bluuebunny/crossref_metadata_2025 huggingface dataset:
Spatial Distribution of Far Infrared and Radio Continuum Emission in Spiral Galaxies
Authors: Mayya Y.D. , Rengarajan T.N.
Published: July 2016

A study of 8 nearby spiral galaxies (NGC 2903, 3079, 3198, 3628, 4303, 4321, 4656 and 6946) is carried out using the radio continuum (RC) and far infrared (FIR) images at 1′ resolution. These images are used to study the radial gradients in the ratios of FIR to RC (Q60 and Q100), warm dust temperature (Td(60/100)) etc. The main results are illustrated with NGC 2903 as an example in Fig. 1, where azimuthally averaged quantities are plotted. Td(60/100) decreases away from the center (45–25 K), increasing again by ∼ 5 K in outer galaxies. Typically Q60 decreases by a factor of three away from the center in a given galaxy, but has an order of magnitude spread in the pixel values over all the galaxies. In contrast, Q100 shows flatter gradient, which is expected from the observed temperature gradient. 20 cm RC emission profile is also shown in Fig. 1. The RC and FIR profiles can be fitted by a combination of central gaussian and exponential disk components. In general RC and FIR have about the same fraction of exponential component with the exception of NGC 3628, in which the FIR is dominated by the gaussian while the RC is mostly disk component (see Fig. 2). In 5 of the remaining 7 galaxies, the exponential component contributes > 50% of the total. In general RC scale lengths are larger than the FIR.
Results of a Radio Continuum Survey of Spiral Galaxies at 10.55 GHz
Authors: Niklas S. , Wielebinski R. , Klein U. , Braine J.
Published: July 2016

The Revised Shapley-Ames Catalog (Sandage & Tamman, 1981) contains 335 spiral galaxies brighter than BT = 12. A subsample of these galaxies with δ ≥ –25° and total flux densities at 1.49 GHz (Condon, 1987) above 10 mJy were observed at λ2.8 cm using the 100-m radio telescope of the MPIfR Bonn. Depending on the expected flux density and extent of the source two observational methods were used: cross-scanning and mapping. In total, radio flux densities of 192 galaxies have been derived (Niklas et al., 1995). Additionally, a literature search was made in order to get flux densities at other frequencies.
Galaxy Evolution in Distant Clusters
Authors: Poggianti B.M. , Barbaro G.
Published: July 2016

A significant evolution has been detected in intermediate redshift clusters (z < 0.9), first by photometric studies ([1], [2]), which showed an excess of blue objects; subsequent spectroscopic studies revealed anomalies in most of the galaxies, mainly consisting of excessively strong Balmer lines. In order to explain the spectroscopic observations, bursts of star formation superimposed to the traditional scenario of galactic evolution are needed. The analysis of spectral lines and colours by means of an evolutionary synthesis model ([3]), including both the stellar contribution and the emission of the ionized gas, allows in most of the cases the determination of the time elapsed since the end of the burst and the fraction of galactic mass involved in it. In the clusters considered (AC103, AC114, AC118 at z = 0.31, [4]), the theoretical analysis demonstrates that the bursts affect substantial galactic mass fractions, typically 30 % or more. The observations can be equally well reproduced by either elliptical+burst models or by spiral+burst models in which the star formation is truncated at the end of the burst. The analysis of an UV colour such as (1550-V) is proposed as a valid method to distinguish between the two cases for Hδ strong red galaxies.
The Redshift Evolution of CIV in Galaxy Halos
Authors: Stengler Larrea E. A.
Published: July 2016

Improved and reliable profile fitting codes have made it recently possible to calculate reliable column densities of gas producing QSO absorption lines. Even using intermediate to low resolution spectra, the obtained column densities are very accurate, as has been extensively proved by Jenkins (1986). We applied this technique to the 131 CIV absorption systems in the survey by Sargent Boksenberg and Steidel (1988) and Steidel (1990). Since several lines were saturated, many CIV column densities, N(CIV), are only lower limits, and a survival analysis (Avni et al. 1980) is required to obtain the underlying redshift distribution of CIV column densities, which we present in Figure 1. Together with the number density distribution of strong (log N(CIV) ≥ 14.2) and weak systems shown in Figure 2, we have found that i. Both strong and weak systems become generally weaker below z ∼ 2, and II. Weak systems become less numerous below z ∼ 2, whereas the stronger systems grow steadily in number density down the lowest redshifts sampled. For details of the analysis, and on how this fits into a model for the CIV absorption systems see Stengler-Larrea et al. (1995, in preparation).
The Galaxy Populations of Clusters at High Redshifts: A “Hubble Atlas”
Authors: Trager S.C. , Faber S.M. , Dressler A. ,   The WF/PC-I Instrument Definition Team
Published: July 2016

We present first results of a Hubble Space Telescope imaging and a Palomar and Keck Observatories spectroscopy program of distant, rich galaxy clusters in the form of a “Hubble Atlas” of morphological types at z ≥ 0.75. Two clusters from the compilation of Gunn, Hoessel & Oke (1985) have been studied to date, Cl1322+3027 at z ≈ 0.76 and Cl1603+4313 at z ≈ 0.90.
Star Formation Histories of Spiral Galaxies from a Multi-Wavelength Study
Authors: Xu C.
Published: July 2016

We study the star formation histories of a sample of 113 nearby spiral galaxies using their radio continuum (20cm), FIR (40-120μm), H (1.65μm) and B (4400Å) luminosities. The first two are used as indicators of star formation rate over the past ∼ 108 years, as suggested by the tight and nearly universal FIR/radio correlation (Xu et al. 1994). Compared to other indicators of recent star formation rate such as Hα and UV, FIR and radio continuum have the advantage of being insensitive to extinction. The B luminosity is taken as star formation indicator for the time scale of 3 109 years, and the H luminosity for the time scale of 1010 years. We find:

1.

The long-term star-formation history (from a few billion years to the entire Hubble time), as indicated by the B-to-H luminosity ratio, depends strongly on the Hubble type.

2.

The recent star-formation history in the last a few billion years, as indicated by the radio-to-B luminosity ratio and the FIR-to-B luminosity ratio, does not depend on the Hubble type.

3.

Galaxies of a given Hubble type have similar long-term star-formation histories. On the other hand, their recent star-formation histories in the last a few billion years can be much different: the ratio between the star-formation rate averaged over the past 108 years to that over the past 3 109 years can be different by two orders of magnitude, as indicated by the scattering of the radio-to-B luminosity ratio and that of the FIR-to-B luminosity ratio. This is not likely to be due to the extinction on the B luminosity, because the scattering of the B-to-H luminosity ratio for a given type is much smaller.
A Molecular Worm in Scutum
Authors: Dame T. M.
Published: July 2016

Over the past four years, Pat Thaddeus and I have been using the CfA 1.2 m telescope to carry out a new CO survey of the first Galactic quadrant with a sensitivity per solid angle 3–10 times higher than previous CO surveys of the plane, and 16 times higher than the only previous extensive wide-latitude survey (Dame et al. 1987). Since a preliminary purpose of this survey is the study of molecular gas out of the plane in the inner Galaxy, the observations have so far been confined mainly to several vertical strips across the plane covering a few degrees in Galactic longitude and 6°–8° in Galactic latitude; details of this on-going survey are given in Dame & Thaddeus (1995).
FCRAO CO Survey of the Outer Galaxy
Authors: Heyer Mark H.
Published: July 2016

FCRAO has initiated an imaging survey of CO J=1–0 emission from the outer Galaxy to better understand the physical properties of the molecular gas component of the interstellar medium and to determine the relationship of this component to spiral arm features. When completed in Spring 1996, the CO Survey will cover 103° < lII < 145°, −3° < bII < 5°, and −150 < VLSR < 50 km s–1 with angular sampling of 50″ and velocity resolution of 0.8 km s–1. During the first year of observations, we have focused upon two fields with longitude ranges of 103° < lII < 112° and 131° < lII < 139°. The first field corresponds to the Cepheus region while the second field contains the W3, W4, and W5 complex of HII regions. To date, 700,000 CO spectra have been collected. In this contribution, we present preliminary results from the first year of observations.
Large-Scale Magnetic Structures Responsible for Coronal Disturbances
Authors: Bumba V. , Sýkora J.
Published: July 2016

In the first part of our communication, in a short summary of our recent results, it is demonstrated that over the last 15 years (the time interval for which the magnetic synoptic charts are available) the largest solar activity, usually connected with proton-flare occurrence, has been very closely related to a characteristic large-scale pattern in the magnetic field distribution with a life-time of the order of 8–10 solar rotations. These regular features are seen in the negative as well as in the positive polarity, although they can be seen better in the negative polarity where their forms are more pronounced, regardless of the activity cycle. The form alternates with the location in the northern or the southern solar hemispheres due to the mutual relations of both polarities, individual active regions, the influence of the differential rotations, the shift in longitude, etc. This pattern could be observed up to the large August 1972 proton-flare activity.

The large-scale magnetic patterns described are accompanied by characteristic large-scale features in the green (λ 5303) coronal emission, presented in the form of isophotes on the synoptic charts (reduced to a unified photometric scale).

In the second part of the presentation, preliminary results, concerning the correlation of the longitudinal distribution of the green coronal emission with the negative and the positive polarity fields for two time intervals (August 1960–September 1961 and January 1969–December 1969) are described. The existence of two ‘coronal active longitudes’ in both intervals, as well as the close relation of these longitudinal emission maxima to certain parts of the large-scale characteristic bodies of negative polarity, is discussed. Also, the existence of one heliographic longitude, connected with ‘coronal holes’ (minimal green corona emission), and its relation to the positive polarity large-scale pattern are proved.
Coronal Disturbances Observed in the Optical Emmission Lines
Authors: Waldmeier M.
Published: July 2016

Some examples are presented of fast variations of the structure and the intensity of coronal condensations. For the observations the lines λ 5303 and λ 5694 have been used. Most of the observed phenomena are flare-connected, but all of them are related to some kind of Hα-activity. Sudden brightening of the emission lines may occur after the disappearance of a filament. The events have a duration of up to several hours and consist of hot clouds of high density that are slowly rising from the upper chromosphere into the lower corona.
Forbidden Line Excitation Data for Certain Coronal Lines
Authors: Czyzak S. J. , Aller L. H. , Euwema R. N.
Published: July 2016

Plasma diagnostics of the active corona require data on transition probabilities and collision cross sections for relevant coronal emission lines. Atomic parameters pertaining to a number of coronal transitions have been derived as follows:
High Resolution Studies of Type III Solar Radio Bursts
Authors: Chiuderi C. , Giachetti R. , Mercier C. , Rosenberg H. , Slottje C.
Published: July 2016

(Solar Phys.). High spectral, temporal and spatial resolution observations were obtained with the 60-channel Utrecht solar radio spectrograph (160–320 MHz) and the 169 MHz Nançay solar radioheliograph. From a large number of type III bursts the average height was found to be 0.37 solar radius above the photosphere, corresponding to approximately the Newkirk streamer density, if the bursts are emitted at the harmonic of the local plasma frequency. No center-to-limb variation, nor east-west asymmetry was observed. All double bursts, double humped bursts, precursor-type III had exactly the same position and general shape for both members of the pair. From this it was concluded that fundamental-harmonic pairs are very rare at frequencies above 160 MHz (Mercier and Rosenberg, 1974).
Coronal Density Structures in Regions of Type III Activity
Authors: Leblanc Yolande , Kuiper Thomas B. H. , Hansen Shirley
Published: July 2016

(Solar Phys.). We identify from daily K-corona observations the coronal regions located above type III burst sources. The radio observations were made with the east–west log-periodic array at Clark Lake Observatory. East–west positions of 260 isolated type III bursts during March and April 1971 have been measured between 20 and 65 MHz (disregarding storms of type III bursts). The K-corona observations are made with the HAO K-coronameter at Mauna Loa, Hawaii. During 1971, the heights of observation were 3.6′, 5′, 9′ and 13′ above the limb.
Paired Type III Bursts
Authors: Caroubalos C. , Heyvaerts J. , Pick M. , Trottet G.
Published: July 2016

Radioheliographic observations of type III bursts occurring by pairs in a repetitive fashion were made with the high time resolution E–W Nançay Radio heliograph (169 MHz). The data were available in digitized form with a rate of 25 E–W profiles per second. The study is based on two days of observations: for the first one (January 14, 1971) the radio source was at 16′W and for the second one (June 29, 1971) at only 4′W.
A Theory of Type I Solar Radio Bursts
Authors: Sy W. N.-C.
Published: July 2016

(Proc. Astron. Soc. Australia). A theory is developed to account for the observed properties of type I storm bursts in terms of plasma radiation – that is, electromagnetic radiation at the electron plasma frequency resulting from the non-linear scattering of electron plasma waves on plasma ions. Now the average brightness temperature of a type I source is greater than 109 K, or even higher if, because of coronal scattering, the apparent source size is larger than the true source size. For brightness temperatures as high as 109 K the non-linear scattering must be of the induced kind in which electromagnetic radiation below the frequency of the electron plasma waves is amplified. For such radiation to be strongly circularly polarized in the o-mode, as observed in type I bursts, requires that the amplification be more effective in the o-mode than in the x-mode (Figure 1). This is found to be so for plasma waves excited by electrons travelling parallel to the magnetic field. The electric field of the plasma waves is then also parallel to the magnetic field. The non-linear scattering is more efficient for that magnetoionic mode which has the greater component of electric field in the same direction. This mode is the o-mode.
X-Ray Evidence for the Acceleration, Containment, and Emission of High Energy Flare Particles
Authors: Frost Kenneth J.
Published: July 2016

An instrument aboard the Fifth Orbiting Solar Observatory has observed hard solar X-rays from January 1969 to May 1972. A large number of X-ray bursts generated by solar cosmic ray flares have been observed. The X-ray bursts consist, in general, of two non-thermal components. The earliest occurring non-thermal component, coincident with the explosive phase, consists of a group of one to about ten X-ray bursts that are, for each burst, approximately 10 s duration and symmetrical in rise and decay. The time structure and multiplicity of these bursts is remarkably similar to that found in type III radio bursts in the meterwave band. The spectra of these bursts steepens sharply at energies greater than 100 keV indicating a limit at this energy for electron acceleration during the explosive or flash phase of the flare. For several flares these multiple X-ray bursts have occurred in coincidence with a group of type III bursts.
Particle Acceleration in Solar Flares
Authors: Sturrock P. A.
Published: July 2016

A review of observational data supports the proposal that there are two distinct phases of particle acceleration in solar flares. ‘Phase 1’ is associated with the flash phase and is here interpreted as acceleration during field-line reconnection. ‘Phase 2’ is associated with type II and type IV radio bursts, and is ascribed to stochastic acceleration in the turbulent plasma behind a magnetohydrodynamic shock formed ahead of an ejected plasmoid.
1. Magnetic fields in astrophysics
Authors: Van De Hulst H. C.
Published: July 2016

This symposium is held under the auspices of the International Astronomical Union at the department of electronics of a technical university. This combination of astronomy and technical electronics has already become so familiar, that it hardly strikes us as peculiar. This shows how strongly the case for electric and magnetic phenomena in a wide variety of astrophysical problems has been proven. However, all of this is comparatively recent history. One glance at an older epoch may illustrate this point and, perhaps, may help us to take fewer things for granted during our discussions.
3. A fluid self-excited dynamo
Authors: Davis Leverett
Published: July 2016

The possibility that a simply connected perfectly conducting fluid body could generate an increasing external magnetic field by acting as a self-excited dynamo is demonstrated by exhibiting a cycle of motions that doubles the external field each cycle. The essential feature of the motion is that interior points become surface points. This requires points which were originally adjacent to become widely separated. The possibility of such motions is demonstrated and some of the conditions that might lead to their development are considered.
7. Experimental work at the university of chicago on the onset of thermal instability in a layer of fluid heated from below
Authors: Nakagawa Yoshinari , Prendergast Kevin H.
Published: July 2016

This paper will summarize the experimental work at the University of Chicago on the problem of the onset of thermal instability in a layer of fluid heated from below. The purpose of this work has been to test certain theoretical predictions of the Rayleigh number at which instability sets in, and to determine the type of instability which appears at the critical point. The earlier experiments of this series were done at the hydrodynamics laboratory of the University of Chicago in connexion with a program of meteorological reseach[1, 2, 3, 4]. The current work is being done at the newly organized hydromagnetics laboratory of the Enrico Fermi Institute of Nuclear Studies. This laboratory utilizes the magnet of the old Chicago cyclotron, with pole pieces 92·7 cm in diameter and a gap of 22·1 cm. The magnet was reconstructed to allow the field strength to be varied from 0 to 13,000 gauss; the field is uniform to better than 1 % over the experimental area. The new laboratory is under the administrative supervision of Professors S. K. Allison and S. Chandrasekhar; the experiments are being done by Y. Nakagawa. The theoretical investigations are primarily the work of Chandrasekhar[5, 6, 7, 8, 9, 10] and it will be convenient to review some of his results before discussing the experiments.
8. Ionized gas in a magnetic field
Authors: Schlüter A.
Published: July 2016

The ionized gas is described as a mixture of several fluids; each obeying a quasi-hydrodynamic equation of motion with additional terms describing the mechanical interaction. Particularly, two- and three-fluid models are considered. The nature of the approximations (‘quasi-neutrality’, ‘creeping diffusion’) is discussed. Conservation-laws are formulated for the case of negligible effect of mutual encounters and of pressure diffusion. These models lead to a generalization of Ohm's law; it is shown that the additional terms are of practical importance if one has three components, of which one may be neutral.
12. Solar electrodynamics
Authors: Cowling T. G.
Published: July 2016

A historical account of the subject's development is attempted. Prior to 1940, the most significant papers were those by Larmor (1919) and Cowling (1934) on dynamo theories of solar fields: by Kiepenheuer (1935) on the corona; and by Ferraro (1937) on isorotation. These indicated the importance of electromagnetic forces and were groping towards the idea of frozen-in fields. The latter idea was, however, not clearly stated before Alfvén's 1941–2 papers.

Theory since then is divided into sections concerned with mechanical effects of magnetic fields, theories of sunspots, and the nature and origin of solar magnetic fields. The first includes theories of magnetic control of support of coronal filaments and prominences (van de Hulst, Alfvén, Dungey) and theories of magnetic influence on sunspot equilibrium. The second includes Alfvén's and Walén's theories of the solar cycle, and Biermann's explanation of sunspot coolness in terms of magnetic inhibition of convection. Sunspot theories, being discussed more fully by Biermann, are considered only briefly.

Electromagnetic heating covers theories of coronal heating and flares, discharge phenomena, particle acceleration and radio emission. Many of the older theories (Alfvén's on coronal heating, Giovanelli's on flares, that of Bagge and Biermann on cosmic rays) are set aside because of their neglect of self-induction effects and inadequacy of the mechanism of conversion. The relative motion of charged particles and neutral atoms (Piddington, Cowling) is described as supplying a powerful heating effect.

As regards the magnitude of the general solar magnetic field, it is suggested that the observed value can be discarded only if decisive reasons are given. Other theories having so far proved inadequate, dynamo theories of the origin of solar fields are regarded as the most promising. These can be partial, as when a toroidal field capable of explaining spot fields is supposed to be generated from the general field (Walén and others), or when a turbulent field is supposed to be generated from a smaller regular field (Alfvén and others): or total, when a simultaneous explanation of all fields is attempted (e.g. Parker). A general appraisal is made of the different theories.
16. Some effects of hydromagnetic waves in the solar atmosphere
Authors: Piddington J. H.
Published: July 2016

A hitherto undisclosed source of absorption of hydromagnetic waves, due to the presence of neutral atoms, is investigated quantitatively. In the chromosphere the rate of absorption due to this effect may be 1010 times greater than that due to ordinary viscosity.

General solar heating, due to hydromagnetic waves caused by granules, is investigated and order-of-magnitude agreement with observational data is found.

The new effect is discussed in connexion with heating near sunspots and with flares.
29. The internal constitution of sunspots
Authors: Schlüter A. , Temesváry S.
Published: July 2016

The constitution of stationary single sunspots of circular shape is considered. Account is taken of the mechanical effects of the magnetic field, including those which arise from the curvature of the lines of force. To make the system of magneto-hydrostatic equations manageable, it is assumed that the relative distribution of the vertical component of the magnetic field is the same across the flux-tube of the spot in all depths. Preliminary results indicate that suppression of convective energy transport by the magnetic field in those depths in which ionization of hydrogen takes place, will give the essential observable properties of sunspots, relatively independent on the asumptions about the physical processes in greater depths. There the physical properties of matter can deviate but very little from those of the indisturbed hydrogen convection zone.
31. On the theory of ionized interstellar gas motion
Authors: Terletzky J. P.
Published: July 2016

It is pointed out that the model of mutually penetrating ideal charged and neutral gases can be used with particular success to describe the motion of an extremely rarefied plasma. As a simplest instance of application of such a model, the acceleration of totally ionized gases in crossed electric and magnetic fields is considered. It is shown that the general solution of the problem in two limiting cases is either magneto-hydrodynamic or the free charge solution.
32. Interplanetary magnetic field
Authors: Alfvén H.
Published: July 2016

The magnetic field outside the sun (interplanetary magnetic field) is certainly far from a dipole field. A model of it has recently been suggested (Tellus,8, 1, 1956). This model is in agreement with cosmic ray and magnetic storm data and reconcilable with the coronal ray structure. Some possibilities to check the model are discussed.
33. The present state of the corpuscular theory of magnetic storms
Authors: Ferraro V. C. A.
Published: July 2016

The evidence in favour of a corpuscular theory of magnetic storms is briefly reviewed and reasons given for believing that the stream must be neutral but ionized and carry no appreciable current. It is shown that under suitable conditions the stream is able to pass freely through a solar magnetic field; the stream may also be able to carry away with it a part of this field. However, because of geometrical broadening of the stream during its passage from the sun to the earth, the magnetic field imprisoned in the gas may be wellnigh unobservable near the earth.

The nature, composition and dimensions of the stream near the earth are discussed and it is concluded that on arrival the stream will present very nearly a plane surface to the earth if undistorted by the magnetic field.

Because of its large dimensions, the stream will behave as if it were perfectly conducting. During its advance in the earth's magnetic field the currents induced in the stream will therefore be practically confined to the surface. The action of the magnetic field on this current is to retard the surface of the stream which being highly distortible will become hollowed out. Since the stream surface is impervious to the interpenetration of the magnetic tubes of force, these will be compressed in the hollow space. The intensity of the magnetic field is thereby increased and this increase is identified with the beginning of the first phase of a magnetic storm. This increase will be sudden, as observed, owing to the rapid approach of the stream to the earth.

The distortion of the stream surface is discussed and it is pointed out that two horns will develop on the surface, one north and the other south of the geomagnetic equator. Matter pouring through these two horns will find its way to the polar regions.

The main phase of a magnetic storm seems most simply explained as due to a westward ring-current flowing round the earth in its equatorial plane. Under suitable conditions such a ring-current would be stable if once set up. The mode of formation of the ring is, however, largely conjectural. The possibility that the main phase may be of atmospheric origin is also briefly considered. It is shown that matter passing through the two horns to the polar regions could supply the energy necessary for the setting up of the field during the main phase. The magnetic evidence in favour of such a hypothesis, however, seems wanting.
34. The present state of the electric field theory of magnetic storms and aurorae
Authors: Block L.
Published: July 2016

The main features of the electric field theory are outlined. The theory should be considered as a first approximation. The validity of the approximations and assumptions introduced is discussed.

Some model experiments on the theory are described. It is impossible to construct an entirely true model of nature in the laboratory. The similarities and differences between nature and model are discussed.

The mechanism of the model seems to be described very well by the theory. Some experimental results, which because of the complicated phenomena cannot be predicted by the theory, are compared with observations in nature. As far as we can see at present, the agreement between nature and model is astonishingly good.
36. The 27-day variation in cosmic ray intensity and in geomagnetic activity
Authors: Forbush Scott E.
Published: July 2016

The amplitude of the average 27-day wave in cosmic ray intensity, at Huancayo, Peru, and its phase relative to that for the 27-day wave in international magnetic character figure (ICF) is determined from results of harmonic analysis of data for each of 246 intervals (or solar rotations) of 27 days. From these data, the variability of which is essential for tests of statistical significance, the amplitude of the average 27-day wave in cosmic ray intensity and its phase relative to that in geomagnetic activity is determined for each of three groups of solar rotations selected according to the average of the amplitudes of the 27-day waves in magnetic activity. A fourth group contained only 27-day intervals in which large cosmic ray decreases occurred. Relative to that in magnetic activity, the phase of the 27-day wave in cosmic ray intensity is found for the averages, to be the same for the four groups.

The maxima of the average cosmic ray waves occur about 1·5 days after the minima of the corresponding waves in ICF. In general, the amplitude of the average 27-day wave in cosmic ray intensity, in the co-ordinate system in which its phase is relative to that of the 27-day wave in ICF tends to be greater for the selected groups of rotations with larger average ICF amplitudes. For most years near sunspot minimum the amplitude of the 27-day cosmic ray wave does not differ significantly from zero.

Bartels found for 27-day waves in ICF the effective number of statistically independent 27-day waves for N successive solar rotations to be N/3; the number found for cosmic ray intensity is N/2. Thus, on the average the 27-day recurrence tendency is less for cosmic ray intensity than for magnetic activity.
41. The solar daily variation of the cosmic ray intensity
Authors: Elliot H. , Rothwell P.
Published: July 2016

Some recent measurements of the solar daily variation for cosmic rays incident from the east and west directions at 45° to the vertical in London are described. The results do not agree with those to be expected if the variation was due to a non-isotropic flux of primary particles entering the earth's magnetic field. This result is discussed in relation to other evidence and it is concluded that the daily variation is probably due to a modulation of the primary cosmic ray intensity in the earth's magnetic field.
47. Untersuchungen über impulsentladungen im zusammenhang mit der möglichkeit von kontrollierbaren thermonuklearen reaktionen
Authors: Artsimovich L. A.
Published: July 2016

Eine notwendige Voraussetzung für die Entstehung von thermonuklearen Reaktionen ist eine hohe Temperatur des Stoffes. Die ersten Spuren vom Entstehen solcher Reaktionen können wir bei der Erwärmung des Stoffes (Deuterium oder einer Mischung von Deuterium und Tritium) bis zu T ~ 106 zu entdecken hoffen. Aber nur bei T ~ 108 können die thermonuklearen Reaktionen als eine neue Energiequelle ein Interesse erwecken.
The sugar composition of fruits in the diet of spider monkeys (Ateles geoffroyi) in tropical humid forest in Costa Rica
Authors: Riba-Hernández Pablo , Stoner Kathryn E. , Lucas Peter W.
Published: July 2016

Spider monkeys (Ateles geoffroyi) detect sucrose at a threshold lower than any primate yet tested and prefer sucrose to glucose or fructose in laboratory tests. This preferential selection of sucrose led to the hypothesis that such acute discrimination is related to a diet of sucrose-rich fruits. Furthermore, it has been suggested that fruit sugars may be related to distinct guilds of vertebrate seed-dispersers. The objectives of this study were: (1) to test if spider monkeys select sucrose-rich fruits both within and among plant species and (2) to test the hypothesis that sugar concentration is related to bird, bat or monkey seed-dispersal syndromes. Data were collected from one troop of spider monkeys in south-western Costa Rica. Interspecific comparison of ingested fruits shows that spider monkeys consumed species with significantly higher concentrations of glucose and fructose than sucrose. Similarly, at the intraspecific level, food-fruits had significantly more fructose and glucose than non-food fruits, but no difference was found for sucrose. The three different sugar types were not correlated with the importance of the species in the diet based on the amount of time they spent consuming each species. Although sucrose concentrations were significantly higher in primate-dispersed species compared with those dispersed by other vertebrates, soluble carbohydrates in primate-dispersed fruits were principally composed of glucose and fructose. Neither fructose nor glucose concentrations showed significant differences across the three categories of seed dispersal.
VICTORIANS LIVE
Authors: Sussman Herbert
Published: July 2016

The Cult of Beauty

CATHERINE MAXWELL

Imitating the Inimitable: Performing Charles Dickens's Life in Recent British Theatre

BENJAMIN POORE

“Famous Men and Fair Women”: Pre-Raphaelitism and Photography Reconsidered

ANDREA WOLK RAGER

Jane Eyre2011

CAROLYN WILLIAMS
Copenhagen Natural Radiocarbon Measurements III, Corrections to Radiocarbon Dates Made with the Solid Carbon Technique
Authors: Tauber Henrik
Published: July 2016

In the Copenhagen I and II date lists radiocarbon dates for samples representing the late-glacial Aller⊘d oscillation and early Neolithic periods in Switzerland and Denmark were given. At the time of publication no account was taken of the dilution of the atmosphere with inactive carbon by the extensive combustion of fossil fuels since the Industrial Revolution (Suess, 1955), and of its influence on the dating results. This effect as measured by Suess amounted to 3.4% depletion in wood samples from the heavily industrialized east coast of the United States. Several later measurements have shown that the magnitude of this reduction in atmospheric C14concentration varies in different areas. The average universal decrease was calculated by Fergusson (1958) as 2.03 ± .15%. However, the magnitude of reported Suess effects may vary with the chosen reference sample as a result of periodic changes (de Vries effect) in the atmospheric C14concentration as found by de Vries (1958).
Copenhagen Radiocarbon Dates IV
Authors: Tauber Henrik
Published: July 2016

The following list includes samples from sites or sections described in archaeologic or geologic publications. Several others, already dated, will be published when the archaeologic and geologic investigations are concluded.
British Museum Natural Radiocarbon Measurements II
Authors: Barker H. , Mackey C. J.
Published: July 2016

The second series of radiocarbon measurements made at the British Museum Research Laboratory are reported in the following list. The equipment and method used remain the same as described in our first date list (Barker and Mackey, 1959) and, as stated there, the error terms are not based solely on counting statistics but are widened to include contributions of ±80 years for possible isotopic fractionation effects and ±100 years for the de Vries-effect. Ages are calculated on a half-life of 5568 ± 30 years.
University of Michigan Radiocarbon Dates V
Authors: Crane H. R. , Griffin James B.
Published: July 2016

The following is a list of radiocarbon dates obtained since the time of the preparation of Michigan list IV. The method of measurement and treatment of data are the same as those described in the introductions to lists III and IV.
Design scrying: an alternative aesthetics for synthetic biology
Authors: Armstrong Rachel
Published: July 2016

In 1911, Stéphane Leduc originally proposed that synthetic biology is a branch of synthetic chemistry that can offer a portfolio of design tools that broaden the possibilities of an aesthetics of life. In the production of generative fields that underpin the synthesis of living systems, lifelike materials may be transfigured and transformed without being constricted by naturalistic expectations. The role of ‘design scrying’ in this exploration is discussed particularly in the generation of images through the interface distortions that occur at the surfaces of ‘dark gels’. These non-deterministic images generating media enable discussion of the aesthetics of life that enable designers to venture beyond the conventions of representation in the natural sciences and synthetic biology, as it is currently practiced in scientific laboratory settings. The implications of this approach are considered through the possibility of using lifelike materials in the choreography of space where lifelike materials, trembling interfaces, and living technologies give rise to the emergence ‘soft living architectures’. These establish the possibility of the development of living spaces that possess some of the properties of living things but may not have the full status of being truly alive.
Family Finance: Value Creation and the Democratization of Cross-Border Governance
Authors: Kobrak Christopher
Published: July 2016

As Mira Wilkins has argued, there is a curious disconnect between business and financial history (Wilkins 2004). Whereas business history literature has rediscovered the importance of family business in many countries and in many sectors of contemporary commercial life, for example, little has been written about family banking as an alternative to joint-stock, management-run financial institutions. This lacuna is odd for many reasons. First, family banking is one of the best-known examples of family business in history. Second, family banks once played a much greater role in international investment banking than it does today. Third, some family financial institutions are still active (dominant) in certain market segments and countries. This paper will focus on how, when and why family banking lost its position in international (multinational) banking during the first few decades of the twentieth century. Although political upheaval and a widespread movement to reduce the power of private financial institutions undermined their businesses, family banks suffered, too, from America's maturing as a financial center. I will argue that this shift is connected with the increased importance of American markets and financial regulations, which, in the 1930s, deliberately steered financial transactions away from private dealings and toward transparent impersonal exchanges and capital markets with new forms of aggregated capital and individual investors, in which private banks were ill-suited to manage or at the least for which they had no special competitive edge. Using concepts drawn from an earlier paper on family businesses and relying mostly on secondary sources, this paper will further argue that in markets or market segments, such as Leveraged Buyouts, where uncertainty forms a greater part of the transactional environment, family banking still plays a significant role.
Reconsidering Japan's Underperformance in Pharmaceuticals: Evidence from Japan's Anticancer Drug Sector
Authors: Umemura Maki
Published: July 2016

Unlike its automobile or electronics industries, Japan's pharmaceutical industry did not become a global leader. Japan remains a net importer of pharmaceuticals and has introduced few global blockbuster drugs. Alfred Chandler argued that Japan's pharmaceutical firms remained relatively weak because Western firms enjoyed an insurmountable first first-mover advantage. However, this case study of the anticancer drug sector illustrates that Chandler's explanation is incomplete. Japanese medical culture, government policy, and research environment also played a substantial role in shaping the industry. In the 1970s and 1980s, these factors encouraged firms to develop little few effective drugs with low side effects, and profit from Japan's domestic market. But, these drugs were unsuitable to foreign markets with more demanding efficacy standards. As a result, Japan not only lost more than a decade in developing ineffective drugs, but also neglected to create the infrastructure necessary to develop innovative drugs and build a stronger pharmaceutical industry.
How valid is your case formulation? Empirically testing your cognitive behavioural case formulation for tailored treatment
Authors: Mumma Gregory H. , Fluck Jonathan
Published: July 2016

Although clinicians have used cognitive behavioural case formulations (CBCFs) to guide treatment for many years, the validity of the case formulation (CF) is rarely evaluated. Given the central role of the formulation in treatment planning, particularly for complex or comorbid cases, a straightforward method to empirically evaluate the validity of the CBCF could increase the effectiveness of a treatment plan tailored for a particular client. This article describes a step-by-step, person-specific approach to evaluating a CBCF that can be used for appropriate cases in a clinical practice or especially a clinical training setting. The evaluation focuses on discriminant validity of person-specific scales and constructs and patterns of predicted functional relationships between idiosyncratic cognitions and distress. The approach is illustrated with an adult seen in a training clinic who was diagnosed with generalized anxiety and recurrent major depressive disorders and who completed 28 brief end-of-day, individualized questionnaires. The clinician's CBCF hypotheses were empirically evaluated using mostly simple statistical analyses available in readily accessible worksheets. Intervention implications of the CF evaluation are discussed.
Crystal structure of mammalian acid sphingomyelinase
Authors: Gorelik Alexei , Illes Katalin , Heinz Leonhard X. , Superti-Furga Giulio , Nagar Bhushan
Published: July 2016

Acid sphingomyelinase (ASMase, ASM, SMPD1) converts sphingomyelin into ceramide, modulating membrane properties and signal transduction. Inactivating mutations in ASMase cause Niemann–Pick disease, and its inhibition is also beneficial in models of depression and cancer. To gain a better understanding of this critical therapeutic target, we determined crystal structures of mammalian ASMase in various conformations. The catalytic domain adopts a calcineurin-like fold with two zinc ions and a hydrophobic track leading to the active site. Strikingly, the membrane interacting saposin domain assumes either a closed globular conformation independent from the catalytic domain, or an open conformation, which establishes an interface with the catalytic domain essential for activity. Structural mapping of Niemann–Pick mutations reveals that most of them likely destabilize the protein’s fold. This study sheds light on the molecular mechanism of ASMase function, and provides a platform for the rational development of ASMase inhibitors and therapeutic use of recombinant ASMase.
Development and validation of a whole-exome sequencing test for simultaneous detection of point mutations, indels and copy-number alterations for precision cancer care
Authors: Rennert Hanna , Eng Kenneth , Zhang Tuo , Tan Adrian , Xiang Jenny , Romanel Alessandro , Kim Robert , Tam Wayne , Liu Yen-Chun , Bhinder Bhavneet , Cyrta Joanna , Beltran Himisha , Robinson Brian , Mosquera Juan Miguel , Fernandes Helen , Demichelis Francesca , Sboner Andrea , Kluk Michael , Rubin Mark A , Elemento Olivier
Published: July 2016

We describe Exome Cancer Test v1.0 (EXaCT-1), the first New York State-Department of Health-approved whole-exome sequencing (WES)-based test for precision cancer care. EXaCT-1 uses HaloPlex (Agilent) target enrichment followed by next-generation sequencing (Illumina) of tumour and matched constitutional control DNA. We present a detailed clinical development and validation pipeline suitable for simultaneous detection of somatic point/indel mutations and copy-number alterations (CNAs). A computational framework for data analysis, reporting and sign-out is also presented. For the validation, we tested EXaCT-1 on 57 tumours covering five distinct clinically relevant mutations. Results demonstrated elevated and uniform coverage compatible with clinical testing as well as complete concordance in variant quality metrics between formalin-fixed paraffin embedded and fresh-frozen tumours. Extensive sensitivity studies identified limits of detection threshold for point/indel mutations and CNAs. Prospective analysis of 337 cancer cases revealed mutations in clinically relevant genes in 82% of tumours, demonstrating that EXaCT-1 is an accurate and sensitive method for identifying actionable mutations, with reasonable costs and time, greatly expanding its utility for advanced cancer care.
Biopolymers form a gelatinous microlayer at the air-sea interface when Arctic sea ice melts
Authors: Galgani Luisa , Piontek Judith , Engel Anja
Published: July 2016

The interface layer between ocean and atmosphere is only a couple of micrometers thick but plays a critical role in climate relevant processes, including the air-sea exchange of gas and heat and the emission of primary organic aerosols (POA). Recent findings suggest that low-level cloud formation above the Arctic Ocean may be linked to organic polymers produced by marine microorganisms. Sea ice harbors high amounts of polymeric substances that are produced by cells growing within the sea-ice brine. Here, we report from a research cruise to the central Arctic Ocean in 2012. Our study shows that microbial polymers accumulate at the air-sea interface when the sea ice melts. Proteinaceous compounds represented the major fraction of polymers supporting the formation of a gelatinous interface microlayer and providing a hitherto unrecognized potential source of marine POA. Our study indicates a novel link between sea ice-ocean and atmosphere that may be sensitive to climate change.
Griffiths phase and long-range correlations in a biologically motivated visual cortex model
Authors: Girardi-Schappo M. , Bortolotto G. S. , Gonsalves J. J. , Pinto L. T. , Tragtenberg M. H. R.
Published: July 2016

Activity in the brain propagates as waves of firing neurons, namely avalanches. These waves’ size and duration distributions have been experimentally shown to display a stable power-law profile, long-range correlations and 1/f b power spectrum in vivo and in vitro. We study an avalanching biologically motivated model of mammals visual cortex and find an extended critical-like region – a Griffiths phase – characterized by divergent susceptibility and zero order parameter. This phase lies close to the expected experimental value of the excitatory postsynaptic potential in the cortex suggesting that critical be-havior may be found in the visual system. Avalanches are not perfectly power-law distributed, but it is possible to collapse the distributions and define a cutoff avalanche size that diverges as the network size is increased inside the critical region. The avalanches present long-range correlations and 1/f b power spectrum, matching experiments. The phase transition is analytically determined by a mean-field approximation.