segunda-feira, 26 de abril de 2010

Leis de Kepler e órbitas dos planetas


Johannes Kepler (1571-1630), discípulo de Tycho Brahe, utilizando os dados colhidos por seu mestre, descreveu, de modo singelo e preciso, os movimentos planetários.
Primeira lei:
Um planeta se move descrevendo uma órbita elíptica tendo o Sol como um dos focos. Ver esquema.
Segunda lei:
A linha que liga o Sol ao planeta varre áreas iguais em intervalos de tempo iguais. Ver esquema.
Terceira lei:
É constante para todos os planetas a razão entre o tempo (T) que o planeta leva para dar uma volta completa em torno do Sol elevado ao quadrado e o raio médio (r) de sua órbita elevado ao cubo. T2/r3 = constante. As leis de Kepler aplicam-se a quaisquer corpos que gravitem em órbita de uma grande massa central. Ver esquema.
Por isso, elas são aplicáveis não apenas ao nosso Sistema Solar, como também a outros sistemas do Universo. Elas podem ser também ser aplicadas, por exemplo, para um satélite que gravite em órbita de um planeta qualquer. 
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