CIVIC COMMUNITY APPROACHES TO RURAL DEVELOPMENT IN THE SOUTH: ECONOMIC GROWTH WITH PROSPERITY

The free market-based policies of the corporate community model have skewed economic development across the South. For many small, rural communities, the consequences of global capitalism have resulted in declining real wages, high underemployment, and increasing rates of income inequality. Backed by recent scholarship and grassroots movements that suggest both civic engagement and the presence of smaller-scale, locally controlled enerprises can help determine whether communities prosper or decline, this paper explores the links between social structure and rural development in the South. The goal is to expand our understanding of civic community theory as an alternative to the neoclassical economic model of development. Using a local problem-solving framework, we suggest that a departure from the traditional, neoclassical path of development is in order. We conclude that rural policy makers must establish a role for civic community in the rural development process if they wish to protect the welfare of workers and communities, while increasing the prospects of economic growth with prosperity.civic community, economic growth, rural development, social capital, Southern United States, Community/Rural/Urban Development, R11, O21, R58,

Gravitational Wave Hotspots: Ranking Potential Locations of Single-Source Gravitational Wave Emission

The steadily improving sensitivity of pulsar timing arrays (PTAs) suggests that gravitational waves (GWs) from supermassive black hole binary (SMBHB) systems in the nearby universe will be de- tectable sometime during the next decade. Currently, PTAs assume an equal probability of detection from every sky position, but as evidence grows for a non-isotropic distribution of sources, is there a most likely sky position for a detectable single source of GWs? In this paper, a collection of galactic catalogs is used to calculate various metrics related to the detectability of a single GW source resolv- able above a GW background, assuming that every galaxy has the same probability of containing a SMBHB. Our analyses of these data reveal small probabilities that one of these sources is currently in the PTA band, but as sensitivity is improved regions of consistent probability density are found in predictable locations, specifically around local galaxy clusters.Comment: 9 pages, 9 figures, accepted for submission in Ap

Crying and Attachment Style: The Role of Romantic Relationships

Crying is an attachment behavior that functions to elicit support from others (Nelson, 1998); the context in which the crying occurs is important in understanding whether it is adaptive or maladaptive (Hendriks & Vingerhoets, 2006). However, very little research has examined whether and how attachment style is associated with adult crying, and if this association might vary by an individual’s relationship status. Using a sample of 305 first-year college students and a series of hierarchical regressions, we examined the moderating effect of relationship status on the associations between attachment style (measured using the Revised Experiences in Close Relationships Scale; Fraley, Waller, & Brennan, 2000) and crying frequency and tendency. We found that attachment anxiety was positively associated with both crying frequency and tendency, whereas attachment avoidance was negatively associated with crying tendency. However, we found moderation effects only in the case of attachment avoidance; specifically, we found that attachment avoidance was associated with a lower frequency of crying and tendency to cry only for those individuals involved in romantic relationships. Attachment anxiety, on the other hand, was associated with greater crying frequency and tendency regardless of relationship status. These results demonstrate not only that crying may act as an attachment behavior, but also that the activation or deactivation of this particular attachment behavior may be dependent on the existence of a romantic attachment figure

Q^2 Evolution of Generalized Baldin Sum Rule for the Proton

The generalized Baldin sum rule for virtual photon scattering, the unpolarized analogy of the generalized Gerasimov-Drell-Hearn integral, provides an important way to investigate the transition between perturbative QCD and hadronic descriptions of nucleon structure. This sum rule requires integration of the nucleon structure function F_1, which until recently had not been measured at low Q^2 and large x, i.e. in the nucleon resonance region. This work uses new data from inclusive electron-proton scattering in the resonance region obtained at Jefferson Lab, in combination with SLAC deep inelastic scattering data, to present first precision measurements of the generalized Baldin integral for the proton in the Q^2 range of 0.3 to 4.0 GeV^2.Comment: 4 pages, 3 figures, one table; text added, one figure replace

Uncertainties in determining parton distributions at large x

We critically examine uncertainties in parton distribution functions (PDFs) at large x arising from nuclear effects in deuterium F2 structure function data. Within a global PDF analysis, we assess the impact on the PDFs from uncertainties in the deuteron wave function at short distances and nucleon off-shell effects, the use of relativistic kinematics, as well as the use of less a restrictive parametrization of the d/u ratio. We find that in particular the d-quark and gluon PDFs vary significantly with the choice of nuclear model. We highlight the impact of these uncertainties on the determination of the neutron structure function, and on W boson production and parton luminosity at the Tevatron and the LHC. Finally, we discuss prospects for new measurements sensitive to the d-quark and gluon distributions but insensitive to nuclear corrections.Comment: 37 pages, 13 figures. Final published versio

Unpolarized structure functions at Jefferson Lab

Over the past decade measurements of unpolarized structure functions at Jefferson Lab with unprecedented precision have significantly advanced our knowledge of nucleon structure. These have for the first time allowed quantitative tests of the phenomenon of quark-hadron duality, and provided a deeper understanding of the transition from hadron to quark degrees of freedom in inclusive scattering. Dedicated Rosenbluth-separation experiments have yielded high-precision transverse and longitudinal structure functions in regions previously unexplored, and new techniques have enabled the first glimpses of the structure of the free neutron, without contamination from nuclear effects.Comment: 21 pages, 9 figures; typo in Eq. (3) corrected, references added; to appear in J. Phys. Conf. Proc. "New Insights into the Structure of Matter: The First Decade of Science at Jefferson Lab", eds. D. Higinbotham, W. Melnitchouk, A. Thoma

Star Formation in the Field and Clusters of NGC 5253

We investigate the star formation history of both the bright star clusters and the diffuse `field star' population in the dwarf starburst galaxy NGC 5253 using STIS longslit ultraviolet spectroscopy. Our slit covers a physical area of 370 x 1.6 pc and includes 8 apparent clusters and several inter-cluster regions of diffuse light which we take to be the field. The diffuse light spectrum lacks the strong O-star wind features which are clearly visible in spectra of the brightest clusters. This discrepancy provides compelling evidence that the diffuse light is not reflected light from nearby clusters, but originates in a UV-bright field star population, and it raises the issue of whether the star formation process may be operating differently in the field than in clusters. We compare our spectra to STARBURST99 evolutionary synthesis models which incorporate a new low metallicity atlas of O-star spectra. We favor a scenario which accounts for the paucity of O-stars in the field without requiring the field to have a different IMF than the clusters: stellar clusters form continuously and then dissolve on ~10 Myr timescales and disperse their remaining stars into the field. We consider the probable contribution of an O-star deficient field population to the spatially unresolved spectra of high redshift galaxies. (Abridged)Comment: 26 pages, 10 figures, accepted for publication in Ap