Solar wind effects on Jupiter non-Io DAM emissions during Ulysses distant encounter (2003–2004)
E. Echer1, P. Zarka2, W. D. Gonzalez1, A. Morioka3 and L. Denis4
Instituto Nacional de Pesquisas Espaciais, Sao Jose dos Campos, SP, Brazil e-mail: firstname.lastname@example.org
2 Observatoire de Paris, Meudon, France
3 Planetary plasma and atmospheric research center, Tohoku University, Sendai, Japan
4 Observatoire de Paris, Station de Radioastronomie, Nançay, France
Accepted: 11 May 2010
Aims. We analyze solar wind data from the Ulysses spacecraft during the distant Jupiter encounter from 2003 November to 2004 March as well as Nançay decametric (DAM) radio observations non-controlled by Io.
Methods. The Ulysses solar wind data are balistically propagated towards Jupiter and are correlated with Nançay non-Io DAM emissions.
Results. It is found that the average solar wind dynamic pressure around the time of DAM emissions is 1.7 times higher than its average value during the Ulysses encounter. The occurrence of fast forward (FS) and reverse (RS) interplanetary shocks and heliospheric current sheet crossings (HCS) is correlated with the occurrence of non-Io DAM emissions. We note an enhanced probability of occurrence of non-Io DAM emissions after the expected arrival of FS, RS and HCS at Jupiter. However, about half emissions (54%) did not seem to be associated with these interplanetary structures. We also note that the average duration and power of non-Io DAM emissions are enhanced during periods associated with those interplanetary structures.
Conclusions. From the results obtained in this work it seems that non-Io DAM emissions occur during intervals of enhanced solar wind dynamic pressure. Yet, there is no direct correlation between the non-Io DAM emissions duration or power versus the solar wind pressure values and the interplanetary shock Mach number.
Key words: planets and satellites: general / solar wind
© ESO, 2010