Titlebook: Visualization in Scientific Computing ’97; Proceedings of the E Wilfrid Lefer,Michel Grave Conference proceedings 1997 Springer-Verlag/Wein

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書(shū)目名稱Visualization in Scientific Computing ’97影響因子(影響力)學(xué)科排名




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書(shū)目名稱Visualization in Scientific Computing ’97讀者反饋學(xué)科排名

西瓜

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Xiaoyang Mao,Makoto Kikukawa,Noboru Fujita,Atsumi Imamiya.Interstellar optical absorption lines and H. 21-cm emission lines show a number of very large aggregates with properties similar to those of ‘cloud complexes’. At nonzero velocities especially for . < 0°, exist optical lines which have no Hi counterparts. These are almost certainly produced in low-

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T. C. Sprenger,M. H. Gross,A. Eggenberger,M. Kaufmannerable at 14.6-m wavelength and used this instrument to study local radio disturbances. He found that the static that was received usually could be categorized by one of the following descriptions: intermittent and strong, intermittent and weak, or very steady and weak. The first two types of static

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Freek Reinders,Frits H. Post,Hans J. W. Spoeldert studies of H II regions (see, for example, review by Wynn-Williams and Becklin 1974) and of the Becklin-Neugebauer source in Orion (Penston, Allen and Hyland 1971) over the next few years generally confirmed the expectation that hydrogen recombination lines were to be found in H II regions but not

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Kalpathi R. Subramanian,Dina M. Lawrence,M. Taghi Mostafavirder to investigate the spatial distribution of these two types of physically variable stars in the galaxy. The work was intended to be complete down to a photographic magnitude of 13.14 at maximum ligth for all stars officially named and classified as Mira or SRa (period > 95 days) in the General C