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Katarzyna Otmianowska-Mazur ( OA UJ Kraków ) ‏

Katarzyna Otmianowska-Mazur ( OA UJ Kraków ) ‏ Grzegorz Kowal ( Uniw. Sao Paulo, Brazylia / OA UJ Kraków ) ‏ Katarzyna Kulpa-Dybeł (OA UJ Kraków) Hubert Siejkowski, (OA UJ Kraków) Marian Soida (OA UJ Kraków) Barbara Kulesza-Żydzik (OA UJ Kraków) Michał Hanasz (CA UMK, Toruń)

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Katarzyna Otmianowska-Mazur ( OA UJ Kraków ) ‏

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  1. Katarzyna Otmianowska-Mazur (OA UJ Kraków)‏ Grzegorz Kowal (Uniw. Sao Paulo, Brazylia/OA UJ Kraków)‏ Katarzyna Kulpa-Dybeł (OA UJ Kraków) Hubert Siejkowski, (OA UJ Kraków) Marian Soida (OA UJ Kraków) Barbara Kulesza-Żydzik (OA UJ Kraków) Michał Hanasz (CA UMK, Toruń) Dominik Woltański (CA UMK, Toruń) Dominik Bomans (RUHR, Bochum) 3D numerical simulations of magnetic field evolution in barred galaxies and in spiral galaxies under influence of tidal forces

  2. Schedule of my talk: • Introduction: observations and simulation • Magnetic field evolution in barred galaxies • Magnetic field evolution in galaxies under • influence of tidal forces

  3. Observations of magnetic field in barred and spiralgalaxies Most of spiral and barred galaxies have large-scale ordered magnetic field structures The existence of bars, spirals and rings considerably influences large-scale magnetic field configuration In most of barred galaxies we observe strong interactions between gas and large-scale magnetic fieldwhich undergo shear and compression Similar facts are observed in spiral galaxies under influence of tidal forces Ref. Beck et al.. 2002, A&A 391, 83 Patrikeev, I.; Fletcher, A.et al. 2006A&A 458, 441

  4. M51, total power 6cm +B-vectors, VLA +Effelsberg+ HST optical image

  5. Simulations Moss et al. 2007,A&A 465, 157 Magnetic fields in barred galaxies. Modelling of NGC 1365 Computation 3D, dynamo, velocity fitted to HI and CO Agreement of the model and observation is good in top left andbottom right regions near the bar, differences are much higher in other regions.

  6. Kotarba et al. 2009, MNRAS 397, 733 Magnetic field structure due to the global velocity field in spiral galaxies Self-consistent N-body/SPH simulationwith solution of induction equation in SPH parts The Authors obtained magnetic field structures similar to observed in spiral galaxies

  7. Results of our 3D simulations MHD code Grzegorz Kowal First paper: 1.2 x 1011 Msun sizes (X, Y, Z) – 20kpc x20kpcx 5 kpc, resolution: 512 x 512 x 129 (39pc) size of bar 4 x 2 x 2 kpc Second experiment: 1.75 x 1011 Msun sizes: 30 kpc x 30 kpc x 7.59kpc resolution 512 x 512 x 128 (59 pc) size of bar 6 x 3 x 3 kpc Kulesza-Żydzik, Kulpa-Dybeł, Otmianowska-Mazur, Kowal, Soida2009, A&A498L, 21 Kulesza-Żydzik et al. 2010 send to publication

  8. Bars without CR driven dynamo

  9. Initial curve of rotation

  10. Resonanses ILR 0.24kpc, 4.64kpc CR 11.39kpc OLR > 15kpc ILR 0.33 kpc, 3.06 kpc CR 6.9 kpc OLR = 10.44 kpc ILR 0.69 kpc, 1.31 kpc CR 3.93 kpc OLR = 5.81 kpc

  11. Bars with CR driven dynamo Cosmic rays are included to calculate polarization maps Total magnetic energy

  12. Spirals and tidal forces r50a60 r50a00 Resolution 256 x 256 x 64 30 kpc x 30 kpc x 7.5 kpc Total mass: 810 x 109 Msun the second galaxy1010 Msun No CR driven dynamo

  13. r50a30 r50a30

  14. r100a00 r50a30

  15. Densities cuts r100a30 r50a60 r50a00

  16. r50a30

  17. Conclusions • In calculations of magnetic field evolution in barred • galaxies our model reproduces large-scale structures • of magnetic field observed in such galaxies. • In the same time our simulations solve the problem of • magnetic arms shift to inter-arm region. • Our second experiment shows that under influence oftidal forces galaxies form magnetic and spiral arms. • It also reproduces large-scale structures of magnetic field observed in spiral galaxies.

  18. Invitations to posters: Siejkowski et al. „Cosmic ray driven dynamo in the ISM of irregular galaxies” Kulpa-Dybeł et al. „Can turbulent reconnection be fast in 2D” Kulpa-Dybeł et al. „3D MHD simulations of magnetic field and radio polarization of barred galaxies”

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