As in many other countries, the eighties have seen the re-emergence of poverty as a political issue in Australia. Rising unemployment and the increased incidence of sole parenthood have put more children at risk of poverty, a development which has prompted increased policy concern. This paper presents estimates of the incidence and structure of poverty in Australia in 1981–82, 1985–86 and 1989–90, using the poverty standard developed by the Poverty Commission in the seventies. The estimates for 1989–90 are based on data generated from the 1986 Income Distribution Survey by a microsimulation model that allows for trends in demographic change, labour market participation and income during the second half of the eighties. The results indicate that the overall poverty rate has increased from 9.2 per cent in 1981–82 to 12.8 per cent in 1989–90. This is despite the fact that the incomes of many low income groups have increased in real terms, in many cases substantially. The reason for this apparent paradox is that the poverty standard is a relative one, and has thus itself been increased in line with average community incomes. One of the conclusions of the paper is that it may be necessary to reconsider the use of a relative poverty standard when assessing short-run trends in the extent of poverty.

A distinction is often made between magisterial and radical reformers in the early modern period, Luther and Thomas Müntzer being frequently taken as representatives of two quite different reformations, especially in regard to the understanding of Scripture and of the political realm. It can, however, be argued that the Reformation as a whole was radical, and that it is misleading to characterise one aspect of it as mainstream, another peripheral. The comparison between Müntzer and the Scottish reformer, John Knox, appears to support the contention that the chasm between the two camps is not unbridgeable.

The Oxford Dictionary of National Biography (ODNB), originally designated the New Dictionary of National Biography, was published in 2004 as a successor to the renowned Dictionary of National Biography (DNB), edited by Sir Leslie Stephen (1832–1904) and itself published in sixty-three volumes between 1885 and 1900, with supplements. All of the subjects in the old DNB were retained for the ODNB; new entries were commissioned for a significant proportion of the existing subjects (including almost all of those falling within the early medieval period); and of course the opportunity was taken to add entries for a large number of new subjects. In its print version, the ODNB occupies sixty volumes, though it is unlikely to be found in that form outside reference libraries; most importantly, it is also available online, to subscribing institutions, with search facilities and other useful features. Like its most distinguished predecessor, the ODNB is already well established as an invaluable academic resource.

We present and analyze spectra of the Type IIn supernova 1994W obtained between 18 and 202 days after explosion. During the first 100 days the line profiles are composed of three major components: (i) narrow P Cygni lines with absorption minima at −700 km s−1; (ii) broad emission lines with blue velocity at zero intensity ~ 4000 km s−1; (iii) broad, smooth, extended wings most apparent in Hα. These components are identified with the expanding circumstellar (CS) envelope [5], shocked cool gas in the forward postshock region, and multiple Thomson scattering in the CS envelope, respectively. The absence of broad P Cygni lines from the supernova (SN) is the result of the formation of an optically thick, cool, dense shell at the interface of the ejecta and the CS envelope. Models of the SN deceleration and Thomson scattering wings are used to recover the Thomson optical depth of the CS envelope, τT ≥ 2.5 during first month, its density (n ~ 109 cm-3) and radial extent, ~ (4 — 5) × 1015 cm. The plateau-like SN light curve, which we reproduce by a hydrodynamical model, is powered by a combination of internal energy leakage after the explosion of an extended presupernova (~ 1015 cm) and subsequent luminosity from circumstellar interaction. We recover the pre-explosion kinematics of the CS envelope and find it to be close to homologous expansion with outmost velocity ≈ 1100 km s-1 and a kinematic age of ~ 1.5 yr. The high mass (≈ 0.4 M⊙) and kinetic energy (≈ 2 × 1048 erg) of the CS envelope combined with small age strongly suggest that the CS envelope was explosively ejected only a few years before the SN explosion.