Mythical Expectations

According to the conventional account, economists have relied on three types of expectations: static (contained in the original Keynesian Phillips curve); adaptive (introduced by Milton Friedman’s in the course of his Monetarist counter-revolution) and rational (part of Robert Lucas’s natural rate New Classical counter revolution). This chapter argues that there is a fourth expectational type: the myths associated with these natural rate counter revolutions. ISBN: 978140394959

The New Zealand Jury

In New Zealand, the recent history of the jury has been one of fairly steady decline. This is particularly so of the civil jury, which has become virtually extinct with little realistic prospect of revival

Hinode/Extreme-Ultraviolet Imaging Spectrometer Observations of the Temperature Structure of the Quiet Corona

We present a Differential Emission Measure (DEM) analysis of the quiet solar corona on disk using data obtained by the Extreme-ultraviolet Imaging Spectrometer (EIS) on {\it Hinode}. We show that the expected quiet Sun DEM distribution can be recovered from judiciously selected lines, and that their average intensities can be reproduced to within 30%. We present a subset of these selected lines spanning the temperature range $\log$ T = 5.6 to 6.4 K that can be used to derive the DEM distribution reliably. The subset can be used without the need for extensive measurements and the observed intensities can be reproduced to within the estimated uncertainty in the pre-launch calibration of EIS. Furthermore, using this subset, we also demonstrate that the quiet coronal DEM distribution can be recovered on size scales down to the spatial resolution of the instrument (1$"$ pixels). The subset will therefore be useful for studies of small-scale spatial inhomogeneities in the coronal temperature structure, for example, in addition to studies requiring multiple DEM derivations in space or time. We apply the subset to 45 quiet Sun datasets taken in the period 2007 January to April, and show that although the absolute magnitude of the coronal DEM may scale with the amount of released energy, the shape of the distribution is very similar up to at least $\log$ T $\sim$ 6.2 K in all cases. This result is consistent with the view that the {\it shape} of the quiet Sun DEM is mainly a function of the radiating and conducting properties of the plasma and is fairly insensitive to the location and rate of energy deposition. This {\it universal} DEM may be sensitive to other factors such as loop geometry, flows, and the heating mechanism, but if so they cannot vary significantly from quiet Sun region to region.Comment: Version accepted by ApJ and published in ApJ 705. Abridged abstrac

Mundell's International Economics: Adaptations and Debates

Most of the chapters in Mundell's International Economics differ, owing to adaptation, from the original sources. The revisions yield valuable insights into the contributions made by the initial publications. In this paper we look only at the changes that take the form of elisions of material. These outtakes are amusing but demonstrate how Mundell was willing to either irritate or ignore his discussants. Issues raised by them are important enough to warrant our further consideration. In doing so we question both the validity and the interpretation of some of the conclusions in the Nobel-cited capital mobility paper. Copyright 2005, International Monetary Fund

EUV spectral line formation and the temperature structure of active region fan loops: observations with Hinode/EIS and SDO/AIA

With the aim of studying AR fan loops using Hinode/EIS and SDO/AIA, we investigate a number of inconsistencies in modeling the absolute intensities of Fe VIII and Si VII lines, and address why their images look very similar despite the fact that they have significantly different formation temperatures in ionization equilibrium: log T/K = 5.6 and 5.8. These issues are important to resolve because confidence has been undermined in their use for DEM analysis, and Fe VIII is the main contributor to the AIA 131A channel at low temperatures. Furthermore, they are the best EIS lines to use for velocity studies, and for assigning the correct temperature to velocity measurements in the fans. We find that the Fe VIII 185.213A line is particularly sensitive to the slope of the DEM, leading to disproportionate changes in its effective formation temperature. If the DEM has a steep gradient in the log T/K = 5.6 to 5.8 range, or is strongly peaked, Fe VIII 185.213A and Si VII 275.368A will be formed at the same temperature. We show that this effect explains the similarity of these images in the fans. Furthermore, we show that the most recent ionization balance compilations resolve the discrepancies in absolute intensities. We then combine EIS and AIA to determine the temperature structure of a number of fan loops and find that they have peak temperatures of 0.8--1.2MK. The EIS data indicate that the temperature distribution has a finite (but narrow) width < log sigma/K = 5.5 which, in one case, is found to broaden substantially towards the loop base. AIA and EIS yield similar results on the temperature, emission measure, and thermal distribution in the fans, though sometimes the AIA data suggest a relatively larger thermal width. The result is that both the Fe VIII 185.213A and Si VII 275.368A lines are formed at log T/K ~ 5.9 in the fans, and the AIA 131A response also shifts to this temperature.Comment: To be published in ApJ. Figure 6 is reduced resolution to meet size limits. The abstract has been significantly shortened (original in PDF file

The Temperature and Density Structure of the Solar Corona. I. Observations of the Quiet Sun with the EUV Imaging Spectrometer (EIS) on Hinode

Measurements of the temperature and density structure of the solar corona provide critical constraints on theories of coronal heating. Unfortunately, the complexity of the solar atmosphere, observational uncertainties, and the limitations of current atomic calculations, particularly those for Fe, all conspire to make this task very difficult. A critical assessment of plasma diagnostics in the corona is essential to making progress on the coronal heating problem. In this paper we present an analysis of temperature and density measurements above the limb in the quiet corona using new observations from the EUV Imaging Spectrometer (EIS) on \textit{Hinode}. By comparing the Si and Fe emission observed with EIS we are able to identify emission lines that yield consistent emission measure distributions. With these data we find that the distribution of temperatures in the quiet corona above the limb is strongly peaked near 1 MK, consistent with previous studies. We also find, however, that there is a tail in the emission measure distribution that extends to higher temperatures. EIS density measurements from several density sensitive line ratios are found to be generally consistent with each other and with previous measurements in the quiet corona. Our analysis, however, also indicates that a significant fraction of the weaker emission lines observed in the EIS wavelength ranges cannot be understood with current atomic data.Comment: Submitted to Ap