In his Preface the author' says that he started out to review all the more important theories upon the topics ordinarily discussed under human motivation but soon found himself more and more limited to the presentation of his own point of view. This very well characterizes the book. It is a very personal product. It is an outline with some defense of the author's own thinking about instincts and appetites and sentiments and how they function in human behavior. And as the author draws so heavily upon James and McDougall, especially the latter, the book may well be looked upon as a sort of sequel to their efforts. There is a thought-provoking distinction presented between instinct and appetite. An instinct is said to be aroused always by something in the external situation; and, correspondingly, an appetite is said to be aroused by sensations from within the body itself. This places, of course, a heavy emphasis upon the cognitive factor in all instinctive behaviors; and the author prefers to use the cognitive factor, especially the knowledge of that end-experience which will satisfy, as a means of differentiating one instinct from another. In this there is a recognized difference from McDougall who placed more emphasis for differentiation upon the emotional accompaniment. The list of instincts arrived at by this procedure is much like that of McDougall, although the author is forced by his criteria to present the possibility of food-seeking and sex and sleep operating both in the manner of an appetite and also as an instinct. The Shand-McDougall concept of sentiment is taken over and used in the explanation of moral motivation. There is the development within each personality of a sentiment for some moral principle. But this sentiment is not a very powerful motivating factor. It is reinforced by social pressures and by religion, which is treated as an effort of finite man to live in harmony with the infinite reality. Those whose psychological thinking is largely in terms of McDougall will doubtless find this volume a very satisfying expansion; but those who are at all inclined to support their psychological thinking by reference to experimental studies will not be so well pleased. The James-Lange theory, for example, is discussed without mention of the many experimental studies which it has provoked. Theoretical sources appear in general to be preferred to experimental investigations.

Human MotivationThe Mind in Action: A Study of Motives and Values. A. Campbell Garnett

Many problems in the experimental estimation of parameters for models can be solved through use of the likelihood ratio test. Applications of the likelihood ratio, with particular attention to photon counting experiments, are discussed. The procedures presented solve a greater range of problems than those currently in use, yet are no more difficult to apply. The procedures are proved analytically, and examples from current problems in astronomy are discussed.

Parameter estimation in astronomy through application of the likelihood ratio. [satellite data analysis techniques

A life-span theory of development is presented that is based on the concepts of primary and secondary control. Primary control refers to behaviors directed at the external environment and involves attempts to change the world to fit the needs and desires of the individual. Secondary control is targeted at internal processes and serves to minimize losses in, maintain, and expand existing levels of primary control. Secondary control helps the individual to cope with failure and fosters primary control by channeling motivational resources toward selected action goals throughout the life course. Primary control has functional primacy over secondary control. An analysis of extensive and diverse literatures spanning infancy through old age shows that trade-offs between primary and secondary control undergo systematic shifts across the life course in response to the opportunities and constraints encountered. In this article, we present a life-span theory of development based on the concept of control. Research on life-span development has become an increasingly active area of inquiry in the last two decades and has the potential of yielding fundamental theories about the emergence and transformation of human behavior over the life course (e.g., P. B. Baltes, 1987). However, as noted by Birren and Bengtson (1988), the field of life-course development and aging is at present best characterized as data rich but theory poor. Most existing developmental theories embrace limited temporal and functioning domains. With the exception of personality theorists such as Erikson, Loevinger, Gould, and Levinson (see Cavanaugh, 1990; Schulz & Ewen, 1993), psychologists have made few attempts to develop lifespan theories of development, in part because such efforts require the integration of information from multiple domains, including the behavioral, social, and biological sciences. A second formidable challenge posed by such an undertaking is the problem of level of analysis. Ideally, such a theory should explain both macro-level behaviors such as major life-course decisions

http://psycnet.apa.org/journals/rev/102/2/284.pdf

A life-span theory of control.

Neutron Stars 1: Equation of State and Structure

Young massive clusters are dense aggregates of young stars that form the fundamental building blocks of galaxies. Several examples exist in the Milky Way Galaxy and the Local Group, but they are particularly abundant in starburst and interacting galaxies. The few young massive clusters that are close enough to resolve are of prime interest for studying the stellar mass function and the ecological interplay between stellar evolution and stellar dynamics. The distant unresolved clusters may be effectively used to study the star-cluster mass function, and they provide excellent constraints on the formation mechanisms of young cluster populations. Young massive clusters are expected to be the nurseries for many unusual objects, including a wide range of exotic stars and binaries. So far only a few such objects have been found in young massive clusters, although their older cousins, the globular clusters, are unusually rich in stellar exotica. In this review we focus on star clusters younger than $\sim100$ Myr, more than a few current crossing times old, and more massive than $\sim10^4$ \Msun, irrespective of cluster size or environment. We describe the global properties of the currently known young massive star clusters in the Local Group and beyond, and discuss the state of the art in observations and dynamical modeling of these systems. In order to make this review readable by observers, theorists, and computational astrophysicists, we also review the cross-disciplinary terminology.

/pdf/young-massive-star-clusters-1mlfusxprp.pdf

Young Massive Star Clusters

Accretion and Magnetic Field Decay in Neutron Stars Entering Binaries

Thin metallic films are commonly used in space industry. Important applications are e.g. multilayer insulation blankets (MLI) or solar sail membranes. In a sufficiently large distance from the Earth atmosphere, the solar wind and electromagnetic radiation are the dominating factors for material degradation. The solar protons while penetrating the metals recombine to neutral hydrogen atoms and then form molecular hydrogen bubbles. Their high concentration within the metals’ lattice has a direct influence on their physical properties.

Up to now, no material that was exposed to the interplanetary space conditions has been returned to Earth. Therefore, studies both theoretical and experimental carried out in the terrestrial laboratories are necessary to predict the changes in the mechanical and thermo-optical properties of the metals.

The aim is to present the basics behind formation processes of molecular hydrogen bubbles as well as their influence on physical properties of exposed metals to the solar wind. The other degradation mechanisms are discussed as well, e.g. the delamination processes caused by corpuscular radiation. Ideas of protection possibilities of the metals are drawn.

The experimental studies were performed by use of the Complex Irradiation Facility (CIF) of the DLR’s Institute of Space Systems in Bremen, Germany. The CIF’s linear proton accelerator allows to irradiate specimens to well defined proton fluxes. A series of experiments have been made to simulate the growth of the bubbles at different physical conditions which represent those at the interplanetary space.

The post-degradation studies of the exposed metallic films have been performed by use of an electron microscope and number of image-processing methods to analyze the morphology of the specimens. It has been proven that at the early stage of the bubble growth the average bubble radius R evolves according to R~t^1/3 law.

One of the consequences of the molecular hydrogen bubbles formation is a significant increase of the metallic surface roughness or changes of the samples’ thermo-optical properties. However, the bubble formation depends strictly on physical conditions at which the samples are exposed to the solar wind protons. Dependency on bubble formation mechanism due to temperature as well as proton kinetic energy is given.

Metallic Surfaces under Interplanetary Medium - Degradation Mechanisms and Protection Possibilities

We consider the expulsion of proton fluxoids along neutron vortices from the superfluid/superconductive core of neutron star with weak ($B<10^{10}$ G) magnetic field. The velocity of fluxoids is calculated from the balance of buoyancy, drag and crustal forces. We show, that the proton fluxoids can leave the superfluid core sliding {\it along} the neutron vortices on a timescale of about $10^7$ years. An alternative possibility is that fluxoids are aligned with the vortices on the same timescale. As the result, non--aligned surface magnetic fields of millisecond pulsars can be sustained for $\ga 10^9$ years only in case of a comparable dissipation timescale of the currents in the neutron star crust. This defines upper limits of the impurity concentration in the neutron star crust: $Q \la 0.1$ if a stiff equation of state determines the density profile.

/pdf/on-the-nature-of-the-residual-magnetic-fields-in-millisecond-3h47uu376h.pdf

On the Nature of the Residual Magnetic Fields in Millisecond Pulsars

The paper deals with a simple spherical mean-field dynamo model of $\alpha^2$-type in the case of high electrical conductivity. A spherically symmetric distribution of turbulent motions is assumed inside a spherical fluid body surrounded by free space, and some complete form of the corresponding mean electromotive force is taken into account. For a turbulence lacking reflectional symmetry finite growth rates of magnetic fields prove to be possible even in the limit of perfect conductivity, that is, the model corresponds to a fast dynamo. In accordance with the theorem by Bondi and Gold the dynamo-generated field is completely confined in the fluid body.

Ulrich Geppert

Papers

Accretion and Magnetic Field Decay in Neutron Stars Entering Binaries

Metallic Surfaces under Interplanetary Medium - Degradation Mechanisms and Protection Possibilities

On the Nature of the Residual Magnetic Fields in Millisecond Pulsars

Turbulent Dynamo Action and the High-Conductivity Limit: a Hidden Dynamo

The influence of impurities on the spin-lattice relaxation in some uniaxial ferroelectrics