5,575 research outputs found
Infrared Line Emission from Planetary Nebulae. I - General Theory
General theory of infrared line emission from planetary nebul
Peering Forward, 10 Years After: International Policy and Consumer Credit Regulation
A key change since the financial crisis of 2008 is the internationalization of interest in consumer finance. International institutions monitor household credit because of its impact on financial stability and market expansion. Macroprudential concerns drove this interest, resulting in a sea change in approaches to consumer credit regulation in many jurisdictions. This article critically analyses the emerging international policy paradigm, contrasting pre-and post-crisis regulatory approaches and highlighting continuing tensions about key policy choices. It then uses two recent sites of contestation, debt adjustment and the regulation of high-cost credit to demostrate the persistence of conflict over the positioning of consumers within an emergent stability focused paradigm of financial consumer protection
SPH Simulations of Direct Impact Accretion in the Ultracompact AM CVn Binaries
The ultracompact binary systems V407 Vul (RX J1914.4+2456) and HM Cnc (RX
J0806.3+1527) - a two-member subclass of the AM CVn stars - continue to pique
interest because they defy unambiguous classification. Three proposed models
remain viable at this time, but none of the three is significantly more
compelling than the remaining two, and all three can satisfy the observational
constraints if parameters in the models are tuned. One of the three proposed
models is the direct impact model of Marsh & Steeghs (2002), in which the
accretion stream impacts the surface of a rapidly-rotating primary white dwarf
directly but at a near-glancing angle. One requirement of this model is that
the accretion stream have a high enough density to advect its specific kinetic
energy below the photosphere for progressively more-thermalized emission
downstream, a constraint that requires an accretion spot size of roughly
1.2x10^5 km^2 or smaller. Having at hand a smoothed particle hydrodynamics code
optimized for cataclysmic variable accretion disk simulations, it was
relatively straightforward for us to adapt it to calculate the footprint of the
accretion stream at the nominal radius of the primary white dwarf, and thus to
test this constraint of the direct impact model. We find that the mass flux at
the impact spot can be approximated by a bivariate Gaussian with standard
deviation \sigma_{\phi} = 164 km in the orbital plane and \sigma_{\theta} = 23
km in the perpendicular direction. The area of the the 2\sigma ellipse into
which 86% of the mass flux occurs is roughly 47,400 km^2, or roughly half the
size estimated by Marsh & Steeghs (2002). We discuss the necessary parameters
of a simple model of the luminosity distribution in the post-impact emission
region.Comment: 24 pages, 5 figures, Accepted for publication in Ap
The Turn-On of Mass Transfer in AM CVn Binaries: Implications for RX J0806+1527 and RX J1914+2456
We report on evolutionary calculations of the onset of mass transfer in AM
CVn binaries, treating the donor's evolution in detail. We show that during the
early contact phase, while the mass transfer rate, \Mdot, is increasing,
gravity wave (GW) emission continues to drive the binary to shorter orbital
period, \Porb. We argue that the phase where \Mdot > 0 and \nudot > 0
(\nu = 1/\Porb) can last between and yrs, significantly longer
than previously estimated. These results are applied to RX J0806+1527 (\Porb =
321 s) and RX J914+2456 (\Porb=569 s), both of which have measured \nudot >
0. \emph{Thus, a \nudot > 0 does not select between the unipolar inductor
and accretion driven models proposed as the source of X-rays in these systems}.
For the accretion model, we predict for RX J0806 that \ddot{\nu} \approx
\ee{1.0-1.5}{-28} Hz s and argue that timing observations can probe
at this level with a total yr baseline. We also place
constraints on each system's initial parameters given current observational
data.Comment: 5 pages, 3 figures, accepted to ApJ
A burst from the direction of UZ Fornacis with XMM-Newton
The XMM-Newton pointing towards the magnetic cataclysmic variable UZ For
finds the source to be a factor > 10^3 fainter than previous EXOSAT and ROSAT
observations. The source was not detected for the majority of a 22 ksec
exposure with the EPIC cameras, suggesting that the accretion rate either
decreased, or stopped altogether. However a 1.1 ksec burst was detected from UZ
For during the observation. Spectral fits favour optically thin, kT = 4.4 keV
thermal emission. Detection of the burst by the on-board Optical Monitor
indicates that this was most probably an accretion event. The 0.1-10 keV
luminosity of 2.1 x 10^30 erg/s is typical for accretion shock emission from
high state polars and would result from the potential energy release of ~ 10^16
g of gas. There is no significant soft excess due to reprocessing in the white
dwarf atmosphere.Comment: 7 pages, 2 postscript figures, ApJL, in pres
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