attained. It is suggested that this may be a suitable trigger mechanism for the recently proposed emerging flux model of a solar flare.This work was done while the author was participating in the CECAM workshop on Plasma Physics applied to Active Solar Phenomena, August–September 1976 at Orsay, France, and the Skylab Solar Workshop on Solar Flares (sponsored by NASA and NSF and managed by the High Altitude Observatory).  相似文献   

On the dissociation of nitrogen by electron impact and by E.U.V. photo-absorption     

E.C. Zipf  R.W. McLaughlin 《Planetary and Space Science》1978,26(5):449-462

The dissociation of N₂ by electron impact and by e.u.v. photo-absorption is studied, and it is shown that the forbidden predissociation of the numerous ¹Π_u and ¹Σ_u⁺ valence and Rydberg states of N₂ in the 11–24eV energy range is the dominant mechanism for N atom production. By measuring the absolute emission cross sections for the e.u.v. singlet bands of N₂ and by using the generalized oscillator strength data of Lassettre (1974), it has been possible to construct a detailed model of the total N₂ dissociation cross section which is in good agreement with the measurements of Winters (1966) and Niehaus (1967) and provides some insights into the maximum possible $\text{N(}{}^2\text{D)}$ yield from dissociative excitation. The total cross section for exciting N₂ e.u.v. radiation in the 800Å–1100Å wavelength range has been measured and found to have a value of 3.4 ×10^?17 cm² at 100 eV under optically thin conditions. Although this result implies that large fluxes of e.u.v. photons should be excited in auroral substorms and in the airglow, they are not observed, and we show that this development is a consequence of radiation entrapment and predissociation. The total cross section for dissociating N₂ by electron impact is given for optically thin and thick media. And some questions concerning the energy budget of a magnetospheric storm which are raised by these results, are discussed.  相似文献   

Pre-flare association of magnetic fields and millimeter-wave radio emission     

E. B. Mayfield  K. P. White III 《Solar physics》1976,47(1):277-284

Observations of radio emission at 3.3 mm wavelength associated with magnetic fields in active regions are reported. Results of more than 200 regions during the years 1967–1968 show a strong correlation between peak enhanced millimeter emission, total flux of the longitudinal component of photospheric magnetic fields and the number of flares produced during transit of active regions. For magnetic flux greater than 10²¹ maxwells flares will occur and for flux of 10²³ maxwells the sum of the H flare importance numbers is about 40. The peak millimeter enhancement increases with magnetic flux for regions which subsequently flared. Estimates of the magnetic energy available and the correlation with flare production indicate that the photospheric fields and probably chromospheric currents are responsible for the observed pre-flare heating and provide the energy of flares.This work was supported in part by NASA Contract No. NAS2-7868 and in part by Company funds of The Aerospace Corporation.  相似文献   

Corporate Organisation, Corporate Strategy and Agribusiness Development in New Zealand: An Introductory Study with Particular Reference to the Fruit and Vegetable Processing Industry     

R. B. Le Heron  E. C. R. Warr 《New Zealand geographer》1976,32(1):1-16

  相似文献   

Type IV dm bursts: Onset and sudden reductions     

Arnold O. Benz  Jan Kuijpers 《Solar physics》1976,46(2):275-290

The effect of collisions of suprathermal electrons with a thermal background plasma is investigated and is shown to cause flattening of a monotonically descending velocity distribution of fast particles. As a result flare-produced energetic electrons that are trapped in a coronal magnetic arch and that are initially distributed in energy according to a power-law, can give rise to an instability of Langmuir waves in the background plasma and the subsequent emission of continuum radiation as observed in type IV dm bursts.To explain the appearance of sudden reductions observed in type IV dm outbursts the effects both of magnetic compressions of the source region and of renewed injections of fast particles on the continuum source are investigated. It is found that the latter process can explain the observed reductions.  相似文献   

Dynamics of coronal hole regions     

Roger A. Kopp  Thomas E. Holzer 《Solar physics》1976,49(1):43-56

The hydrodynamic properties of a steadily expanding corona are explored for situations in which departures from spherically symmetric outflow are large, in the sense that the geometrical cross section of a given flow tube increases outward from the Sun faster than r ² in some regions. Assuming polytropic flow, it is shown that in certain cases the flow may contain more than one critical point. We derive the criterion for determining which of these critical points is actually crossed by the transonic solution which begins at the Sun and extends continuously outward. Next, we apply the theory to geometries which exhibit rapid spreading of the flow tubes in the inner corona, followed by more-or-less radial divergence at large distances. This is believed to be the type of geometry found in coronal hole regions. The results show that, if this initial divergence is sufficiently large, the outflow becomes supersonic at a critical point encountered low in the corona in the region of high divergence, and it remains supersonic at all greater heights in the corona. This feature strongly suggests that coronal hole regions differ from other open-field regions of the corona in that they are in a fast, low density expansion state over much of their extent. Such a dynamical configuration makes it possible to reconcile the low values of electron density observed in coronal holes with the large particle fluxes in the associated high speed streams seen in the solar wind.The National Center for Atmospheric Research is sponsored by the National Science Foundation.  相似文献   

Differential rotation and giant cell circulation of solar Ca+-network     

E. H. Schröter  H. Wöhl 《Solar physics》1976,49(1):19-32

We report new results obtained from high precision computer controlled tracings of ca. 400 bright Ca⁺-mottles made during summer 1975 in continuation of our 1974 program (Schröter and Wöhl, 1975). In particular, we looked in 1975 for the existence of a giant circulation pattern in the equatorial zone. We find for the differential rotation: = 13.93 – 2.90 sin² B (deg/day, sidereal) when combining the new measurements with those obtained in 1974. Observations from 26th April until June 19th give strong evidence that at that time four giant circulation cells, crossing the solar equator, (i.e. a nonaxisymmetric velocity field pattern with respect to the solar equator) did exist. This yields two more rapid and two slower rotating sectors with v = ±80 m s^–1. These giant cells transport angular momentum towards the equator.  相似文献   

Scandium,chromium, iron,cobalt and nickel in some basic and ultrabasic rocks from west Norway     

L.B. Garmann  A.O. Brunfelt  K.S. Heier 《Chemical Geology》1976,18(1):49-53

Sixteen eclogites and ultrabasic rock samples from west Norway have been analyzed for Sc, Cr, Fe, Co and Ni by instrumental neutron-activation analysis.In gneiss-eclogites, Sc and Co give values from about 30 to 60 ppm and Cr and Ni from 180 to 700 ppm. An eclogite surrounded by a peridotite body shows nearly the same content of Sc and Co as do the gneiss-eclogites, but up to 20 times more Cr. Ni is only slightly more enriched in this particular eclogite than in the others.The ultrabasites have only a few ppm Sc, Co concentrates around 100 ppm while the Cr and Ni values are mainly found between 2 and 3,000 ppm.Fe shows an average value of nearly 10%.  相似文献