Prestigious Houses or Provisional Homes? The \u3ci\u3eghar\u3c/i\u3e as a Symbol of Kathmandu Valley Peri-Urbanism

Compared to the uniform brick architecture and contiguous courtyard structure of houses in the urban core of Kathmandu Valley cities, the houses of the growing urban periphery appear fragmented, disorganized, and unplanned. While critics attribute this haphazard growth to a site-then-services (house first, then infrastructure) approach of rural migrants, in this paper I consider it a result of an alternative formulation of planning generated by three-plus decades of economic and governmental liberalization. The practices of new homeowners in the periphery must be understood within the greater context of peri-urbanism controlled by a complex negotiation of brokers, contractors, housing companies, and neighborhood associations. I draw from the multiple expressions of what ‘ghar’ (house/ home) means to make sense of everyday life in a new neighborhood on the western edge of Kathmandu Valley. While ghar references the singular focus on building a prestigious house, it also indexes aspirations of neighborly cooperation and collective action to develop neighborhoods. Based on an ethnographic account of one family’s struggles to build a ghar, I track how such aspirations can unravel into debt, shame, and alienation, which ultimately produce a provisional sense of place in the city

Agglomeration Index Towards a New Measure of Urban Concentration

A common challenge in analyzing urbanization is the data. The United Nations (UN) compiles information on urbanization (urban population and its share of total national population) that is reported by various countries but there is no standardized definition of ‘urban’, resulting in inconsistencies. This situation is particularly troublesome if one wishes to conduct a cross-country analysis or determine the aggregate urbanization status of the regions (such as Asia or Latin America) and the world. This paper proposes an alternative to the UN measure of urban concentration that we call an agglomeration index. It is based on three factors: Population density, The population of a ‘large’ city centre and Travel time to that large city centre. The main objective in constructing this new measure is to provide a globally consistent definition of settlement concentration in order to conduct cross-country comparative and aggregated analyses. As an accessible measure of economic density, the agglomeration index lends itself to the study of concepts such as agglomeration rents in urban areas, the ‘thickness’ of a market, and the travel distance to such a market with many workers and consumers. With anticipated advances in remote sensing technology and geo-coded data analysis tools, the agglomeration index can be further refined to address some of the caveats currently associated with it.agglomeration index, urbanization, accessibility map, cost surface

Dynamics of Circumstellar Disks III: The case of GG Tau A

(abridged) We present 2-dimensional hydrodynamic simulations using the Smoothed Particle Hydrodynamic (SPH) code, VINE, to model a self-gravitating binary system similar to the GG Tau A system. We simulate systems configured with semi-major axes of either $a=62$~AU (`wide') or $a=32$~AU (`close'), and with eccentricity of either $e=0$ or $e=0.3$. Strong spiral structures are generated with large material streams extending inwards. A small fraction accretes onto the circumstellar disks, with most returning to the torus. Structures also propagate outwards, generating net outwards mass flow and eventually losing coherence at large distances. The torus becomes significantly eccentric in shape. Accretion onto the stars occurs at a rate of a few $\times10^{-8}$\msun/yr implying disk lifetimes shorter than $\sim10^4$~yr, without replenishment. Only wide configurations retain disks by virtue of robust accretion. In eccentric configurations, accretion is episodic, occurs preferentially onto the secondary at wrates peaked near binary periapse. We conclude that the \ggtaua\ torus is strongly self gravitating and that a major contribution to its thermal energy is shock dissipation. We interpret its observed features as manifestations of spiral structures and the low density material surrounding it as an excretion disk created by outward mass flux. We interpret GG Tau A as a coplanar system with an eccentric torus, and account for its supposed mutual inclination as due to degeneracy between the interpretation of inclination and eccentricity. Although the disks persist for long enough to permit planet formation, the environment remains unfavorable due to high temperatures. We conclude that the GG Tau A system is in an eccentric, $a\sim62$~AU orbit.Comment: Accepted for publication in the Astrophysical Journa

From Anecdote to Evidence: Assessing the Status and Condition of Arts Education at the State Level

Without solid evidence about the status and condition of arts education in the nation's public schools, it is difficult to make a convincing case for the arts. This research and policy brief draws on the experiences of five states -- Illinois, Kentucky, New Jersey, Rhode Island, and Washington -- as the basis for a discussion of various approaches and methodologies for conducting statewide arts education research

Linear perturbations in viable f(R) theories

We describe the cosmological evolution predicted by three distinct $f(R)$ theories, with emphasis on the evolution of linear perturbations. The most promising observational tools for distinguishing $f(R)$ theories from $\Lambda$CDM are those intrinsically related to the growth of structure, such as weak lensing. At the linear level, the enhancement in the gravitational potential provided by the additional $f(R)$ `fifth force' can separate the theories, whereas at the background level they can be indistinguishable. Under the stringent constraints imposed on the models by Solar System tests and galaxy-formation criteria, we show that the relative difference between the models' linear evolution of the lensing potential will be extremely hard to detect even with future space-based experiments such as {\it Euclid}, with a maximum value of approximately 4% for small scales. We also show the evolution of the gravitational potentials under more relaxed local constraint conditions, where the relative difference between these models and $\Lambda$CDM could prove discriminating.Comment: 14 pages, 16 figures. Version 3 with minor changes to match version published in Physical Review