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Journals and Conferences
The well-known analytical solution of Burgers’ equation is extended to curvilinear coordinate systems in three-dimensions by a method which is much simpler and more suitable to practical applications than that previously used . The results obtained are applied to incompressible flow with cylindrical symmetry, and also to the decay of an initially… (More)
The vector Burgers equation is extended to include pressure gradients and gravity. It is shown that within the framework of the ColeHopf transformation there are no physical solutions to this problem. This result is important because it clearly demonstrates that any extension of Burgers equation to more interesting physical situations is strongly limited.
We discuss a large flare that was observed simultaneously by RHESSI in hard X–rays and by the Nobeyama Radio Heliograph (NoRH) in microwaves. The imaging observations made both by RHESSI and NoRH show many interesting features which may be relevant for producing realistic flare models.
We investigate accelerated electron energy spectra for different sources in a large flare using simultaneous observations obtained with two instruments, the Nobeyama Radio Heliograph (NoRH) at 17 and 34 GHz, and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) at hard X-rays. This flare is one of the few in which emission up to energies… (More)
We developed a method for making quantitative characterizations of bi-grid rotating modulation collimators (RMC's) that are used in a Fourier transform x-ray imager. With appropriate choices of the collimator spacings, this technique can be implemented with a beam-expanded He-Ne laser to simulate the plane wave produced by a point source at infinity even… (More)
Aims. We present a summary of the analysis of thirty microflares, observed simultaneously by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in hard X-rays and by Nobeyama RadioHeliograph (NoRH) in microwaves (17 GHz). Methods. We used microflares observed by RHESSI in the energy range 3−25 keV, and for larger events, up to 35 keV. The… (More)
1. V. V. Zhelkznyakov, Sov. Astron. AJ 6, 3 (1962); T. Kakinuma and G. Swarup, Astrophys. J. 136, 975 (1962); M. R. Kundu, Solar Radio Astronomy (Interscience, New York, 1965); P. Lantos, Ann. Astrophys. 31, 101 (1968); E. Ya. Zlotnik, Sov. Astron. AJ 12, 245 (1968); ibid., p. 464; V. V. Zheleznyakov, Radio Emissionfrom the Sun and Planets (Pergamon, New… (More)