We will review the approach used for studying the conversion of a hadronic star into a quark star based on the assumption of a infinitely thin combustion zone and we will discuss why, in this scheme, the combustion stops before the whole hadronic star is converted.
During the current run of an electron-positron collider DAFNE special electrodes for electron cloud suppression have been inserted in all dipole and wiggler magnets of the positron ring. In this paper we discuss the impact of these electrodes on beam
dynamics and overall collider performance. In particular we report results of measurements such as e-cloud instabilities growth rate, transverse beam size variation, tune shifts along the bunch train etc. with the electrodes switched on and off that clearly indicate the effectiveness of the electrodes for e-cloud suppression.
We show that the r-mode instability can generate strong toroidal fields in the core of accreting millisecond quark stars by inducing differential rotation. We follow the spin frequency evolution on a long time scale taking into account the magnetic d
amping rate in the evolution equations of r-modes. The maximum spin frequency of the star is only marginally smaller than in the absence of the magnetic field. The late-time evolution of the stars which enter the r-mode instability region is instead rather different if the generated magnetic fields are taken into account: they leave the millisecond pulsar region and they become radio pulsars.
In this communication we present a generalization of the map formalism, introduced in [1] and [2], to the analysis of electron flux at the chamber wall with particular reference to the exploration of LHC conditioning scenarios.
Bunch-by-bunch longitudinal diagnostics is a key issue of modern accelerators. To face up this challenging demand, tests of mid-IR compact uncooled photoconductive HgCdTe detectors have been recently performed at DAFNE. Different devices were used to
monitor the emission of e- bunches. The first experiments allowed recording of 2.7 ns long e- bunches with a FWHM of a single pulse of about 600 ps. These results address the possibility to improve diagnostics at DAFNE and to this purpose an exit port on a bending magnet of the positron ring has been set-up. An HV chamber, hosting a gold-coated plane mirror that collects and deflects the radiation through a ZnSe window, is the front-end of this port. After the window, a simple optical layout in air allows focusing IR radiation on different detectors. The instrumentation will allow comparison in the sub-ns time domain between the two rings and to identify and characterize bunch instabilities. Moreover, to improve performances tests of new photovoltaic detectors with sub-ns response times are in progress. We will briefly summarize the actual status of the 3+L experiment and will discuss future applications of fast IR photovoltaic detectors and the development of fast IR array detectors.
The formation of a strange or hybrid star from a neutron star progenitor is believed to occur when the central stellar density exceeds a critical value. If the transition from hadron to quark matter is of first order, the event has to release a huge
amount of energy in a very short time and we would be able to observe the phenomenon even if it is at cosmological distance far from us; most likely, such violent quark deconfinement would be associated with at least a fraction of the observed gamma ray bursts. If we allow for temporal variations of fundamental constants like $Lambda_{QCD}$ or $G_N$, we can expect that neutron stars with an initial central density just below the critical value can enter into the region where strange or hybrid stars are the true ground state. From the observed rate of long gamma ray bursts, we are able to deduce the constraint $dot{G}_N/G_N lesssim 10^{-17} {rm yr^{-1}}$, which is about 5 orders of magnitude more stringent than the strongest previous bounds on a possible increasing $G_N$.
