The planetary spin and rotation period: a modern approach |
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| Authors: | A I Arbab Saadia E Salih Sultan H Hassan Ahmed El Agali Husam Abubaker |
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| Institution: | 1. Department of Physics, Faculty of Science, University of Khartoum, P.O. Box 321, Khartoum, 11115, Sudan
2. Department of Physics, College of Applied and Industrial Science, University of Bahri, Khartoum, Sudan
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| Abstract: | Using a new approach, we have obtained a formula for calculating the rotation period and radius of planets. In the ordinary gravitomagnetism the gravitational spin (S) orbit (L) coupling, $\vec{L}\cdot\vec{S}\propto L^{2}$ , while our model predicts that $\vec{L}\cdot\vec{S}\propto\frac{m}{M}L^{2}$ , where M and m are the central and orbiting masses, respectively. Hence, planets during their evolution exchange L and S until they reach a final stability at which MS∝mL, or $S\propto\frac{m^{2}}{v}$ , where v is the orbital velocity of the planet. Rotational properties of our planetary system and exoplanets are in agreement with our predictions. The radius (R) and rotational period (D) of tidally locked planet at a distance a from its star, are related by, $D^{2}\propto\sqrt{\frac{M}{m^{3}}}R^{3}$ and that $R\propto\sqrt{\frac {m}{M}}a$ . |
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