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We present λ3.5 cm and λ6.2 cm radio continuum maps in total and polarized intensity of the barred galaxies NGC 1097 (at 2′′–15′′ resolution) and NGC 1365 (at 9′′–25′′ resolution). A previously unknown radio galaxy southwest of NGC 1097 is reported. Apart from a smooth faint envelope and a bright central region, both galaxies exhibit radio ridges roughly(More)
The Herzenberg dynamo, consisting of two rotating, electrically conducting spheres with non-parallel spin axes, immersed in a nite, spherical conducting medium, is simulated numerically for a variety of parameters not accessible to the original asymptotic theory. Our model places the spheres in a spatially periodic box. The largest growth rate is obtained(More)
Photosensitive effects distinguished as type I and type IIA photosensitivity within optical fibers were observed in a much more pronounced form within germanosilica waveguides deposited by hollow-cathode plasma-enhanced chemical-vapor deposition. With increasing exposure to 193-nm UV light, positive index changes greater than 2 x 10(-3) were observed,(More)
  • J . S . Rodwell, J . H . J . Schamin, L . Mucina, S . Pignatti, J . Dring, Derek Moss
  • Folia Geobotanica
  • 2007
E. Edgar & H.E. Connor: Flora of New Zealand. Vol. 5, Gramineae; Manaal~" Whenua Press, Lincoln, 2000, 650pp. Price USD 55.-, ISBN 0-478-09331-4. The present volume completes the Flora of New Zealand series started in 1961. It covers the family Gramineae, represented in New Zealand by 188 native and 226 naturalized species. The treatment is based on many(More)
Key words magnetic fields – magnetohydrodynamics (MHD) Although current interest in astrophysical dynamo theory is largely focussed on flows with both large-and small-scale motions, historically the study of dynamos driven by laminar flows has been important. Some classical laminar flow dynamos are reviewed. These results were obtained in an asymptotic(More)
The up-turn in Euclidean normalised source counts below 1mJy at 1.4GHz is well established in many deep radio surveys. There are strong reasons, observationally and theoretically, to believe that this up-turn is due to strong evolution of the starforming population up to z=2. However this hypothesis needs further confirmation spectroscopically and the(More)
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