arXiv subjects
Publications and source records attributed to Philippe Jetzer.
We discuss spherically symmetric static solutions of the Einstein-Klein-Gordon equations for a real scalar field with a mass and a quartic self-interaction term. As for the massless case the solutions have a naked singularity at the origin. However, linear stability analysis shows that these solutions as well as the massless ones are dynamically unstable.
We study the time evolution of small classical perturbations in a gauge invariant way for a complex scalar field in the early zero curvature Friedmann-Lema\^ıtre universe. We, thus, generalize the analysis which has been done so far for a real scalar field. We give also a derivation of the Jeans wavenumber in the Newtonian regime starting from the general relativistic equations, avoiding the so-called Jeans swindle. During the inflationary phase, whose length depends on the value of the bosonic charge, the behavior of the perturbations turns out to be the same as for a real scalar field. In the oscillatory phase the time evolution of the perturbations can be determined analytically as long as the bosonic charge of the corresponding background solution is sufficiently large. This is not possible for the real scalar field, since the corresponding bosonic charge vanishes.
One of the most important problems in astrophysics concerns the nature of the dark matter in galactic halos, whose presence is implied mainly by the observed flat rotation curves in spiral galaxies. Due to the Pauli exclusion principle it can be shown that neutrinos cannot be a major constituent of the halo dark matter. As far as cold dark matter is concerned there might be a discrepancy between the results of the N-body simulations and the measured rotation curves for dwarf galaxies. A fact this, if confirmed, which would exclude cold dark matter as a viable candidate for the halo dark matter. In the framework of a baryonic scenario the most plausible candidates are brown or white dwarfs and cold molecular clouds (mainly of $H_2$). The former can be detected with the ongoing microlensing experiments. In fact, the French collaboration EROS and the American-Australian collaboration MACHO have reported the observation of altogether $\sim$ 10 microlensing events by monitoring during several years the brightness of millions of stars in the Large Magellanic Cloud. In particular, the MACHO team announced the discovery of 8 microlensing candidates by analysing their first 2 years of observations. This would imply that the halo dark matter fraction in form of MACHOs (Massive Astrophysical Compact Halo Objects) is of the order of 45-50% assuming a standard spherical halo model. The most accurate way to get information on the mass of the MACHOs is to use the method of mass moments, which leads to an average mass of 0.27$M_{\odot}$.
The French collaboration EROS and the American-Australian collaboration MACHO have reported the observation of altogether $\sim$ 10 microlensing events by monitoring during several years the brightness of millions of stars in the Large Magellanic Cloud. In particular the MACHO team announced the discovery of 8 microlensing candidates by analysing their first 2 years of observations. This would imply that the halo dark matter fraction in form of MACHOs (Massive Astrophysical Compact Halo Objects) is of the order of 45-50%. The most accurate way to get information on the mass of the MACHOs is to use the method of mass moments. For the microlensing events detected so far by the MACHO collaboration in the Large Magellanic Cloud the average mass turns out to be 0.27$M_{\odot}$.
The most accurate way to get information on the mass of the MACHOs (Massive Astrophysical Compact Halo Objects) is to use the method of mass moments. For the microlensing events detected so far by the EROS and the MACHO collaborations in the Large Magellanic Cloud the average mass turns out to be 0.08$M_{\odot}$. Assuming a spherical standard halo model we find that MACHOs contribute about 20\% to the halo dark matter. The eleven events recorded by OGLE, mainly during its first two years of operation, in the galactic bulge lead to an average mass of 0.29$M_{\odot}$, whereas forty events detected by MACHO during its first year give 0.16$M_{\odot}$, thus suggesting that the lens objects are faint disk stars.
We study the coupled Einstein-Klein-Gordon equations for a complex scalar field with and without a quartic self-interaction in a curvatureless Friedman-Lema\^ı\-tre Universe. The equations can be written as a set of four coupled first order non-linear differential equations, for which we establish the phase portrait for the time evolution of the scalar field. To that purpose we find the singular points of the differential equations lying in the finite region and at infinity of the phase space and study the corresponding asymptotic behavior of the solutions. This knowledge is of relevance, since it provides the initial conditions which are needed to solve numerically the differential equations. For some singular points lying at infinity we recover the expected emergence of an inflationary stage.
Recently the French EROS collaboration and the American-Australian MACHO collaboration have reported the observation of altogether three possible microlensing events by monitoring over several years the brightness of millions of stars in the Large Magellanic Cloud. For each of these events, assuming they are due to microlensing, we compute the most likely mass for the dark compact halo object, which acted as gravitational lens. The most likely masses are 0.12, 0.31 and 0.38 $M_{\odot}$. The average mass calculated using the method of moments turns out to be 0.14 $M_{\odot}$.
It has been shown by Paczyński that gravitational microlensing is potentially a useful method for detecting the dark constituents of the halo of our galaxy, if their mass lies in the approximate domain $10^{-6}<M/M_\odot<10^{-1}$. Microlensing observations now im progress monitor several millions of stars in the Large Magellanic Cloud and in the Galactic Bulge. Here I discuss the main features of the microlensing events: in particular their rates and probability.
It has been shown by Paczyński that gravitational microlensing is potentially a useful method for detecting the dark constituents of the halo of our galaxy, if their mass lies in the approximate domain $10^{-6} < M/M_{\odot} < 10^{-1}$. Microlensing observations now under way monito several millions of stars in the Large Magellanic Cloud and in the Galactic Bulge. Here I discuss the main features of the microlensing events: in particular their rates and probability, taking also into account a possible flattened shaper for the halo.
It has been shown by Paczyński that gravitational microlensing is a useful method to detect brown dwarfs in the dark halo of our galaxy. At present several experiments are carried out to monitor several million stars in the Large Magellanic Cloud with the aim to find such microlensing events. Here I discuss the possibility to use as targets stars in the Andromeda galaxy. Such an experiment would be sensitive to both the brown dwarfs in our halo and in the one of M31. The optical depth $τ$ to gravitational microlensing due to brown dwarfs in the halo of M31 turns out to be $\sim 10^{-6}$, which is comparable to the value of $τ$ for our own halo. I also compute the microlensing rate and the average lensing duration and consider moreover the dependence of $τ$ on the shape of the halo.