Wyniki wyszukiwania - Biblioteka Nauki

Ten serwis zostanie wyłączony 2025-02-11.

Nowa wersja platformy, zawierająca wyłącznie zasoby pełnotekstowe, jest już dostępna.
Przejdź na https://bibliotekanauki.pl

Ograniczanie wyników

3 Acta Astronomica

Znaleziono wyników: 3

Liczba wyników na stronie

Wyniki wyszukiwania

Sortuj według:

Ogranicz wyniki do:

Hydrodynamical Models of Accretion Disks in SU UMa Systems

100%

Kornet K. , Różyczka M.

tom Vol. 50, No. 2

163--175

We numerically test the mode-coupling model (Lubow 1991a) of tidal instability in SU UMa systems. So far, all numerical models confirming it have been based on SPH codes and isothermal equation of state. In our paper we present Eulerian models, using both isothermal approximation and the full energy equation. We also investigate influence of different ways of mass transfer. While isothermal models behave similarly to SPH simulations, the behavior of models with full energy equation is quite different, and the mode-coupling model is not confirmed in this case.

Doppler Tomograms from Hydrodynamical Models of Dwarf Nova Disks

100%

Gawryszczak A. J. , Różyczka M.

tom Vol. 53, No. 1

73--83

We present three-dimensional models of accretion disks in U Gem-like systems and calculate their Doppler tomograms. The tomograms are based on two different assumptions concerning the origin of line emission from the disk. The assumption of lines originating due to irradiation of the surface layer of the disk by the central source leads to a better agreement with observations. We argue that fully three-dimensional modeling is necessary to properly interpret the observed tomograms.

Hot Jupiters and Central Cavities of Protoplanetary Disks

80%

Starczewski S. , Gawryszczak A. J. , Wönsch R. , Różyczka M.

Acta Astronomica

2007

tom Vol. 57, No. 2

123--138

We investigate numerically the orbital evolution of massive extrasolar planets within central cavities of their parent protoplanetary disks. Assuming that they arrive at the inner edge of the disk due to type II migration, we show that they spiral further in. We find that in magnetospheric cavities more massive planets stop migrating at a larger distance from the edge of the disk. This effect may qualitatively explain the correlation between masses and orbital periods found for massive planets with P shorter than 5 days.