Wyman's solution, self-similarity and critical behaviour

We show that the Wyman's solution may be obtained from the four-dimensional Einstein's equations for a spherically symmetric, minimally coupled, massless scalar field by using the continuous self-similarity of those equations. The Wyman's solution depends on two parameters, the mass $M$ and the scalar charge $\Sigma$. If one fixes $M$ to a positive value, say $M_0$, and let $\Sigma^2$ take values along the real line we show that this solution exhibits critical behaviour. For $\Sigma^2 >0$ the space-times have eternal naked singularities, for $\Sigma^2 =0$ one has a Schwarzschild black hole of mass $M_0$ and finally for $-M_0^2 \leq \Sigma^2 < 0$ one has eternal bouncing solutions.Comment: Revtex version, 15pages, 6 figure

First Detection of Ar-K Line Emission from the Cygnus Loop

We observed the Cygnus Loop with XMM-Newton (9 pointings) and Suzaku (32 pointings) between 2002 and 2008. The total effective exposure time is 670.2 ks. By using all of the available data, we intended to improve a signal-to-noise ratio of the spectrum. Accordingly, the accumulated spectra obtained by the XIS and the EPIC show some line features around 3 keV that are attributed to the S He$\beta$ and Ar He$\alpha$ lines, respectively. Since the Cygnus Loop is an evolved ($\sim$10,000 yr) supernova remnant whose temperature is relatively low ($<$1 keV) compared with other young remnants, its spectrum is generally faint above 3.0 keV, no emission lines, such as the Ar-K line have ever been detected. The detection of the Ar-K line is the first time and we found that its abundance is significantly higher than that of the solar value; 9.0$^{+4.0}_{-3.8}$ and 8.4$^{+2.5}_{-2.7}$ (in units of solar), estimated from the XIS and the EPIC spectra, respectively. We conclude that the Ar-K line originated from the ejecta of the Cygnus Loop. Follow-up X-ray observations to tightly constrain the abundances of Ar-rich ejecta will be useful to accurately estimate the progenitor's mass.Comment: 12 pages, 9 figures, accepted for publication in PAS

Continuous measurement of heart rate variability following carbon dioxide pneumoperitoneum during nitrous oxide/sevoflurane anaesthesia

Background: Previous studies of autonomic nervous system activity through analysis of heart rate variability (HRV) have demonstrated increased sympathetic activity during positive-pressure pneumoperitoneum. We employed an online, continuous method for rapid HRV analysis (MemCalc&trade;, Tarawa, Suwa Trust, Tokyo, Japan) to demonstrate rapid changes in autonomic nervous system during pneumoperitoneum for laparoscopy. Method: The powers of low-frequency (LF) (0.04-0.15 Hz) and high-frequency (HF) (0.15-0.4 Hz) components of HRV in 20 healthy adult patients were monitored under sevoflurane anaesthesia for 10 minutes after the initiation of carbon dioxide pneumoperitoneum at 10 mmHg. Results: Heart rate increased promptly, but transiently, just after peritoneal insufflation. At that time, the ratio between the LF and HF components increased on HRV. Similar, but small, changes occurred following head-up positioning. Conclusion: By monitoring HRV continuously, we have demonstrated that the change in autonomic nervous system balance induced by peritoneal insufflation was prompt and transient. The change in autonomic nervous system activity could have been due to increased sympathetic activity, reduced vagal activity, or both.Keywords: heart rate variability; positive pressure pneumoperitoneum; continuous monitorin

Birth and evolution of a dense coronal loop in a complex flare region

&lt;p&gt;&lt;b&gt;Context:&lt;/b&gt; During the 14th/15th of April 2002, several flares occurred in NOAA active region complex 9893/9910. Two of these were previously interpreted as having anomalously high coronal column densities.&lt;/p&gt; &lt;p&gt;&lt;b&gt;Aims:&lt;/b&gt; We develop a scenario using multiwavelength observations to explain the high coronal column density (1020 cm-2) present at the onset of the 14th April 2002 M3.7 hard X-ray event.&lt;/p&gt; &lt;p&gt;&lt;b&gt;Methods:&lt;/b&gt; Prior to this event a series of flares occurred in close temporal and spatial proximity. We observe the sequence of flares in a multiwavelength regime from radio to hard X-rays. This allows us to study the particle acceleration and plasma evaporation in these events.&lt;/p&gt; &lt;p&gt;&lt;b&gt;Results:&lt;/b&gt; The observations of these flares lead us to propose a sequence of reconnections between multiple systems of loops in a 3 dimensional field geometry. We suggest that the dense loops in the M3.7 event can be explained as being already filled with plasma from the earlier events; these loops then themselves become unstable or reconnect leading to particle acceleration into an overdense coronal environment. We explore the possibility that a high-beta disruption is behind the instability of these dense loops, leading to the 14th April 2002 M3.7 event and the observation of hard X-rays in the corona at energies up to &#8776; 50 keV.&lt;/p&gt

Noncommutative Metafluid Dynamics

In this paper we define a noncommutative (NC) Metafluid Dynamics \cite{Marmanis}. We applied the Dirac's quantization to the Metafluid Dynamics on NC spaces. First class constraints were found which are the same obtained in \cite{BJP}. The gauge covariant quantization of the non-linear equations of fields on noncommutative spaces were studied. We have found the extended Hamiltonian which leads to equations of motion in the gauge covariant form. In addition, we show that a particular transformation \cite{Djemai} on the usual classical phase space (CPS) leads to the same results as of the $\star$-deformation with $\nu=0$. Besides, we will shown that an additional term is introduced into the dissipative force due the NC geometry. This is an interesting feature due to the NC nature induced into model.Comment: 11 page

Jet photonique simple ou double pour la détection d'objets sub-longueur d'onde

National audienceOn appelle « jet photonique » un faisceau électromagnétique ayant une grande concentration de puissance en champ proche. Ce jet photonique possède des propriétés comme une faible divergence et une faible largeur à mi-hauteur. Il peut être appliqué pour la détection d'objet de taille sub-longueur d'onde. Les jets photoniques peuvent être observés pour des longueurs d'onde optiques dans le voisinage d'une sphère diélectrique micrométrique. Ils peuvent être obtenus également dans la gamme des microondes. Dans cet article, nous montrons la réalisation et la mise en évidence de ces jets photoniques dans la gamme microondes. La modélisation développée a permis de mettre en oeuvre des systèmes produisant des jets simples ou doubles. L'expérimentation et ses résultats sont présentés et la détection facile d'objets de faible taille devant la longueur d'onde est mise en évidence ainsi que la mise en évidence de leur mouvement