Many countries are currently facing high mortality caused by the circulation of SARS-CoV-2 among the elderly not yet vaccinated. Vaccine shortage poses relevant challenges to health authorities, called to act in a timely manner, and with scarcity of vaccine, and data. We have developed a model for estimating of the impact of vaccination on the mortality of the elderly following a schedule of mRNA SARS-CoV-2 vaccine that prioritize first dose administration, as alternative to the standard schedule of two doses administered 3 to 4 weeks apart. We studied the Italian scenario, considering it representative of other Countries facing similar conditions in terms of virus circulation, mortality, and vaccine shortage, in the period from February 10 to April 14 2021. Under different conditions of quantity of vaccine administration, the schedule prioritizing first doses showed always significant increase of protected individuals, and a decrease of deaths, up to 19.8% less than the standard schedule. These findings support the vaccination option of prioritizing the first dose in the elderly until vaccine supplies are adequate.
Formation of disks with long-lived spiral arms from violent
by Francesco Sylos Labini, Luis Diego Pinto, and Roberto
Dear Dr. Sylos-Labini,
We are pleased to inform you that your paper has been selected by the
editors of Physical Review E to be an Editors’ Suggestion.
On a possibile solution of the core-cusp problem and the fundamental properties of self gravitating quasi-stationary states.
One of the crucial problems for the galaxy formation theory is to explain the cusp-core paradox: while the simulations of the theoretical models give rise to a diverging density profile at a small distance (1 / r) from the center, observations of galaxy profiles show that these are constant.
To understand the origin of these profiles it is necessary to understand the fundamental properties of the quasi-equilibrium states of gravitational systems and in particular what kind of dynamical path they followed during their formation.
We have found that, depending on the initial conditions, these stationary states can exhibit a small-scale divergent profile or a flat profile. This difference corresponds to a different dynamical nature underlying their origin.
Coming back to galaxies, the profiles indicate that the dynamic that gave them origin is a violent type of relaxation. That is, a dynamical process different from the “standard” one of cold dark matter models.
15 pages, 24 figures, Accepted for publication in Astronomy and Astrophysics
This work represents a development of the study of the collapses of purely self-gravitating systems (see https://physics.aps.org/articles/v12/s19) to the case in which a dissipational gas component is also present. These latter systems show much richer morphological and kinematical structures that may have important observational implications to understand the kinematic and dynamics of the Milky Way as revealed by ongoing surveys such as the Gaia Mission.
by Francesco Sylos Labini, Luis Diego Pinto, Roberto Capuzzo-Dolcetta
Recent statistical deconvolution methods have produced extended kinematical maps in a range of heliocentric distances that are a factor of two to three larger than those analysed in the Gaia Collaboration based on the same data. In this paper, we use such maps to derive the rotation curve both in the Galactic plane and in off-plane regions and to analyse the density distribution. By assuming stationary equilibrium and axisymmetry, we used the Jeans equation to derive the rotation curve. Then we fit it with density models that include both dark matter and predictions of the MOND (Modified Newtonian dynamics) theory. Since the Milky Way exhibits deviations from axisymmetry and equilibrium, we also considered corrections to the Jeans equation. To compute such corrections, we ran N-body experiments of mock disk galaxies where the departure from equilibrium becomes larger as a function of the distance from the centre. The rotation curve in the outer disk of the Milky Way that is constructed with the Jeans equation exhibits very low dependence on R and z and it is well-fitted both by dark matter halo and MOND models. The application of the Jeans equation for deriving the rotation curve, in the case of the systems that deviate from equilibrium and axisymmetry, introduces systematic errors that grow as a function of the amplitude of the average radial velocity. In the case of the Milky Way, we can observe that the amplitude of the radial velocity reaches ∼10% that of the azimuthal one at R≈20 kpc. Based on this condition, using the rotation curve obtained from the Jeans equation to calculate the mass may overestimate its measurement.
Aims: Here, we investigate the dynamical effects produced by different mechanisms that can explain the radial and vertical components of these extended kinematic maps, including a decomposition of bending and breathing of the vertical components. This paper as a whole tries to be a compendium of different dynamical mechanisms whose predictions can be compared to the kinematic maps.
Methods: Using analytical methods or simulations, we are able to predict the main dynamical factors and compare them to the predictions of the extended kinematic maps of Gaia-DR2.
Results: The gravitational influence of Galactic components that are different from the disk, such as the long bar or bulge, the spiral arms, or a tidal interaction with Sagittarius dwarf galaxy, may explain some features of the velocity maps, especially in the inner parts of the disk. However, they are not sufficient in explaining the most conspicuous gradients in the outer disk. Vertical motions might be dominated by external perturbations or mergers, although a minor component may be due to a warp whose amplitude evolves with time. Here, we show with two different methods, which analyze the dispersion of velocities, that the mass distribution of the disk is flared. Despite these partial explanations, the main observed features can only be explained in terms of out-of-equilibrium models, which are either due to external perturbers or to the fact that the disk has not had time to reach equilibrium since its formation.
Spiral galaxies are well-known astrophysical structures, but how they form is not fully understood. This paper describes simulations showing that they could be transient, nonequilibrium structures originating from the collapse of clouds of matter interacting solely through self-gravity.
Synopsis: Galactic Spirals May Form Spontaneously
Initial condition: prolate ellipsoid with a central overdensity. More
Comunicato stampa – Le braccia che avvolgono il nucleo di questa interessante formazione celeste infrangono la terza legge di Keplero per cui la velocità orbitale decresce con la distanza dal centro. Per spiegare questo fenomeno si ipotizzano la materia oscura o una correzione della seconda legge di Newton.
Un team internazionale composto da ricercatori dell’Isc-Cnr e del Laboratoire de Physique Nucleaire et de Hautes Energies di Parigi apre la strada a ipotesi diverse, dimostrando come sia possibile simulare al computer la nascita di una galassia a spirale.
Roma, 22 gennaio 2018 – Hanno la forma di un disco composto da un nucleo con alcune braccia che gli si avvolgono intorno. Sono le galassie a spirale, uno degli oggetti più suggestivi e interessanti dell’universo visibile rivelati dall’astronomia. Francesco Sylos Labini, ricercatore presso l’Istituto dei sistemi complessi del Consiglio nazionale delle ricerche (Isc-Cnr) e del Centro Fermi, ha recentemente pubblicato sulla rivista The Astrophysical Journal una ricerca sul tema in collaborazione con il Laboratoire de Physique Nucleaire et de Haute Energies (Lpnhe) di Parigi.