Marek Kutschera

On the axisymmetric thin disc model of flattened galaxies

Non-monotonic features of rotation curves, and also the related gravitational effects typical of thin discs – like backward-reaction or amplification of rotation by negative surface density gradients – which are characteristic imprints of disc-like mass distributions, are discussed in the axisymmetric thin disc model. The influence of the data cut-off in rotational velocity measurements on the determination of the mass distribution in flattened galaxies is studied. It has also been found that the baryonic matter distribution in the spiral galaxy NGC 5475, obtained in the axisymmetric thin disc approximation, accounts for the rotation curve of the galaxy. To obtain these results, the iteration method developed recently by the authors has been applied.

Transverse gradients of azimuthal velocity in a global disc model of the Milky Way

In this paper, we aim to estimate the vertical gradients in the rotational velocity of the Galaxy. This is carried out in the framework of a global thin disc model approximation. The predicted gradient values coincide with the observed vertical fall-off in the rotation curve of the Galaxy. The gradient is estimated based on a statistical analysis of trajectories of test bodies in the gravitational field of the disc and in an analytical way using a quasi-circular orbit approximation. The agreement of the results with the gradient measurements is remarkable in view of other more complicated, non-gravitational mechanisms used for explaining the observed gradient values. Finally, we find that models with a significant spheroidal component give worse vertical gradient estimates than the simple disc model. In view of these results, we can surmise that, apart from the central spherical bulge and Galactic halo, the gross mass distribution in the Galaxy forms a flattened rather than spheroidal figure.

Global disc models for galaxies NGC 1365, 6946, 7793 and UGC 6446

Spiral galaxies are studied using a simple global disc model as a means for approximate determination of mass profiles. Based on rotation curves and the amount of gas (HI+He), we find global surface mass densities consistent with measurements and compare them with B-band surface brightness profiles. As a result we obtain mass-to-light ratio profiles. We give some arguments for why our approach is reliable and sometimes better than those assuming ad hoc the presence of a massive non-baryonic dark matter halo. Using this model, we study galaxies NGC 7793, 1365, 6946 and UGC 6446. Based on a rotation curve from The HI Nearby Galaxy Survey (THINGS) we also study galaxy NGC 4536 and compare the results with those we published elsewhere for the same galaxy.

Future neutrino observations of nearby pre‐supernova stars before core‐collapse

We discuss important issues which are essential for understanding future capabilities of the large water Cherenkov detectors from astrophysical point of view. The paper is concentrated on the detection of the neutrinos, which are emitted before core‐collapse from massive stars.