bluuebunny/crossref_metadata_2025_split huggingface dataset:
Ionosphere‐magnetosphere coupling: 1. Thermal plasma
Authors: Chappell Charles R. 
Published: February 2008

The past four years have seen a continued increasing interest in the basic processes which connect the thermal plasma population of the ionosphere with that of the outer magnetosphere. Measurement techniques have improved, and we are now able to observe the dynamics of the ionization in these regions as well as their detailed morphology. Although the specific reasons for the formation of the light ion trough and its connection with the plasmapause still elude us, we are beginning to grasp the nature of the many interchange flow processes which seem to play a basic role in the shaping of the well‐known plasmapause and light ion trough features.The thermal plasma population of the magnetosphere has also grown in importance. In addition to attracting the interest of scientists studying the ionosphere and plasmasphere the distribution of thermal plasma has also been found to affect the energetic particle population of the magnetosphere. This interaction between the hot and cold plasma has drawn the attention of workers studying the energetic particles of the radiation belts, the ring current, and the plasma sheet and has further emphasized the tight coupling within the magnetosphere‐ionosphere system.
Relativistic solar protons
Authors: Duggal S. P. 
Published: February 2008

This review attempts to summarize work by U.S. scientists, published during the period from 1971 to 1974, on various aspects of high‐energy solar protons associated with solar flares.In contrast with low‐energy particles, acceleration to higher energies is a rare phenomenon that occurs in discrete explosive events associated with solar disturbances [Van Hollebeke et al., 1974; Pomerantz and Duggal, 1974b]. Since the start of systematic and continuous observations in 1936, 25 ground level enhancements (GLE) representing the arrival of relativistic protons have been recorded [Pomerantz and Duggal, 1974b]. Although the attribution of each of the observed intensity enhancements to a specific solar flare has been relatively straightforward, contrary to earlier ideas no plausible correlation with the general level of solar activity has been established except for the obvious consequence of the fact that flares are rare at sunspot minimum.
Dynamo magnetic field generation
Authors: Levy E. H. 
Published: February 2008

The character of Earth's magnetic field, its internal source and its general shape, have been known since the time of Gilbert, some 400 years ago. The origin of the field has been the subject of speculation since that time; but it is hardly more than twenty years since our understanding of the generation mechanism began to fall together.From our modern perspective we can see that the phenomenon of natural magnetic field generation is common to bodies in the universe. Three of the nine planets in the solar system—Mercury, Earth, and Jupiter—are known with confidence to possess magnetic fields of internal origin. In addition we know of the sun's contemporaneously generated magnetic field. The Galaxy apparently contains a large scale magnetic field. Magnetic fields are common in stars and have intensities which cover a wide range. Some white dwarf stars and some neutron stars apparently possess magnetic fields with intensities far beyond those attained in the laboratory. While this is not an appropriate place to review all of these, it is worth keeping in mind that the subject addresses more bodies than just Earth and even the planets. Today it is reasonable to take the point of view—even if only as a working hypothesis—that many and perhaps all of these magnetic fields have their origins in active or previously active hydromagnetic dynamos.
Seismic source theory
Authors: Johnson Lane R. 
Published: February 2008

It is remarkable that seismology has progressed as far as it has while the knowledge in one vital area, that of the seismic source, has remained in a rather primitive state. However, if the recent research effort in the United States is any indication, this situation may be changing, because several promising lines of attack upon the problems of the seismic source have been generated during the past four years.For the sake of this review, studies of the seismic source will be divided into two basic groups, the theoretical studies which are directed primarily at formulating models of the earthquake process, and the observational studies which are directed primarily at obtaining the data necessary to either check the theoretical studies or investigate the consequences of interpreting earthquakes in terms of a specific model.
Middle atmosphere dynamics
Authors: Hartmann Dennis L. 
Published: February 2008

This review attempts to summarize briefly the efforts of scientists in the United States to understand the large‐scale dynamics and climatology of the middle atmosphere, which have appeared in the reviewed literature between January 1979 and September 1982. Some significant contributions have no doubt been overlooked; and for this I must ask the pardon of both the reader and the omitted author.The body of the review is divided into six sections and followed by a final section suggesting a few of the areas where progress may be expected in the future. The six major subject headings are: (1) New phenomena; (2) Large‐scale waves and instabilities; (3) Equatorial wave, mean‐flow interaction–long‐period oscillations; (4) Extratropical wave, mean‐flow interaction–Sudden warmings; (5) Climatology and general circulation of the middle atmosphere; and (6) Transport of trace chemicals. The division into sections is of course rather arbitrary. Some papers fit well in more than one section, and others do not fit neatly into any of the subheadings chosen.
Introduction to “Magma Genesis, plate tectonics, and chemical differentiation of the Earth” by Peter J. Wyllie
Authors: Lal D. 
Published: February 2008

One of the fundamental problems in geophysics is the chemical differentiation of the Earth, which is accomplished through magmatic processes, which in turn are a direct manifestation of convection within the mantle. The framework of plate tectonics is as yet the best model for explaining the different types and styles of magmatic activity.Experimental petrology calibrates the conditions for partial melting of various rock types and defines the conditions of magma crystallization under varied conditions. Laboratory data provide phase boundaries constraining the sites of partial melting in the Earth's interior.
Foreword
Authors: Wright R. W. H. , Matsushita S. 
Published: February 2008

The papers in this issue are based upon some of the contributions presented at the Third International Symposium on Equatorial Aeronomy held at the Physical Research Laboratories, Ahmedabad, India, February 3‐10, 1969. Previous meetings of the Symposia had been held in Huaychulo, Peru, in 1962, and in Sao José dos Campos, Brazil, in 1965.The earlier meetings had started cooperative work among workers in equatorial regions, initiating a breakdown of the tendency for the worker in equatorial regions to feel himself an ‘out‐station’ from one of the metropolitan countries. The conferences had also served the purpose of bringing some degree of unification among the areas of research that had tended to be pursued in isolated channels. Aeronomy is taken to include all studies of the earth's atmosphere above 60 km. Equatorial aeronomy restricts the interest to the vicinity of the equator and to effects that originate at the equator.
Heat, Moisture, and Momentum Fluxes in the Boundary Layer
Authors: Readings C. J. , Businger J. , Coantic M. , Mahoney A. R. , Naito K. 
Published: February 2008

As there are many techniques available for measuring these fluxes in the boundary layer, the group considered that it would be useful to start by discussing seven principal ones in turn.The vertical flux (or eddy transport) F of any atmospheric parameter ψ may be represented by

urn:x-wiley:00486604:media:rds178:rds178-math-0001
where w is the wind's vertical component, and the prime denotes the instantaneous deviation of the quantity from its mean value (e.g. w″ = w″ −
[Priestley, 1959]. It is important to choose the sampling rate and the observational period so that the required parts of the total flux spectrum are measured [Pasquill, 1962].
Budgets of Turbulent Fluctuations
Authors: Panofsky Hans A. , Atlas D. , Fehlhaber L. , Cermak J. E. 
Published: February 2008

The propagation of electromagnetic or acoustic waves through a turbulent, locally isotropic medium is prescribed, provided we know the coefficient of k−5/3 in the Kolmogorov law. This coefficient is the product of b, a universal constant; N, the dissipation rate of the fluctuations of refractive index; and ϵ−1/3, where ϵ is the rate of dissipation of turbulent velocity fluctuation into heat. We might consider two kinds of problems:How can electromagnetic or acoustic propagation information be used to get information about various meteorological properties?How can meteorological data be used to estimate the propagation of waves?
Foreword
Authors: Evans J. V. 
Published: February 2008

The Symposium on Planetary Atmospheres and Surfaces, held at Woods Hole, Massachusetts, August 11–15, 1969, was the successor to an earlier symposium held in May 1965 in Puerto Rico, whose proceedings were published in vol. 69D, no. 12 (1965) of Radio Science. Both meetings were organized through the initiative of Commission II of URSI (Radio Propagation in Non‐Ionized Media), who secured the sponsorship of URSI (International Union of Radio Science), the IAU (International Astronomical Union), and, in the case of this Symposium, of COSPAR (Committee on Space Research). Financial support for the Symposium was provided by URSI.Whereas the earlier symposium dealt almost exclusively with the results of radar and radio astronomy, the most exciting new results since then have been obtained by space research. Thus, in planning the new symposium the organizers sought to bring together workers in the two fields. This was deemed particularly important in the study of the moon, since it is now possible to determine how well radio and radar astronomy succeeded in describing the properties of the lunar surface prior to its physical investigation by use of landed vehicles. Based on such a comparison, one may be able to apply the radio techniques to planetary surface investigations with greater confidence. Accordingly, four sessions of the symposium were devoted to the moon, permitting extensive reviews of the results secured by the Ranger, Orbiter, and Surveyor vehicles. The organizers and chairmen of these sessions were: Dr. H. Masursky, U. S. Geological Survey; Dr. G. H. Pettengill, Arecibo Ionospheric Observatory; Dr. L. D. Jaffe, Jet Propulsion Laboratory; and Prof. Z. Kopal, University of Manchester. A highlight of the meeting was some preliminary reports on the results of the Apollo experiments. From the talks and lively discussion it would seem that, although there are matters of detail to be ironed out, we now have a good physical description of the surface properties of the moon and recognize that both external and internal processes have played a part in shaping them. However, considerable work has to be done before we may hope to understand the full history of the moon and its origin.
Radar‐Derived Statistics on Slant‐Path Attenuation at 10 GHz
Authors: Rogers R. R. 
Published: February 2008

Attenuation due to rain at 10 GHz over the radar line of sight has been measured automatically during the past three summer seasons. Data from five months were analyzed to give statistics on the frequency of occurrence, the extent in azimuth, the duration, and the dependence on elevation angle of 5‐ and 10‐db attenuation events. Results show that the frequency of occurrence diminishes rapidly as the elevation increases from horizontal to 10°, and is essentially constant from there on to 20°. 5 db is exceeded 10 hours per year at 3° elevation, 4 hours per year at 10°, and 3.5 hours per year at 20°. At all elevations 10 db is exceeded about one‐fifth as frequently as 5 db.The azimuth extents of attenuating rain regions vary from 1°, the narrowest extent measurable, to values exceeding 60°. At low elevations the distributions of azimuth extent are strongly peaked at the narrow end. With increasing elevation the distributions flatten. The average azimuth extent of a 5‐db region increases approximately linearly from 10° at an elevation of 3° to 33° at an elevation of 20°. For all elevations the average 10‐db extents are about half the 5‐db extents. The average duration of a 5‐db event decreases from about 30 min at near‐horizontal paths to less than 10 min at an elevation of 20°. For all elevations the average duration of a 10‐db event is about two‐thirds that of the 5‐db event. These results indicate the characteristics of rain attenuation to be expected over satellite‐to‐ground communication links for the Montreal area.
Transient Responses: Resonance Spikes of Topside Sounders: Summary Report
Authors: Petit M. 
Published: February 2008

In summarizing the discussions, the following statements appeared well established:At the plasma frequency, ƒN. The waves responsible for resonance signals are electrostatic in character. Their propagation vector k is directed nearly parallel to the magnetic field. These waves with frequency slightly greater than the plasma frequency do not exist in cold plasma theory, while in kinetic theory they appear inside the resonance cone.
VLF Emissions: Summary Report
Authors: Kimura I. 
Published: February 2008

In addition to a review on whistler mode propagation and VLF emissions, the introductory talk by M. J. Rycroft (University of Southampton, England) covered several recent topics, three of which were mostly discussed: (a) recent results of a ray tracing to be compared with Walter and Angerami's [1969] and Scarabucci's [1970] computations, (b) effect of thermal anisotropy on the real part of the refractive index, hence on raytracing, especially in plasmas with β = 1, (c) simultaneous rocket observation of electron flux (energies higher than 45 kev) and whistler‐mode noise intensity.The rest of this session was mainly devoted to generation mechanisms of VLF emissions; a few other topics such as an electrostatic instability in the magnetosphere were also included.
Excitation: Summary Report
Authors: Rawer K. 
Published: February 2008

Three short papers were read after the review paper by T. W. Johnston.P. E. Vandenplas (Ecole Royale Militaire, Brussels, Belgium) gave a survey concerning resonances observed in laboratory plasma capacitors. For such a capacitor with plate distance l and plates covered with rarified sheaths, cold plasma theory gives the main resonance of an infinite plane capacitor as a serial one at a frequency ƒN (1 − a/l)1/2, where a is the thickness of the (homogeneous) plasma sheath between the plates. In warm plasma theory apart from a correction term of the order λDe2/a2(λDe is electron Debye‐length) this resonance splits up into a narrow series of successive resonances, the distance of which is controlled by the same parameter. Furthermore, since the ‘warm’ dispersion equation is of fourth order now, other eigenvalues lead to new resonances of another type, which have been found in the laboratory also.
Radar Measurement of Ionosphere Motion in the Presence of Current‐Induced Spectral Asymmetries
Authors: Rino Charles L. 
Published: February 2008

The technique of measuring ionosphere motion from the shift in the incoherent‐scatter ion line has been known for some time. The underlying assumption in the adaptations of the technique applied so far is that there are no detectable current‐induced asymmetries in the spectrum. In the auroral zone this assumption can be violated during magnetospheric storms. To cope with this possibility we use an estimate of the first moment of the spectrum together with a matched‐filter‐like estimate.The first moment is the sum of the first moment of the unshifted spectrum plus the Doppler shift. The matched‐filter estimate, while not unaffected by asymmetries, tends to give an estimate closer to the Doppler shift. Hence, a difference between the two estimates is an indication of a current flowing in the range gate where the spectrum is measured. We assume that no other sources of asymmetry are present, although a large temperature gradient would have a similar effect. In principle the difference can be calibrated to give the magnitude of the current. This step is not yet completed owing to uncertainties in the composition of the ionosphere at low altitudes and a loss of frequency resolution due to the finite pulse length. The detectability of the currents by our method, however, is not affected by poor frequency resolution.Preliminary results from the Chatanika Auroral‐Zone Incoherent‐Scatter Radar are presented which show large velocities correlated in detail with simultaneous magnetometer data. Also an indication of a current flow has been observed in premidnight data taken on a very active night. An azimuth scan showed the sense of the current to be predominantly westward.
Some Aspects of the Day‐to‐Day Variability of the Equatorial Anomaly: American and Japanese Sectors
Authors: Rush C. M. , Miller D. 
Published: February 2008

The day‐to‐day variability observed in the structure of the equatorial anomaly during a period of high solar activity is investigated. Using hourly values of ƒ0F2 observed at a number of ionosonde locations in the American and Japanese longitude sectors during 1958, the structure of the equatorial F2 region has been obtained on an hourly basis for an entire year. It is observed that the equatorial anomaly shows considerable day‐to‐day fluctuations in both its structure and its diurnal development.The anomaly is generally best developed in the evening hours, and day‐to‐day changes in the time of best development are typically on the order of 2 to 4 hr. It is observed that the time when the anomaly attains its maximum development is not the same on both sides of the magnetic equator, although this time is closer to coincidence during the equinoctial months than during the solstices. Also during the equinoctial months, the anomaly crests tend to be more symmetric about the equator than during the solstices. The relative magnitudes of the crests display a noticeable changeover with time during the northern solstice in both longitude sectors. The crest on the winter side of the magnetic equator is larger during the day, and the summer crest is larger at night. The exact time that this changeover occurs varies on the order of 5 to 7 hr on a day‐to‐day basis. During the southern solstice this crest changeover is observed only in the Japanese sector.
Commission 3. On the ionosphere
Authors: Schmerling E. R. 
Published: February 2008

This session was chiefly concerned with the chemical and dynamical factors that are now known to control the distribution of electrons in the D region. The current status of knowledge of the electron‐density profile in the D region was reviewed by G. C. Reid (USA), with emphasis on the diurnal and seasonal variations and on the rapid changes that occur during sunrise. With regard to the overall electron ‘budget’ of the region, it was pointed out that important discrepancies between theory and observation still remain and that we are not yet certain whether these result from imperfect knowledge of production rates or of loss mechanisms, or from a combination of both.L. Thomas (UK) reviewed the current status of knowledge of the ion chemistry of the D region. A central feature of this is the formation of heavy, water‐cluster, positive ions, and although a satisfactory mechanism for producing these ions from O2+ has been known for some time, we still do not know the mechanism involved in the case of NO+, the dominant primary ion species. With regard to negative ions, the need for definitive measurements of composition was emphasized, because the existing measurements show major disagreements. Laboratory measurements of photodetachment cross sections are also urgently needed, particularly for such species as NO3−, CO4−, and their hydrates, since model calculations indicate that these should be the dominant species in the D region.
Studies of the blood‐brain barrier: Preliminary findings and discussion
Authors: Frey Allan H. 
Published: February 2008

The tasks I have been assigned as a discussant are, first, to discuss results of my current experimentation that extends my earlier blood‐brain barrier work as it bears upon the work presented by the panelists. Second, I am to comment on the work presented by the various panelists.I will briefly sketch three of my current experiments. One concerns the effect of microwave energy on the blood‐vitreous barrier of the eye. Another is concerned with the possibility of passage of dye through the placental barrier to the fetus. The third is concerned with the possibility of low‐intensity microwave energy enhancing the passage of cancer chemotherapeutic substances through the blood‐brain barrier.
Correction to “Magnetic elliptical polarization of Schumann resonances”
Authors: Sentman D. D. 
Published: February 2008

In the paper “Magnetic elliptical polarization of Schumann resonances” (Radio Science, 22(4), 595–606, 1987), two typographical errors appear. The right‐hand side of equation (1) should be preceded by a plus sign instead of a minus sign, and the right‐hand side of equation (6) is missing a factor of 1/sin (θ). However, the entries in Table 1 are tabulated from the correct expressions, and subsequent conclusions are unaffected.The author regrets the errors.
Über die tägliche Periode des Erdmagnetismus und der erdmagnetischen Störungen an polarstationen
Authors: Lüdeling Von Dr. G. 
Published: February 2008

In seiner Abhandlung “Zur Theorie des Erdmagnetismus”1 weist Herr von Bezold nochmals auf die seiner Zeit schon von Gauss und in neuerer Zeit auch von Anderen, wie den H. H. A. Schuster und Ad. Schmidt betonte Wichtigkeit hin, an Stelle der Declination und Horizontal‐Intensität die Componenten der erdmagnetischen Kraft in der horizontalen Ebene und ihre Variationen zu betrachten.Bezeichnet man die Componenten mit X und Y und zwar so, dass X die Nord‐Süd‐Componente, Y die Ost‐West‐Componente darstellt (wobei die Richtungen nach Nord und Ost positiv gerechnet sind), bedeuten ferner ΔX und ΔY die Variationen dieser Componenten, so lassen sich die beiden Variationen der Componenten zu einer Resultante vereinigen. Indem man für die 24 Stunden des Tages derartige, aus den Variationen der Componenten sich ergebende Resultanten nach Grösse und Richtung an einen festen Anfangspunkt legt, erhält man durch die Verbindung der Endpunkte der Resultanten eine geschlossene Curve. Solche Curven, die Herr von Bezold “Vectordiagramme” nennt, sind zwar schon von Gauss empfohlen und später auch von Lloyd, Airy und Anderen construirt und benutzt worden, doch hat man ihnen jedenfalls nicht diejenige Bedeutung zugelegt, die ihnen wohl ohne alle Frage für die Untersuchung der täglichen Periode der erdmagnetischen Erscheinungen zukommt. Das mag zu nicht geringem Theile dem Umstände zuzuschreiben sein, dass die zuletzt genannten Forscher die Diagramme nicht nach dem astronomischen, sondern nach dem magnetischen Meridian orientirt haben. In Folge dessen lassen sich aber die Componenten X und Y nicht unmittelbar aus ihnen entnehmen. Auch verhüllen sich dadurch recht wesentliche Eigenthümlichkeiten derselben, so z. B. die Thatsache, dass unter der Annahme eines in sich gleichbleibenden, im Laufe des Tages die Erde umkreisenden Systems von Kräften diese Diagramme für alle Punkte eines und desselben Parallelkreises dieselbe Gestalt und Lage haben müssen. Das Gleiche gilt von dem Zusammenhange zwischen der mittleren Zeit des Durchganges des Vectors durch den magnetischen Meridian und der mittleren Declination, u. s. w.