By James E. Huheey, Elle A. Keiter, Richard L. Keiter
Los autores exponen en esta obra el conjunto primary de temas que conforman esa disciplina, así como algunos otros que los estudiantes y los maestros pueden encontrar interesantes.
Completamente actualizado, el libro incluye una introducción a los grupos puntales, un nuevo capítulo sobre simetría, otro sobre enlace y otros más que incluyen espectroscopia y cristalografía, todos ellos profusamente ilustrados y ejemplificados con objeto de ser más entendibles.
Los lectores de esta obra pueden provenir de ramas diversas, con experiencia en fisicoquímica y química orgánica. Sin embargo, para muchos este libro será el primer contacto con los angeles química inorgánica, por lo que los primeros capítulos presentan los fundamentos de los angeles estructura atómica y molecular desde l. a. perspectiva de los angeles química inorgánica.
Al terminar el estudio del libro, se espera que el estudiante comprenda cabalmente los angeles enorme diversidad de los angeles química inorgánica, l. a. cual estudia 109 elementos, cada uno con sus propias características.
Estudio de estructuras, reactividad, catalizadores, estabilidad termodinámica, simetría, técnicas experimentales, fases gaseosas, soluciones, química del estado sólido, entre otros.
Desde los primeros tiempos, el hombre se interesó por aprovechar los minerales en beneficio propio. Sin embargo, sus conocimientos eran pragmáticos. Con el tiempo, el conocimiento sobre los minerales se aplicó a los angeles extracción de metales preciosos y, de ese modo, l. a. química inorgánica fue ganando terreno hasta convertirse en los angeles base teórica para l. a. explotación racional no sólo de los minerales, sino de las moléculas y átomos que los componen.
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Extra resources for Química inorgánica
Example text
Niemann, H. , W. Kasprzak, A. Hedin, D. Hunten, and N. Spencer, Mass spectrometric measurements of the neutral gas composition of the thermosphere and exosphere of Venus, J. Geophys. , 85, 7817, 1980. 25. Fox, J. , and S. W.
Despite this marked variation, it is useful to provide average values for the parameters describing the interplanetary medium near the Earth, for which there is a large body of measurements. The Earth’s orbit is approximately 217 solar radii from the Sun, which is defined to be one astronomical unit (1 AU ≈ 150 million km). 24 66 81 wind plasma generally takes 2 to 3 days to reach the Earth. Near the Earth the speed ranges from 200 to 900 km s−1 and the density varies from 1 to 80 cm−3 . As the plasma moves away from the Sun, it expands and cools, with the electron temperature decreasing from about one million kelvin in the corona to about 100 000 K near the Earth.
The fact that the β of the plasma is greater than unity for all solar wind conditions means that the magnetic field is relatively weak and is carried along with the flow. In and close to the solar corona, however, the β of the plasma is much less than unity, which indicates that the magnetic field is strong and directs the flow. 3 is that the solar wind velocity is much greater than both the Alfvén wave speed and the ion-acoustic speed, which means that the solar wind is supersonic at 1 AU. 9 Variation of the solar wind velocity (top left panel), density (middle left panel), temperature (bottom left panel), and interplanetary magnetic field (right panel) with distance from the Sun.