Io, one of the Galilean moons, is well known for its volcanic activity. Io's atmosphere consists of volcanic gas whose main constituent is SO2 [e.g., Lellouch et al., 2007]. This volcanic atmosphere is continuously escaping from Io. Particularly, Io's atmosphere becomes magnetospheric plasma through photo-ionization or particle impacts and forms a structure called Io plasma torus. Jupiter's inner magnetosphere is therefore populated with heavy ions of iogenic origin. Neutral particles are produced through the Io plasma torus. For example, NaCl+ ions picked up by Jupiter's corotating magnetic fields from Io's ionosphere and their subsequent destruction by recombination with ambient electrons in the Io plasma torus produce a flow of fast neutral sodium atoms called a " stream" [e.g., Schneider et al., 1991; Wilson et al., 2002]. These fast neutral sodium atoms also form a great nebula [e.g., Mendillo et al., 1990]. [Lellouch et al., 2003] suggested that the most likely source of the NaCl atmosphere seems to be direct volcanic output. This volcanically supplied NaCl gas is immediately ionized in Io's day-side ionosphere, and it goes to the Io plasma torus afterward. The average lifetime of NaCl+ in the torus is 10 hours [Schneider and Wilson, 1994]. This means the supply rate of Na atoms forming the sodium nebula reflects the volcanic output on Io with a time scale of ~ 10 hours. Although Jupiter's inner magnetosphere is populated by iogenic plasma, influence from the solar wind is not negligible. [Desch and Barrow 1984], [Gurnett et al., 2002], and [Nakagawa et al., 2000] showed that Jupiter's hectometric radio emission, called HOM, depends on the solar wind dynamic pressure. The source regions of HOM are located in Jupiter's inner/middle magnetosphere [Ladreiter et al., 1993; Zarka et al., 2001], and HOM activity seems to reflect Jupiter's auroral activity. In fact, [Gurnett et al., 2002] showed that strong HOM emissions and Jupiter's UV aurorae are triggered by shocks in the solar wind. They concluded that HOM is an index of Jupiter's auroral activity and corresponds to Auroral kilometric radiation (AKR) on the earth. While Jupiter's inner magnetosphere is dominated by the planetary rotation as an energy source and Io as a plasma and neutral source, its variability seems, at least partially, controlled by the solar wind. The following question arises: " How does Io's volcanic activity contribute to Jupiter's magnetosphere?" Several studies aimed at observing Jupiter's sodium nebula or sulfur ion emissions from Io plasma torus have shown that Io's volcanic supply varies [Brown and Bouchez, 1997; Mendillo et al., 2004; Nozawa et al., 2005; Yoneda et al., 2009; oneda et al., 2010]. However, with exception of [Bonfond et al., 2012], no previous study has shown a dependence of Jupiter's magnetospheric activity, such as aurora, on Io's volcanic supply yet. In this study, we resolve this question by focusing on the D-line brightness from Jupiter's sodium nebula and HOM activity. Although there are other radio emissions that are also thought to be related to aurora activity on Jupiter, direct relations with the aurora have been seen only in HOM [Gurnett et al., 2002]. Particularly, [Zarka et al., 2001] suggested that the HOM emission comes from regions in L-shell of 7–30 Rj. This includes the source regions of the main oval aurora. Therefore, HOM is the most reliable index to infer the aurora activity, especially the main oval aurora.