A Panel Data Analysis of the Incidence and Impact of Over-education

This paper adds to the overeducation literature using panel data from the British Household Panel Survey. Much has been written about who is more likely to be overeducated, and the impact of being overeducated on wages, at particular points in time using cross-sectional data. Panel data allows us to control for unobserved individual heterogeneity in the determinants of incidence and impact of overeducation. The paper goes on to estimate the determinants of transitions out of overeducation, providing new information about its duration, and the factors that influence being in, and escaping from, this state

Is the Over-Education Wage Penalty Permanent?

Much has been written about the impact of over-education on wages using cross-sectional data, although there have been few studies that analyse the returns to over-education in a dynamic setting. This paper adds to the existing literature by using panel data to investigate the impact and permanence of over-education wage penalties, whilst controlling for unobserved individual heterogeneity. Our fixed effects estimates suggest that the over-education wage penalty cannot solely be explained by unobserved heterogeneity. Over-education is permanent for many workers since around 50 percent of workers over-educated in 1991 are still over-educated in 2005. However, we also show that these workers are of lower quality compared to around 25 percent who find a match within five years of being over-educated. Finally, there is a significant scarring effect for workers over-educated in 1991 since they never fully reach parity compared to those who were matched in 1991, although this is not the case for graduates who manage to find a match within 5 years

Process for the leaching of AP from propellant

A method for the recovery of ammonium perchlorate from waste solid rocket propellant is described wherein shredded particles of the propellant are leached with an aqueous leach solution containing a low concentration of surface active agent while stirring the suspension

Volunteer tourism: Evidence of cathartic tourist experiences

The study involved in-depth interviews with participants of an Australian non-government organization (NGO) that organizes projects in which young volunteers aged between 17 and 26 years from Australia and New Zealand participate in welfare projects with partner NGOs in developing countries. The welfare projects provide on the ground assistance to communities; these may not lead to longer-term sustainable development through longer-term skills training but engage the volunteers and community in a mutual exchange. Typically, participants will be engaged in short term courses in health and hygiene, micro-enterprise management skills, assisting in community health projects, community service with children with disabilities or orphans, painting, construction of school playgrounds and classrooms, guest teaching in schools, cultural exchange and disaster relief. The Australian NGO provides no financial assistance for participants; it primarily organizes and facilitates the travel, project and community work. Each project lasts between two and four weeks and are thus typically short-term in duration. As such, participants can be considered 'shallow volunteer tourists' (Callanan and Thomas 2005)

The Spectroscopic Footprint of the Fast Solar Wind

We analyze a large, complex equatorial coronal hole (ECH) and its immediate surroundings with a focus on the roots of the fast solar wind. We start by demonstrating that our ECH is indeed a source of the fast solar wind at 1AU by examining in situ plasma measurements in conjunction with recently developed measures of magnetic conditions of the photosphere, inner heliosphere and the mapping of the solar wind source region. We focus the bulk of our analysis on interpreting the thermal and spatial dependence of the non-thermal line widths in the ECH as measured by SOHO/SUMER by placing the measurements in context with recent studies of ubiquitous Alfven waves in the solar atmosphere and line profile asymmetries (indicative of episodic heating and mass loading of the coronal plasma) that originate in the strong, unipolar magnetic flux concentrations that comprise the supergranular network. The results presented in this paper are consistent with a picture where a significant portion of the energy responsible for the transport of heated mass into the fast solar wind is provided by episodically occurring small-scale events (likely driven by magnetic reconnection) in the upper chromosphere and transition region of the strong magnetic flux regions that comprise the supergranular network.Comment: 25 pages, accepted to appear in the Astrophysical Journal. Supporting movies can be found in http://download.hao.ucar.edu/pub/mscott/papers/ECH

Deciphering Solar Magnetic Activity: On Grand Minima in Solar Activity

The Sun provides the energy necessary to sustain our existence. While the Sun provides for us, it is also capable of taking away. The weather and climatic scales of solar evolution and the Sun-Earth connection are not well understood. There has been tremendous progress in the century since the discovery of solar magnetism - magnetism that ultimately drives the electromagnetic, particulate and eruptive forcing of our planetary system. There is contemporary evidence of a decrease in solar magnetism, perhaps even indicators of a significant downward trend, over recent decades. Are we entering a minimum in solar activity that is deeper and longer than a typical solar minimum, a "grand minimum"? How could we tell if we are? What is a grand minimum and how does the Sun recover? These are very pertinent questions for modern civilization. In this paper we present a hypothetical demonstration of entry and exit from grand minimum conditions based on a recent analysis of solar features over the past 20 years and their possible connection to the origins of the 11(-ish) year solar activity cycle.Comment: 9 pages - submitted to Frontiers in Solar and Stellar Physic

Gas-phase and heat-exchange effects on the ignition of high- and low-exothermicity porous solids subject to constant heating

This article investigates the ignition of low-exothermicity reactive porous solids exposed to a maintained source of heat (hotspot), without oxygen limitation. The gas flow within the solid, particularly in response to pressure gradients (Darcy’s law), is accounted for. Numerical experiments related to the ignition of low-exothermicity porous materials are presented. Gas and solid products of reaction are included. The first stage of the paper examines the (pseudo-homogeneous) assumption of a single temperature for both phases, amounting to an infinite rate of heat exchange between the two. Isolating the effect of gas production and flow in this manner, the effect of each on the ignition time is studied. In such cases, ignition is conveniently defined by the birth of a self-sustained combustion wave. It is found that gas production decreases the ignition time, compared to equivalent systems in which the gas-dynamic problem is effectively neglected. The reason for this is quite simple; the smaller heat capacity of the gas allows the overall temperature to attain a higher value in a similar time, and so speeds up the ignition process. Next, numerical results using a two-temperature (heterogeneous) model, allowing for local heat exchange between the phases, are presented. The pseudo-homogeneous results are recovered in the limit of infinite heat exchange. For a finite value of heat exchange, the ignition time is lower when compared to the single-temperature limit, decreasing as the rate of heat exchange decreases. However, the decrease is only mild, of the order of a few percent, indicating that the pseudo-homogeneous model is in fact a rather good approximation, at least for a constant heat-exchange rate. The relationships between the ignition time and a number of physico-chemical parameters of the system are also investigated

OSS-1/contamination monitor

A 20-cm high, 18-cm wide, and 30-cm long (8x7x12 inch) box weighing about 7 kg (15 lbs) and consuming about 7 watts of power was carried on the OSS-1 pallet to monitor the mass build-up or accretion of condensible, volatile materials on surfaces in the shuttle bay during all phases of ascent, on-orbit, and descent. Passively thermally controlled, the box holds two witness samples and four actively temperature controlled quartz crystal microbalances (TQCM) whose temperature can vary from -60 C to +80 C. Graphs show the accretion indicated by the TQCM during the launch and early orbital phase. Conditions during tail to the Sun, nose to the Sun, and bay to the Sun attitudes of the shuttle during STS-3 are reflected in temperatures indicated by the OSS-1 thermistor. These temperatures influence outgassing rates of various materials as well as measurements made by the contamination monitor package. The parameters that bear on TQCM measurements data are shown in graphs and discussed