Japan Geoscience Union Meeting 2019

Presentation information

[E] Poster

P (Space and Planetary Sciences ) » P-PS Planetary Sciences

[P-PS01] Outer Solar System Exploration Today, and Tomorrow

Tue. May 28, 2019 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Jun Kimura(Osaka University), Yasumasa Kasaba(Planetary Plasma and Atmospheric Research Center, Tohoku University), Kunio M. Sayanagi(Hampton University)

[PPS01-P05] Pulsation-like variation of Jovian infrared polar emission observed by Subaru 8-m: H3+ and methane emissions

*Yasumasa Kasaba1, Haruna Watanabe1, Hajime Kita2, Chihiro Tao3, Takeshi Sakanoi1, Masato Kagitani1, Orton Glenn1,4, James Sinclair4 (1.Planetary Plasma and Atmospheric Research Center, 2.ISAS/JAXA, 3.NICT, 4.NASA/JPL)

Keywords:Jupiter, polar emission, H3+, CH4, short time variations

In the Jovian high-latitude region, there are emissions with various wavelengths ranges, morphologies, and time variations. They are important tracers of energy injection carried by auroral particles that precipitate from the magnetosphere. The polar IR emissions excited in the Jovian upper atmosphere, which include the H3+ aurora and thermal emissions of hydrocarbons, reflect not only the abundance of emission sources but also the thermal structures. Both are affected by auroral precipitation into the source region. It is known that, in the polar region inner than the auroral oval, the flux of auroral precipitation can have time variations over various scales from years to seconds.

The H3+ aurora observed in near infrared is emitted in thermosphere / ionosphere from thermally excited H3+ ions above the CH4 homopause. Auroral precipitation ionized H2 and produce H3+ ions through ion chemistries. In previous observational studies, the shortest timescale of H3+ auroral intensity change was ~30 min, but detected by ~16-min step imaging. We performed the temporal imaging observation of the Jovian H3+ IR aurora with Subaru/IRCS and the H3+ narrow-band filter on 31 January 2015 and 25 May 2016. The adaptive optics enabled us to see the target with high spatial resolution (~0.2 arcsec). From the images obtained with time resolution of ~150 s on 25 May 2016, we detected a patch-like auroral feature pulsating with a period of ~10 min in noon sector of northern polar region. On the other hand, we could not find any periodic variations from the data obtained on 31 January 2015, which was obtained as slit-viewer image for the other study, and whose time intervals of ~10–30 min every several images was not optimized to this research. In addition, the location where the patch-like emissions observed with high intensities on 25 May 2016 were not so bright on 31 January 2015. The patch-like auroral feature that was pulsating during our observation period on 25 May 2016 have been sometimes observed in UV, but not always. Previous UV observations reported some pulsating auroral features with the periods of ~2–11 min in the northern polar region. However, the locations of them are not consistent with the patch-like feature in this study. The pulsation period of the X-ray aurora, which has a hot spot coinciding with our patch-like IR aurora, is 40–50 min. This region is estimated to connect magnetically to out of the magnetopause, and auroral precipitation there can be caused by dayside reconnection between the Jovian magnetospheric field and interplanetary field.

On the other hand, the hydrocarbon polar emission observed in mid-infrared is emitted from the whole stratosphere. From their locations and morphologies, it is estimated to be related with auroral particles penetrating under the homopause. However, the mechanisms of this link (composition change and/or heating by particle precipitations) are not well understood. Previous studies found the intensity time variation of polar CH4 emission over days and months. We tried to detect the time variation of CH4 emission intensity by continuous imaging observations of the northern polar region over several tens of minutes on 31 March, 24 and 25 May 2018 with Subaru/COMICS. We obtained the images using the 7.8 μm filter, which is sensitive to the CH4 thermal emissions occurring in the pressure range of 20–0.5 mbar and 1 μbar in the Jovian upper stratosphere, with time resolution of ~1 min. On all observation days, the polar region was not bright in 7.8 μm. In addition, we could not find clear time variations of polar CH4 emission intensity during our observation periods, 25, 50 and 60 min on 31 March, 24 and 25 May 2018. This observation result is consistent to the model estimation by Kuroda et al. [2014], which suggested the relaxation time of hydrocarbon thermal emissions in the Jovian upper stratosphere, where is a possible source region of polar CH4 emission, is at least ~105 s (~28 h).