ZOOMING IN ON THE CORONAL POLES WITH SOLAR ORBITER

Transcription

1 ZOOMING IN ON THE CORONAL POLES WITH SOLAR ORBITER DAVID BERGHMANS 1, DAN SEATON 2,3, MATTHEW WEST 1 ON BEHALF OF THE EUI TEAM POLAR PERSPECTIVES MEETING, HAO, BOULDER, COLORADO SEPTEMBER ROYAL OBSERVATORY OF BELGIUM, BRUSSELS, BELGIUM 2CIRES, UNIV. OF COLORADO, BOULDER, COLORADO, USA 3NOAA NATIONAL CENTERS FOR ENVIRONMENTAL INFO., BOULDER, COLORADO, USA

2 SOLAR ORBITER OVERVIEW

3 Mission instruments sensing t e l o i v a r t l U e m e r t s Ex r e g a Im Sun-Facin g Side Both in-situ & remote

4 INSTRUMENTATION In Situ Remote Sensing EUI: Extreme Ultraviolet Imager EPD: Energetic Particle Detector METIS: Coronagraph MAG: Magnetometer PHI: Polarimetric and Helioseismic Imager RPW: Radio and Plasma Waves SoloHI: Heliospheric Imager SWA: Solar Wind Analyzer SPICE: Spectral Imaging of the Coronal Environment STIX: X-ray Spectrometer/Telescope

5 Solar Orbiter has shipped for its pre-flight test campaign in Germany as of this week. Solar Orbiter s heat shield with openings for remote-sensing instruments

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7 Solar Orbiter Orbits 4/ /2030 Image Courtesy ESA, 'CREMA report'

8 EXTREME ULTRAVIOLET IMAGER

9 Extreme Ultraviolet Imager Overview High Resolution EUV Full Sun Imager High Resolution Lyman-α

10 EUI = 3 Telescopes High Res. EUV EUV High Resolution Imager (HRI-EUV) 17nm High Res. Lyman-α Lyman alpha High Resolution Imager (HRI-Lya) 121nm Full Sun Imager (FSI) Full Sun Imager (FSI) 17nm 30.4nm

11 FSI: Full Sun Imager FOV: AU: 4 Rsun 4 Rsun 17nm 30.4nm SUVI 171 Å Mosaic Non-Operational Product resolution: 9 arcsec on AU =1830 km on 2 pixels

12 FSI: Full Sun Imager FOV: AU: 4 Rsun 4 Rsun 17nm 30.4nm SUVI 171 Å Mosaic Non-Operational Product resolution: 9 arcsec on AU =1830 km on 2 pixels

13 FSI: Full Sun Imager FOV: AU: 4 Rsun 4 Rsun 17nm 30.4nm SUVI 171 Å Mosaic Non-Operational Product resolution: 9 arcsec on AU =1830 km on 2 pixels

14 FSI: Full Sun Imager FOV: AU: 4 Rsun 4 Rsun 17nm 30.4nm SUVI 171 Å Mosaic Non-Operational Product resolution: 9 arcsec on AU =1830 km on 2 pixels

15 HRI:High Resolution Imagers FOV: AU = (0.16 R Sun ) 2 resolution: 1 arcsec on AU = 200km

16 Hi-C Sounding Rocket SDO/AIA Hi C Hi-C gives us a preview of what we will see with HRI EUV

17 METIS CORONAGRAPH & POLARIMETRIC AND HELIOSEISMIC IMAGER PHI provides full-disk and high res (up to 150 km) vector magnetic field and LOS velocity maps METIS observes the WL corona between 1.6 and 3.0 R Sun at closest approach

18 ZOOMING IN ON THE POLES

19 Like Juno: Discovery Science! NASA/JPL-Caltech/SwRI/ASI/INAF/JIRAM

20 QUESTIONS FOR A NEW VIEW Are polar coronal holes different from low-latitude coronal holes? How and why? Polar coronal holes don t experience differential rotation, the environment is much more static and PCH s are largely stable for much of the solar cycle. What does that mean for their evolution?

21 entire 15 months of SWAP data is available in the online material. Additionally, Figure 2 shows the schematic view of the evolution of the streamer/pseudostreamer magnetic field configuration. Before the pseudostreamer forms, a streamer encircles the entire pole, as seen in Figure 1A. The neutral line, corresponding to the filament channel, and base of the cavity (Vial and FIGURE 1 Evolution of the pseudostreamer observed with SWAP 174 Å w values. FIGURE 1 Evolution of the pseudostreamer observed with SWAP 174 Å waveband. Color scale is inverted, so black corresponds to the higher intens values. FIGURE 2 Schematic view of streamer to pseudostreamer transition (A,B) disappearance (D). The polarity inversion line is indicated by the dashed black line closed lines are in black. Frontiers in Astronomy and Space Sciences 6 FIGURE 2 Schematic view of streamer to pseudostreamer transition (A,B), followed by the shrinking of the pseudostreamer (C) until its comple disappearance (D). The polarity inversion line is indicated by the dashed black line; domains of opposite polarity are denoted by the open red and blue field lin closed lines are in black. FIGURE 1 Evolution of the pseudostreamer observed with SWAP 174 Å waveband. Color scale is inverted, so black corresponds to the higher intensity values. Guennou, Rachmeler et al. 2016

22 01 Jul I pol /I eq = Jul I pol /I eq = Jul I pol /I eq = Jul I pol /I eq =0.80 SOHO/EIT 304 Å Auchère et al. 2005

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26 PROBA2 SWAP 174 Å EUV Polar View June 2018 September 2018

27 SOLAR ORBITER MISSION PLANNING Operations must be planned far in advance (>6 months) Solar Orbiter Operation Plans (SOOPs) Other instruments can join and plan accordingly, but SO can t alter advance planning, so early science suggestions are welcome Remote Sensing: 10 day perihelion passes, 10 days high latitude (N/S), so 30 days per orbit with remote sensing In Situ: available all the time

28 DATA AVAILABILITY Limited Telemetry: 16,000 images per orbit, 320,000 mission lifetime Open data policy Low Latency data arrives within days (comparable to STEREO Beacon Data) Used for identifying important/disposable data Still in the planning stages Other data can be available in as long as six months available to the community on arrival, no embargo

29 EUI SCIENCE LEADS Pierre Rochus (PI, Belgium) David Berghmans (Co-PI, Belgium) Louise Harra (UK) Udo Schühle (Germany) Frederic Auchère (France) Werner Schmutz (Switzerland, Emeritus)