G R O U P R E S E A R C H E R S

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2 SW C O L L A B O R A T I O N J U P I T E R E A R T H G R O U P R E S E A R C H E R S Suwicha Wannawichian Tatphicha Promfu Paparin Jamlongkul Kamolporn Haewsantati 2

3 SW C O L L A B O R A T I O N C o l l a b o r a t i o n J U P I T E R E A R T H David Ruffolo John Clarke Jonathan Nichols Nicholas Achilleos Marrissa Voigt Licia Ray David Mkrtichian Napaporn A-thano Nikolai Østgaard Jone Reistad Finn Søraas Yukinaga Miyashita Mahidol University, Thailand Boston University, USA University of Leicester, UK University College London, UK Boston University, USA Lancaster University, UK NARIT NARIT University of Bergen, Norway University of Bergen, Norway University of Bergen, Norway Korea Astronomy and Space Science Institute Advisors Jupiter s aurora Earth s aurora 3

4 SW C O L L A B O R A T I O N J U P I T E R E A R T H A u r o r a & M a g n e t o s p h e r e Planets Earth Jupiter B surface (G) Rotation period (hr) Distance to magnetopause (R planet ) Auroral brightness (kr) R E 45 R J 10-10, krayleigh (kr) = 10 9 photon/sec from a 1 cm 2 column of the atmosphere radiated into 4 steradians Clarke et al.,

5 TP C O L L A B O R A T I O N J U P I T E R E A R T H J u p i t e r s O b s e r v a t i o n The effect of hot plasma pressure anisotropy in Jupiter's middle magnetosphere and Ganymede's magnetic footprint Tatphicha Promfu 5

6 TATPHICHA PROMFU M - I C o u p l i n g c u r r e n t s y s t e m Magnetosphere-Ionosphere coupling current system consists with Pedersen current (j i ), Equatorial radial current (I ρ ), and Field-aligned current (j ) Nichols et al.,

7 T A T P H I C H A P R O M F U P l a s m a p r e s s u r e a n i s o t r o p y Pressure anisotropy change the distribution of azimuthal current density a along a field line P h e P h e = when P dominate, it spreads current away from the equatorial plane P h e P h e = 1 when P dominate, the plasma pressure concentrates the azimuthal current in equatorial region P h e P h e = Nichols et al.,

8 TATPHICHA PROMFU R E S U L T Plot of Ganymede s magnetic footprint oval from Grodent et al., 2008 with the observational data in 2007 from Hubble Space Telescope. 8

9 TATPHICHA PROMFU R E S U L T Difference between Ganymede s and Io s footprint brightness variations shows that these two moons are under difference influences of magnetic field structure due to difference locations. 9

10 KH C O L L A B O R A T I O N J U P I T E R E A R T H J u p i t e r s O b s e r v a t i o n The morphology of bright spots emission in Jupiter s aurora and the relation with the solar wind Kamolporn Haewsantati 10

11 KAMOLPORN HAEWSANTATI J U P I T E R S A U R O R A Time-lapse video of Jupiter s auroras using far-ultraviolet-light observations made on May 19, 2016, with the Space Telescope Imaging Spectrograph aboard NASA's Hubble Space Telescope (HST). Credit: NASA, ESA, and J. Nichols (University of Leicester) Publication: June 30,

12 SW C O L L A B O R A T I O N J U P I T E R E A R T H J u p i t e r s O b s e r v a t i o n Influence of plasma in the vicinity of Io on Brightness and Angular Extension of Io s Magnetic Footprint Suwicha Wannawichian 12

13 SW R E S U L T Above figure shows the angular sizes of Io s magnetic footprint (blue dots) in Jupiter s northern auroral region from HST observations during the 2007 campaign in comparison with the magnetic footprint brightness (black dots). 13

14 Output Promfu T., S. Wannawichian, J. D. Nichols, and J. T. Clarke, Periodic behaviors of Io s and Ganymede s magnetic footprints, J. Geophys. Res., in progress (Impact Factor 3.44) Promfu T., S. Wannawichian, and J. D. Nichols, The investigation of Jupiter s radio emission under the influence of Ganymede s magnetic footprint, East-Asia ALMA Science Workshop, November 27-29, 2017, Korea Astronomy and Space Science Institute in Daejeon, Republic of Korea Promfu T., S. Wannawichian, J. D. Nichols, and J. T. Clarke, The study of Jovian magnetospheric plasma using the investigation of satellite footprints brightness, The Siam Physics Congress (SPC2018), May 21-23, 2018, Phisanulok, Thailand Wannawichian S., J. T. Clarke, and J. D. Nichols, Angular Size of Io Magnetic Footprint s Main Alfvèn Wing Spot: In Corresponding to Satellite s Locations, Magnetospheres of the Outer Planets Conference, July 9-13, 2018, Boulder, CO, USA Wannawichian S., J. T. Clarke, and J. D. Nichols, Radio emission from Jupiter as an indicator of auroral magnetic footprint morphology, East-Asia ALMA Science Workshop, November 27-29, 2017, Korea Astronomy and Space Science Institute in Daejeon, Republic of Korea Wannawichian S., A. Laphirattanakul, Influence of plasma in the vicinity of Io on Brightness and Angular Extension of Io s Magnetic Footprint, Chiang Mai J. Sci., 2018, submitted (Impact Factor 0.437)

15 PJ C O L L A B O R A T I O N J U P I T E R E A R T H E a r t h s O b s e r v a t i o n Time variations of OI5577Å emission line and solar wind data including with magnetometer data for investigation of low-latitude aurora Paparin Jamlongkul 15

16 PAPARIN JAMLONGKUL Space-Based Observation vs Ground-Based Observation Solar wind and IMF data vs OI5577Å emission intensities Ground-Based Observation vs Ground-Based Observation SYM/H index and AE index vs OI5577Å emission intensities 16

17 PAPARIN JAMLONGKUL G ro u n d - B a s e d O b s e r vation: O I Å e m i s s i o n i n t e n s i t i e s NARIT Harrison, 2011 Ground-based observational data were obtained by a medium Resolution Echelle Spectrograph (MRES) along with a 2.4 meters diameter telescope at Thai National Observatory, Intanon Mountain, Chiang Mai, Thailand 17

18 PAPARIN JAMLONGKUL M E T H O D DATA R E D U C T I O N Spectral image processing Total Commander Program Dech95-2D Image Processing Program Spectral line profile processing Dech-Fits - Spectra Processing (FITS) Program Wavelength (Angstrom) Intensity (ADU) Pixel 18

19 PAPARIN JAMLONGKUL S p a c e - B a s e d O b s e r vation: Wind spacecraft: locating around L1 point around > 200R E aligning to the sun Study solar wind and Earth s magnetosphere S o l a r w i n d a n d i n t e r p l a n e t a r y m a g n e t i c f i e l d ( I M F ) d a t a ACE spacecraft: locating around L1 point around > 200R E aligning to the sun Monitor solar wind and the interplanetary medium Credit: 19

20 I (ADU) I (ADU) PAPARIN JAMLONGKUL D A T A G ro u n d - B a s e d O b s e r vation: O I Å e m i s s i o n i n t e n s i t i e s 12 dark sky frames with exposure time 30 min, on the nights of 15 th and 16 th February, 2018, during 12:00-22:00 UT Intensity (OI 5577Å) vs Time (UT) :12 14:24 15:36 16:48 18:00 19:12 20:24 21:36 Time (UT) Intensity (OI 5577Å) vs Time (UT) :12 14:24 15:36 16:48 18:00 19:12 20:24 21:36 Time (UT) 20

21 PAPARIN JAMLONGKUL R E S U L T February 15 th, 2018 C o r r e l a t i o n s b e t w e e n s o l a r w i n d / I M F a n d O I Å e m i s s i o n i n t e n s i t i e s February 16 th,

22 SW C O L L A B O R A T I O N J U P I T E R E A R T H E a r t h s O b s e r v a t i o n Substorm onset determination based on POLAR/VIS and POLAR/UVI observations Suwicha Wannawichian 22

23 SW R E S U L T Earth auroral phases, growth, expansion, and recovery phases, are the signatures of Earth s substorm event in the polar regions, as seen from figure below (adapted from Akasofu, 1964). Above, auroral emissions in Earth s northern hemisphere were observed in November 6, 1998, by the Visible Imaging System (VIS) and the Ultraviolet Imager (UVI), instruments onboard POLAR spacecraft. 23

24 SW R E S U L T In addition, the time series plot of integrated auroral flux at magnetic latitude between degrees and magnetic local time between hr was used to assist the determination of onset time. In below figure, time series plot shows the brightening of integrated photon flux of wavelength (dotted), (solid), (dashed), and (long dashed) nm emissions. 24

25 Output Wannawichian S. and Y. Miyashita, Substorm onset determination based on POLAR/VIS and POLAR/UVI observations, The Siam Physics Congress (SPC2018), May 21-23, 2018, Phisanulok, Thailand Jamlongkul P., and Wannawichian S., Time variations of OI5577Å emission line and solar wind data including with magnetometer data for investigation of low-latitude aurora, Thai Space Physics 2018 meeting, July 16, 2018, Mahidol University, Bangkok, Thailand

26 Output Prof. Nick Achilleos Dr. Patrick Guio Assoc. Prof. Jonathan Nichols Assist. Pfof. Licia Ray

27 THANK YOU Great appreciation for our collaborators and additional grants. We would like to express our gratitude for the support from National Astronomical Research Institute of Thailand (Public Organization)