Explaining the Great Moderation: it is not the shocks

This paper shows that the explanation of the decline in the volatility of GDP growth since the mid-eighties is not the decline in the volatility of exogenous shocks but rather a change in their propagation mechanism. JEL Classification: E32, E37, C32, C53Great Moderation, Information, shocks

Coordinated cadastral system for Peninsular Malaysia : from concept to reality

The main objectives of conducting cadastral surveys that had been promulgated in the early days of its practice have since been continually adhered to and later came to be adopted as amongst the principal functions of DSMM. They were stated in the Survey Regulations (DSMM, 1976) as follows: “(a) To provide evidence which will completely and permanently identify the land conveyed by any title issued by government. (b) To compile and make available records of alienation necessary for intelligent land administration.

Acoustic fluidization for earthquakes?

Melosh [1996] has suggested that acoustic fluidization could provide an alternative to theories that are invoked as explanations for why some crustal faults appear to be weak. We show that there is a subtle but profound inconsistency in the theory that unfortunately invalidates the results. We propose possible remedies but must acknowledge that the relevance of acoustic fluidization remains an open question.Comment: 13 page

Transient events in bright debris discs: Collisional avalanches revisited

A collisional avalanche is set off by the breakup of a large planetesimal, releasing small unbound grains that enter a debris disc located further away from the star, triggering there a collisional chain reaction that can potentially create detectable transient structures. We explore this mechanism, using for the first time a code coupling dynamical and collisional evolutions, and investigate if avalanches could explain the short-term luminosity variations observed in some extremely bright discs. We consider two set-ups: a cold disc case, with a dust release at 10au and an outer disc extending from 50 to 120au, and a warm disc case with the release at 1au and a 5-12au outer disc. We find that avalanches could leave detectable structures on resolved images, for both cold and warm disc cases, in discs with optical depth $\tau$ of a few $10^{-3}$, provided that large dust masses ($\gtrsim$10$^{20}$-5$\times$10$^{22}$g) are initially released. The integrated photometric excess due to an avalanche is limited, less than 10% for these released dust masses, peaking in the mid-IR and becoming insignificant beyond $\sim$40-50$\mu$m. Contrary to earlier studies, we do not obtain stronger avalanches when increasing $\tau$ to higher values. Likewise, we do not observe a significant luminosity deficit, as compared to the pre-avalanche level, after the passage of the avalanche. These two results concur to make avalanches an unlikely explanation for the sharp luminosity drops observed in some extremely bright debris discs. The ideal configuration for observing an avalanche would be a two-belt structure, with an inner belt of fractional luminosity >10$^{-4}$ where breakups of massive planetesimals occur, and a more massive outer belt, with $\tau$ of a few $10^{-3}$, into which the avalanche chain reaction develops and propagates.Comment: Accepted for publication in Astronomy & Astrophysics (abstract drastically shortened to meet astro-ph requirements

Large Scale Structure and Cosmic Rays revisited

We investigate the possibility that ultra high energy cosmic rays (E > 10^19 eV) are related to the distribution of matter on large scales. The large scale structure (LSS) data stems from the recent IRAS PSCz redshift survey. We present preliminary predictions drawn from an anisotropic distribution of sources which follows the galaxy distribution.Comment: 6 pages, 2 figures, uses World Scientific style. To appear in the proceedings of "Third International Workshop on New Worlds in Astro-Particle Physics", 1-3 Set. 2000, Faro, Portugal and X ENAA, 27-28 Jul. 2000, Lisbon, Portuga

The Galactic halo magnetic field revisited

Recently, Sun et al. (2008) published new Galactic 3D-models of magnetic fields in the disk and halo of the Milky Way and the distribution of cosmic-ray electron density by taking into account the thermal electron density model NE2001 by Cordes & Lazio (2002, 2003). The models successfully reproduce observed continuum and polarization all-sky maps and the distribution of rotation measures of extragalactic sources across the sky. However, the model parameters obtained for the Galactic halo, although reproducing the observations, seem physically unreasonable: the magnetic field needs to be significantly stronger in the Galactic halo than in the plane and the cosmic-ray distribution must be truncated at about 1 kpc to avoid excessive synchrotron emission from the halo. The reason for these unrealistic parameters was the low scale-height of the warm thermal gas of about 1 kpc adapted in the NE2001 model. However, this scale-height seemed well settled by numerous investigations. Recently, the scale-height of the warm gas in the Galaxy was revised by Gaensler et al. (2008) to about 1.8 kpc, by showing that the 1 kpc scale-height results from a systematic bias in the analysis of pulsar data. This implies a higher thermal electron density in the Galactic halo, which in turn reduces the halo magnetic field strength to account for the observed rotation measures of extragalactic sources. We slightly modified the NE2001 model for the new scale-height and revised the Sun et al. (2008) model parameters accordingly: the strength of the regular halo magnetic field is now 2 microG or lower, and the physically unrealistic cutoff in z for the cosmic-ray electron density is removed. The simulations based on the revised 3D-models reproduce all-sky observations as before.Comment: 11 pages, 6 figures, accepted for publication in Research in Astronomy and Astrophysics (RAA

Propagation Speed of the Maximum of the Fundamental Solution to the Fractional Diffusion-Wave Equation

In this paper, the one-dimensional time-fractional diffusion-wave equation with the fractional derivative of order $1 \le \alpha \le 2$ is revisited. This equation interpolates between the diffusion and the wave equations that behave quite differently regarding their response to a localized disturbance: whereas the diffusion equation describes a process, where a disturbance spreads infinitely fast, the propagation speed of the disturbance is a constant for the wave equation. For the time fractional diffusion-wave equation, the propagation speed of a disturbance is infinite, but its fundamental solution possesses a maximum that disperses with a finite speed. In this paper, the fundamental solution of the Cauchy problem for the time-fractional diffusion-wave equation, its maximum location, maximum value, and other important characteristics are investigated in detail. To illustrate analytical formulas, results of numerical calculations and plots are presented. Numerical algorithms and programs used to produce plots are discussed.Comment: 22 pages 6 figures. This paper has been presented by F. Mainardi at the International Workshop: Fractional Differentiation and its Applications (FDA12) Hohai University, Nanjing, China, 14-17 May 201