The thin disk model, which is a nonstandard approach to the modeling of the spiral galaxy dynamics, will be presented in context of the motion of the halo compact objects located around the Milky Way. Because in the thin disk framework there is no dark matter nonbaryonic component, it is interesting does the motion of the halo compact objects is compatibile with the low Galaxy mass predicted by the disk model.

Broad and strong emission lines are the basic signatures of active galaxies. The lines allowed Maarten Schmidt in 1963 to reveil the cosmological nature of quasars. However, the origin of the lines remained unknown. In our recent paper (Bozena Czerny& Krzysztof Hryniewicz) we showed that the underlying mechanism is the presence of the dust in the accretion disk atmosphere. In particular, we demonstrated that for all active galaxies, independently from their mass and accretion rate the Broad Line Region starsts where the disk atmosphere, descreasing with the distance from the black hole, crosses 1000 K. At such temperature the dust can start to form, and the radiation pressure, acting very efficiently in the presence of dust, pushes the massive outflow. High above the disk the material becomes irradiated by the distant nucler emission, the dust evaporates, and the matter not supported further by the radiation pressure fall back onto the disk. Turbulence created in the process combined with the rotational motion reproduce the observed emission line profiles.

Noncommutative Geometry and Cosmology
Noncommutative geometry is a vast generalisation of the standard differential geometry. Apart from its mathematical elegance it has numerous applications in physical theories. In my talk I will present various different cosmological models based on noncommutative geometry. The talk will have a review character and is addressed to non-experts.
Geometria nieprzemienna a kosmologia
Geometria nieprzemienna jest obszernym uogólnieniem standardowej geometrii różniczkowej. Oprócz matematycznej elegancji teoria ta ma wiele zastosowań w modelach fizycznych. W moim referacie przedstawię różne modele kosmologiczne bazujące na geometrii nieprzemiennej. Referat będzie miał charakter przeglądowy i jest adresowany do szerokiej publiczności.

AGN jets are considered to be produced by injecting magnetic and/or thermal energies into the dilute polar region, where the mass loading processes are essential for determining the jet properties. We discuss the role of the relativistic neutrons escaped from the accretion flow for the mass loading (as well as thermal energy injection). If I have time, I would also talk on my recent work on the emission process of Fermi-GRBs.

Recently, Chrusciel, Eckstein, Nguyen and I have shown that stationary I^+ regular two-component black holes do not exist in axial symmetry. I will discuss the result and the history of the problem.

The relation between the ratio of infrared (IR) and ultraviolet (UV) flux densities (the infrared excess: IRX) and the slope of the UV spectrum (β) of galaxies plays a fundamental role in the evaluation of the dust attenuation of star forming galaxies especially at high redshifts. Many authors, however, pointed out that there is a significant dispersion and/or deviation from the originally proposed IRX-β relation depending on sample selection. We reexamined the IRX-β relation by measuring the far- and near-UV flux densities of the original sample galaxies with GALEX and AKARI imaging data, and constructed a revised formula. We found that the newly obtained IRX values were lower than the original relation because of the significant underestimation of the UV flux densities of the galaxies, caused by the small aperture of IUE. Further, since the original relation was based on IRAS data which covered a wavelength range of λ = 42-122 μm, using the data from AKARI which has wider wavelength coverage toward longer wavelengths, we obtained an appropriate IRX-β relation with total dust emission (TIR):
log ( L_TIR / L_FUV ) = log [ 10^{0.4 ( 3.06 + 1.58 β )} - 1 ] + 0.22.
This new relation is consistent with most of the preceding results for samples selected at optical and UV, though there is a significant scatter around it. We also found that even the quiescent class of IR galaxies follows this new relation, though luminous and ultraluminous IR galaxies distribute completely differently as well known before.

Jednym z fundamentalnych zadań obserwacyjnej kosmologii, związanych z analizą CMB, jest precyzyjne zbadanie wpływu emisji od wszystkich znanych obiektów pomiędzy obserwatorem i CMB. Cała klasa tych obiektów zwanych "foregrounds" obejmuje m.in. emisję rozciągłą i wpływ dyskretnych źródeł Naszej Galaktyki oraz pozagalaktyczne galaktyki typu Starburst, AGN a także efekty komptonizacji w materii gromad galaktycznych. Różne zidentyfikowane przyczyny, które zmieniają lub mogą zmienić mierzony strumień, widmo i polaryzację reliktowych fotonów, muszą być uwzględnione i precyzyjnie usunięte. Badanie ewolucji galaktyk dla dużych "z" samo w sobie jest ciekawym wyzwaniem, więc badanie najdalszych, a więc także najsłabszych źródeł jest ważnym celem. Własności fizyczne radioźródeł i ich kosmologiczna ewolucja, w szczególności ich zmienność mają znaczący wpływ na dokładność pomiarów anizotropii CMB. W celu zbadania populacji słabych źródeł (w sensie odbieranego strumenia) zbudowano i zainstalowano na 32m radioteleskopie CA UMK matrycę odbiorczą OCRA. W referacie przedstawiona będzie główna idea systemu OCRA oraz podsumowane zostaną uzyskane dotychczas wyniki badań. Dotyczą one źródeł galaktycznych i AGN-ów a także efektu S-Z na 30 GHz (długość fali 1cm), wszystko w kontekście wyznaczenia właściwości i wpływu "foregrounds".

Galaxies with low stellar surface brightness (LSB galaxies) constitute a important parallel branch of galaxy evolution (in addition to the "normal" high surface brightness galaxies). Results from optical searches for LSB galaxies imply that the number density distribution stays flat out to a central surface brightness of 26 Bmag/sq-arcsec. Beyond that value, little known up to now. Even within these limits, the currently known LSB population is already a significant contributor to the local baryon density. In my talk I will discuss a new search technique, using supernovae (SNe) as signposts for extreme LSB galaxies. I will present results from our searches and discuss implications for core collapse SNe and the existence of an extremely dim LSB galaxy population. One unexpected result of our study is the detection of SNe without any detectable host galaxy, but relatively close to massive spiral galaxies. An attractive explanation for these SN could be explosions from massive hyper velocity stars, which would manifest the first occurrence of the phenomenon beyond the Local Group of galaxies. This lead to implications for the probability of hypervelocity stars and the ionization of gas in the halos of galaxies.