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Extra resources for A Statistical Discussion of Sets of Precise Astronomical Measurements III; Masses of the Stars

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The geocentric phase o£ Io during periods o£ decametric emission. We have chosen a period £or which both solar wind data and Jupiter observations are available, that is £rom August 1964 to November 1964, £rom September 1966 to March 1967 and £rom November 1967 to April 1968. We have analyzed the Jupiter observations £rom Boulder and Florida observatories. For these observations, we have distinguished the emission related to the 90 0 Io phase (70 0 < ~ 110 0 ) , that is the "Early Io" storms, and the emission related to the 240 arc deg Io phase (150 0 ci 350 0 ) , that is "Late-Io" storms j this terminology is the same as de£ined by Duncan (1970).

Quemadatt t Observatoire de Paris, Meudon tt Groupe de Plasmas Stellaires et Planetaires, Universite de Paris INTRODUCTION The modulation by 10 of the rate of occurrence of radiobursts from Jupiter is well known (Bigg 1964), and many authors have tried to explain this influence of 10 on the emission of the radiobursts. Duncan (1970) proposed that 10 stimulates the emission when it crosses the Rmagnetopause" of Jupiter. Melrose (1967) suggested that the motion of 10 through a "corotating region" inside the magnetosphere of Jupiter may be the cause.

710 $. It is the isorotation model of Ferraro. In this case the convective field is found to be about 200 mv/m when the plasmapause lies at 6 RJ • 2) If the conductivity of the magnetospheric plasma has a finite value, that is the equilibrium state is different from the isorotation, then the plasma may be stabilized in a partial corotation (Alfven, 1968). 35 STUDY OF A JOVIAN PLASMASPHERE velocity In this case the plasma is carried away at the V= (1 /3 K}1I. / '(' ) ¥L where K is the gravitational constant, m the Jupiter mass, and r the distance.

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A Statistical Discussion of Sets of Precise Astronomical Measurements III; Masses of the Stars by Edwin Bidwell Wilson


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