Enforcing the climate change act

This paper examines the enforceability of the duties in the Climate Change Act 2008 which require the UK’s GHG emissions to be reduced over time. Section B highlights how the Act’s other provisions must be interpreted so as to give proper support to these duties. The paper goes on, in Section C, to dispute objections that have been made to the duties’ enforceability – on the grounds that they are ‘target duties’ or ‘non-justiciable’– and argues that the courts can enforce them provided they adopt the amplified role which this new kind of duty requires; by seeking to forge effective but appropriate remedies. Section D suggests what form these remedies might take. Final conclusions are described in Section E

Energy Prices Jump While Food Prices Show Modest Increases

The Consumer Price Index (CPI) is a measure of the average change over time in the prices paid by urban consumers for a market basket of consumer goods and services. Produced monthly by the Bureau of Labor Statistics (BLS), the CPI uses a “market basket,” or a sample of goods and services that consumers purchase for day-to-day living, and weighs each item on the basis of the amount of spending reported by a sample of families and individuals. Widely used as a measure of inflation, the CPI provides information about price changes in the nation’s economy and can be used by government, business, labor, and private individuals as a guide to making economic decisions. Over the last 12 months, the index for all items less food and energy has slowly accelerated. In contrast, the all-items index has decelerated since a 12-month increase of 3.9 percent in September 2011. The September 2011 increase capped a run of steady acceleration in the all-items index that began in December 2010. Despite the contrast, the all-items index increased at a higher rate than the index for all items less food and energy in the first quarter of 2012. This summary compares price changes in the CPI for detailed categories of goods and services over the first quarter of 2012 with those in 2011

Measurements of accretion disc corona size in LMXB: consequences for Comptonization and LMXB models

We present results of measurements of the radial extent of the accretion disc corona in low mass X-ray binaries. These results prove conclusively the extended nature of the ADC, with radial extent varying from 20,000 km in the faintest sources to 700,000 km in the brightest, a substantial fraction of the accretion disc radius, typically 15%. This result rules out the Eastern model for LMXB which is extensively used, in which the Comptonizing region is a small central region. The ADC size depends strongly on the 1 - 30 keV source luminosity via a simple relationship r_ADC = L^{0.88 +/- 0.16} (99% confidence) close to a simple proportionality. We also present limited evidence that the ADC size agrees with the Compton radius r_C, or maximum radius for hydrostatic equilibrium. The results are consistent with models in which an extended ADC is formed by illumination of the disc by the central source. The dependence on luminosity may reflect the known decrease of coronal temperature as the source luminosity increases leading to an increase of r_C. The extended nature of the ADC means that the seed photons for Comptonization must consist of emission from the disc to the same radial extent as the corona, providing copious supplies of soft seed photons. We demonstrate the importance of the size of the ADC to the correct description of Comptonization, and derive the Comptonized spectrum of a LMXB based on thermal Comptonization of these seed photons and show that this differs fundamentally from that of the Eastern model which assumes a cut-off below 1 keV. Finally, we argue that our results are inconsistent with the assumption often made that the X-ray emission of accreting Black Holes and Neutron Stars has a common mechanism depending on the properties of the accretion flow only.Comment: 9 pages, 5 figures, MNRAS in press - final versio

A model for the Z-track phenomenon in GX 5-1 and observational evidence for the physical origins of the kHz QPO

We present results of a combined investigation of the spectral and kHz QPO evolution around the Z-track in GX 5-1 based on high-quality RXTE data. The Extended ADC emission model provides very good fits to the spectra, the results pointing clearly to a model for the nature of the Z-track, in agreement with previous results for the similar source GX 340+0. In this model, at the soft apex of the Z-track, the mass accretion rate Mdot is minimum and the neutron star has its lowest temperature; but as the source moves along the normal branch, the luminosity of the Comptonized emission increases, indicating that Mdot increases and the neutron star gets hotter. The measured flux f of the neutron star emission increases by a factor of ten becoming super-Eddington, and we propose that this disrupts the inner disk so forming jets. In flaring, the luminosity of the dominant Comptonized emission from the ADC is constant, while the neutron star emission increases, and we propose for the first time that flaring consists of unstable nuclear burning on the neutron star, and the measured mass accretion rate per unit area mdot at the onset of flaring agrees well with the theoretical critical value at which burning becomes unstable. There is a striking correlation between the frequencies of the kHz QPO and the ratio of the flux to the Eddington value: f/f_Edd, suggesting an explanation of the higher frequency QPO and of its variation along the Z-track. It is well known that a Keplerian orbit in the disk at this frequency corresponds to a position some distance from the neutron star; we propose that the oscillation always occurs at the inner disk edge, which moves radially outwards on the upper normal and horizontal branches as the measured increasing radiation pressure increasingly disrupts the inner disk.Comment: Astronomy and Astrophysics, in pres

The Gettier Problem

In this chapter, we will explore the luck at issue in Gettier-styled counterexamples and the subsequent problem it poses to any viable reductive analysis of knowledge. In the 1st section, we will consider the specific species of luck that is at issue in Gettier counterexamples, then, in the next section, I will briefly sketch a diagnosis of the Gettier Problem and try to explain why the relevant species of luck has proven to be extremely difficult to avoid. And finally, I will consider a prominent objection to the proposed diagnosis of the Problem

The emission regions in X-ray binaries: dipping as a diagnostic

X-ray dipping in the black hole binary Cygnus X-1, the Galactic jet source GRO J1655-40 and in low mass X-ray binaries is discussed. It is shown that spectral analysis strongly constrains emission models. Measurement of dip ingress/egress times allows the sizes of extended emission regions to be determined, notably for the Accretion Disk Corona which is responsible for Comptonization in X-ray binaries. In LMXB, the radius of the ADC is shown to be between ~ 10^9 and ~ 5x10^10 cm, an appreciable fraction of the accretion disk radius. This is inconsistent with Comptonization models requiring a localized Comptonizing region, for example, in the immediate neighbourhood of the neutron star. Results from a survey of LMXB using ASCA and BeppoSAX reveal an approximate equality between the height of the blackbody emission region on the neutron star and the height of the inner radiatively-supported disk, suggesting either that there is a direct causal link, such as a radial accretion flow between the inner disk edge and the star, or an indirect link, as in the case of accretion flow creep on the surface of the neutron star as suggested by Inogamov & Sunyaev. Finally, the survey shows that the blackbody cannot originate on the accretion disk as the required inner radii in many sources are substantially less than the neutron star radius.Comment: solicited review paper presented at COSPAR 2000 "X-ray and Gamma-ray Signatures of Black Holes and Weakly Magnetized Neutron Stars"; accepted for publication in Advances in Space Research (2nd affiliation added

The evolution of the Australian Defence Force Gap Year program

Through the Australian Defence Force Gap Year program and the preceding Ready Reserve scheme, Australian school-leavers have had the opportunity to experience full-time military training without the obligations of longer-term initial periods of service. This paper analyses these programs, assessing their respective characteristics, identifying both supporters and detractors, and highlighting various challenges. Introduction During the 2013 federal election campaign, the Coalition’s Policy for Stronger Defence contained a pledge to re‑build the ADF Gap Year program. In advocating this initiative, the Coalition argued that the ADF Gap Year ‘has been an effective community engagement and recruitment tool’ and has ‘proven successful in attracting more women to join the ADF and in bolstering the Army Reserve generally’. Subsequently on 28 April 2014, Assistant Minister for Defence, Stuart Robert, officially launched a reinstated version of the ADF Gap Year program to commence in early 2015. Although the ADF Gap Year was a Howard (Coalition) Government initiative, the concept of giving Australian school-leavers the opportunity for 12 months full-time training in the ADF dates back to the early 1990s, when the Australian Labor Party (ALP) enacted the Ready Reserve scheme. This Research Paper will analyse both the Ready Reserve scheme and subsequent Gap Year program; assessing their respective characteristics, identifying both supporters and detractors, and highlighting various challenges