Download Highlights of Spanish Astrophysics II: Proceedings of the by Raúl Jiménez (auth.), Jaime Zamorano, Javier Gorgas, Jesús PDF

By Raúl Jiménez (auth.), Jaime Zamorano, Javier Gorgas, Jesús Gallego (eds.)

This quantity files the contributions provided on the 4th medical assembly of the Spanish Astronomical Society (SEA). masking quite a lot of themes, the 146 contributed papers supply a finished assessment of the present country of Spanish astronomy. The lawsuits comprise precise reports facing the cosmological details got from galaxy spectra, supernovae at excessive redshift, black holes, dynamics of galaxy interactions, and non-LTE inversion of spectral strains.
The contents of those complaints therefore mirror the huge pursuits of the Spanish astronomical neighborhood. The symbolic importance of those complaints can hardly ever be exaggerated, due to the fact that the following, for the second one time, the ocean publishes the court cases of its personal clinical assembly.
This ebook is usually recommended to expert astronomers and astronomy graduate scholars all over the world.

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Extra resources for Highlights of Spanish Astrophysics II: Proceedings of the 4th Scientific Meeting of the Spanish Astronomical Society (SEA), held in Santiago de Compostela, Spain, September 11–14, 2000

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3. Star Formation Rates Estimates For each object the flux of the line is calculated as W N (Ff - Ff), with W N, the width of the narrow filter and F). the flux per unit wavelength in both thr broad (B) and narrow (N) filters. , 1997). With the corrected fluxes, the equivalent width of the lines and the luminosity of the objects is calculated. The luminosity functions are constructed dividing the number of objects by the volume of space covered by the narrow filter. This luminosity function is then fitted to a Schechter function minimizing X2 (Figure 1).

Thus, a continuation of the simulations beyond jet breakout is necessary (we have computed it for models C50 and C51). 8 R* passes over into an external uniform medium with a density 10- 5 gcm- 3 and a pressure 10- 8 p(R*). CATACLYSMIC PROGENITORS OF GAMMA-RAY BURSTS 6 ------ ..... _- ....... - ....... ~ 4 Q. II -6 -6 c ::E 30 -8 0 0 '" -' 25 .... 35 20 -10 15 -12 10 5 5 B 9 Log" r 10 10 15 20 25 30 Lorentz Factor Figure 1. Left: Lorentz factor (bottom) and rest-mass density (top) vs. 24s (solid), respectively.

PASCUAL AND J. GALLEGO Depto. de Astrofisica, Facultad de Fisicas, Universidad Complutense, E-28040 Madrid, Spain A. ARAGON-SALAMANCA School of Physics and Astronomy, University of Nottingham, Nottingham, NG72RD, England AND C. E. GARCIA-DABO AND J. ZAMORANO Depto. de Astrofisica, Facultad de Fisicas, Universidad Complutense, E-28040 Madrid, Spain Abstract. The Ho: line is a direct tracer of the recent star formation. 4, candidates to be emission-line galaxies are detected and the value of the Star Formation Rate (SFR) density is computed.

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