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2015

AN Volume 336 Issue 5 (2015)

• M. Kadler and R. Ojha on behalf of the TANAMI Collaboration, page 499ff:
  • Movie 1 (0.7MB)
    This movie shows the structural evolution of the inner 60 mas of the Cen A jet-counterjet system. The movie is based on eight images obtained by TANAMI between 2007 and 2011, which were convolved with a common beam as indicated by the grey ellipse in the bottom left corner and interpolated between the individual observations. The color scale was fixed to the minimum and maximum flux density of the images. The contour lines start at three times the maximum noise level of the images and increase logarithmically by factors of two.
    

2007

AN Volume 328 Issue 10 (2007)

• S.C. Marsden et al., page 1047ff:
  • Movie 1 (6.1 MB)
    Maximum entropy brightness image reconstruction of IM Peg for rotational cycle 120 from the AST data. The image is a flattened polar projection extending down to a latitude of -60°. The bold line denotes the equator and the radial ticks around the image indicate the phases at which the star was observed.
• M. Steffen, B. Freytag, page 1054ff:
  • Movie 1 (6.1 MB)
    Time sequence showing the evolution of the surface convection pattern of the non-rotating mini-sun M25 over a period of 3 hours. The color-coded quantity is the simulated emergent (gray) continuum intensity (cf. top row of Fig.7).
  • Movie 2 (5.9 MB)
    Pole-on view of the time evolution of the convection pattern at the surface the rotating mini-sun M35 over 3 hours. The rotation period of the rigidly rotating core is 1 hour. (cf. middle row of Fig.7).
  • Movie 3 (6.2 MB)
    As Movie 2, but showing the equator-on view of the emergent intensity obtained for rotating mini-sun M35 (cf. bottom row of Fig.7).
• E. Isik, D. Schmitt, M. Schüssler, page 1111ff:
  • Movie 1 (5.0 MB)
  • Movie 2 (5.9 MB)
  • Movie 3 (0.1 MB)
    

2004

AN Volume 325 Issue 3 (2004)

• R. Baptista, page 179ff:
  • Movie 1 (4.0 MB)
  • Movie 2 (3.7 MB)
• D. Steeghs, page 183ff:
  • Movie 1 (2.0 MB)
  • Movie 2 (1.4 MB)
• A. Schwope et al. page 195ff:
  • Movie 1 (3.0 MB)
    One-pole accretion geometry and high orbital inclination (HU Aqr-like). Inclination 85.0 degree, mass ratio Q = M1/M2 = 1.5.
    Dipol: Azimuth: 45.0 degree, Colatitude: 12.0 degree
    Curtain: Azim.-Start: 01.0 degree, Azim.-End: 63.0 degree
    v-Max: 600.0 km/s (means: v >/< +/- 600 km/s = red/blue)
  • Movie 2 (0.9 MB)
    Two-pole accretion geometry and intermediate orbital inclination (AM Her-like), Inclination 45.0 degrees, mass ratio Q=1.5.
    Dipol: Azimuth: 0.0 degree, Colatitude: 14.5 degree
    Curtain: Azim.-Start: 40.0 degree, Azim.-End: 170.0 degree
    First: 40-70
    Second: 72-170
    v-Max: 600.0 km/s (means: v >/< +/- 600 km/s = red/blue)
    

2002

AN Volume 323 Issue 3-4 (2002)

• B. Freytag, M. Steffen, B. Dorch, page 213ff:
  • Movie 1 (5.9 MB)
• A. Brandenburg, W. Dobler, page 411ff:
  • Movie 1 (0.9 MB)
    Spectra of magnetic and kinetic energies (solid and dotted lines, respectively), together with the modulus of the magnetic helicity spectrum scaled by k/2 (dashed line), which must always be below the magnetic energy curve. The red and blue dots on the dashed curve indicate positive and negative values, respectively. Note that at early times the magnetic helicity is positive at small scales (wavenumbers k > 7-8) and negative at larger scales. The magnetic energy spectrum becomes visible after t>100, but it is then still dominated by small scales, as seen in the spectra as well as xz slices of Bx, By and Bz (below). This is Run 3 of B01. The estimated ratio of turbulent to microscopic magnetic diffusivity is between 20 and 40. Note the formation of a large scale component in addition to a persistent small scale component. The large scale field is of Beltrami type, where the three components are roughly Bx(x,z)=sinx, By(x,z)=0, and Bz(x,z)=cosx. The magnetic Prandtl number is unity, and the forcing wavenumber is 5.
  • Movie 2 (1.5 MB)
    like Movie 1, but with a magnetic Prandtl number of 100, and a kinetic Reynolds number of about unity. Note that at small scales the magnetic energy exceeds the kinetic energy. The large scale magnetic field takes longer to build up. This is because of the larger magnetic Reynolds number which makes it harder to build up the magnetic helicity associated with the large scale field.
  • Movie 3 (0.5 MB)
    like Movie 1, but with a forcing wavenumber of 30. The large scale field is now much cleaner. This is due to a suppression of magnetic energy at intermediate wavenumbers (between k=2 and about 20).

The movies in mpeg-format can be viewed using an mpeg-player; see www.mpeg.org.