The Solar-C; Current status

Transcription

1 The Solar-C; Current status Kiyoshi Ichimoto (Kyoto Univ./NAOJ) and SOLAR-C Working Group Sac Peak Workshop, ; High-resolution solar physics: past, present, future

2 Many Hinode results are related to fundamental MHD processes. waves What we learned from Hinode; magnetic reconnection - Large scale dynamics of the Sun are emerged from the causal chain of small scale (elementary) plasma flows processes. - The chromosphere (interface between photosphere and corona) is extremely dynamic and of turbulence critical importance for understanding the origin of the solar dynamic atmosphere. Local dynamo instability magneto-convection

3 The Solar-C concept (2015 proposed) Objective ; to understand the plasma dynamics as a system that connects the solar surface to the solar corona and interplanetary space, and to investigate the elementary processes that take place universally in cosmic plasmas. EUV spectrograph (EUVST ) + IM (Irradiance Monitor) ESA Gap of Hinode observation JAXA Optical telescope (SUVIT, f1.4m) SUVIT focal plane NASA High resolution corona imager (HCI) Jump from Hinode mass: (1) Advanced spectro-polarimetry determine 3D magnetic field (2) High spatial resolution x 10 for corona, x 3 for photo./chrom. (3) High throughput high time resolution & sensitivity x 10 (4) Wide wavelength coverage accessible to all layers of Sun s atmosphere 2300kg size:3.7 x 3.2 x 7.3m orbit:gyo-synchronus

4 Mission proposal of Solar-C; Solar-C mission proposal was submitted to JAXA Strategic Large mission (2015.2), and to ESA M4 as EPIC (European Participation In Solar-C, ) Solar-C was not selected for the final candidates by ESA and JAXA, though it was highly ranked by evaluation committees. Size of the mission (total cost) was certainly an issue. SC Working Group decided to continue the effort to reestablish a mission concept for the next opportunity of JAXA Strategic Large mission

5 Approach to sharpen the mission concept Take the synergy with DKIST / EST utmost Reduce the aperture of SUVIT from 1.4m to 1m and emphasize the advantage of space, i.e., large FOV, continuous time coverage in high precision spectro-polarimetry Minimize the wavelength coverage without significant loss of science Eliminate a UV channel in SUVIT and solar irradiance monitor Consider a possible descope of EUVST (wavelength, resolution) Consider opportunities of small size missions to realize a part of Solar-C Joint Team (JAXA+NASA+ESA, Next Generation Solar Physics Mission - Science Definition Team; NGSPM-SOT) was organized to access the new mission concept ( ).

6 Basic features of SUVIT (Solar UV-Vis.-IR Telescope) Telescope aperture 1m Diff. 525, 390nm 0.215, 0.132, Spectropolarimeter (SP) Imager & Imagingpolarimeter (FG) wavelength 1083, 525 nm (TBD) Slit width 0.1 (12um) FOV 300 (scan) x 200 (slit) IFU width 0.25 (30um) FOV 25 X 2 (8 slicers to 1 slit, TBD) NFI wavelength nm (TBD) sampling FOV (high res.), (wide FOV) BFI wavelength 280 (TBD) - 500nm, sampling 0.04 FOV 160 x x90 (high res.), 270 x270 (wide FOV)

7 EUVST (EUV Spectrograph Telescope) f30cm /pix - FOV; 400 x300 Effective area vs. wavelength Count rate vs. Temp. 10 times higher sensitivity Seamless T coverage

8 HCI (High resolution Coronal Imager) - He II Fe IX Fe XVIII 94 HCI f32cm - ~4m long

9 SOLAR-C High-resolution Observations = 70 km Yohkoh 1991 Corona-imaging Hinode XRT Corona imaging Fine-scale coronal structures inferred from Hinode Fine-scale chromospheric structures observed by Hinode & GBO Fine-scale kg photospheric structures inferred from Hinode SOHO 1995 Corona-imaging Hinode EIS spectroscopy SDO 2010 Corona-imaging TRACE 1999 HiC 2012 Corona-imaging HCI EUVST SOLAR-C SOHO 1995 Chrom.-Corona-spectroscopy IRIS SDO 2010 Photospheric mag. Hinode SOT Chrom/photo imaging SUVIT DKIST W-b imaging N-b imaging spectropolarimery (mag. fields)

10 SOLAR-C FOV to capture Large Scale Eruptions EUVST/JCI (400 ) SUVIT (270 ) DKIST (diff.limit) Hinode BFI Large FOV is essential for capturing global electric current system (energy buildup), mechanism of eruption, triggering reconnection, precipitation of energy into chromosphere,,,,

11 Spatial scale Spatial and temporal scales covered by Solar-C and DKIST 400 The sun as an active star 200 Large scale structures, explosions 100 Flare, eruption Active region, prominence spicule Flux tube Sunspot, super graniulation SUVIT 0.05 Unknown frontier Ubiquitous fine scale dynamics DKIST Time scale

12 NGSPM-SOT (Next-Generation Solar Physics Mission-Science Objectives Team) An advisory team chartered by JAXA, NASA, and ESA to study and report on a multilateral solar physics mission concept. Step-1: Develop and document scientific objectives for the NGSPM. Step-2: Prioritize the science objectives and access the NGSPM concept for the next decade within likely resources provided by the agencies. Input from community call for white paper (final report was submitted to agencies) Members NASA: David McKenzie, Ted Tarbell, John Raymond, Sarah Gibson JAXA: Toshifumi Shimizu, Kiyoshi Ichimoto, Kanya Kusano, Hirohisa Hara ESA; Bellot Rubio, Mats Carlsson, Lyndsay Fletcher, Sami Solanki + Laurent Gizon, Takashi Sekii (advise for helioseismology) 2017/06/02 14

13 NGSPM science objectives evolved from original SC proposal I: Formation mechanism of the hot and dynamic outer solar atmosphere I-1 chromospheric fine scale structures Foot point B topology, shock, twist,, I-2 Nano-flare heating Tiny brightening, non-thermal plasma I-3 Wave heating Wave mode, energy flux, dissipation I-4 Flux emergence Evolution of 3D vector magnetic field I-5 Solar wind acceleration B topology in CH, Alfven wave in corona I-6 Prominence B field structure, mass circulation II: Mechanism of large-scale solar eruptions and algorithm for prediction II-1 Energy storage Photo./chrom. B field maps II-2 Trigger mechanism Emerging flux, interaction with chrom.b II-3 Mechanism of explosion Large scale dynamics, current system II-4 Physics of fast reconnection Current sheet, plasmoid, shock II-5 Formation mechanism of (d) sunspots Flux tube & flow in convection zone, II-6 particle acceleration & energy transp. electron & ion distribution, response of chrom. III: Mechanism of solar cycle and irradiance variation III-1 Flow structures in convection zone Global flows in the sun III-2 Magnetic flux in the sun Flux tube at tachocline, polar field reversal III-3 Role of turbulence/vortex in dynamo Small scale helicity & a effect, local dynamo III-4 Solar irradiance variations Fine structure of UV source, TSI & SSI model

14 Prioritize the science objectives and instruments 3 Major Objectives 17 sub-objectives 57 required measurements 15 Notional strawman instruments Importance and feasibility of required measurements evaluate the necessity of instruments Top priority instruments; The combination of the five instruments will address well over half of the required measurements: 0.3 coronal/tr spectrograph (T-9) coronal imager (T-7) chromospheric imager and magnetograph (T-4) 0.1 photospheric magnetograph (T-1) 0.1 chromospheric spectrograph (T-5) Possible additional instrument: high-energy spectroscopic imager (T-10) 16

15 Mission concepts 1. Large mission design 3 instruments (T-09, T07, and T-01/04/05) on a single platform. Significant contributions from all the agencies required. Significant scientific and operational advantages: launch & operations simultaneously and integrated, instrument design optimized, save the total costs Smaller, less complex, and less expensive than 2015 Solar-C NGSPM recommendation 2. Constellation of small/med-class missions form a constellation of satellites to realize 3 instruments (T-09, T07, and T-01/04/05). To increase the possibility that some of the instruments are launched as early as possible. Scientific synergy limited unless significant overlap in observing time of the missions 2017/06/02 17

16 Strategic Large Missions (300M$ class) for JAXA-led flagship science mission with HIIA /III vehicle (3 in ten years) Hitomi (2016) #1 #2 #3 Hitomi revival(2021) 2 yr shift #1: Marth Moon (2024) #2: LiteBIRD, Solar-Sail, (Solar-C) (2027) #3: SPICA (2028?) Competitively-chosen medium-sized focused missions (<150M$ class) with Epsilon rocket ( 5 in ten years) Note: 1$= 100 yen Hisaki(2013) Arase (2016) [#1: SLIM(2020) ] #2 (2022) #3(2024) #4 (2026) (DESTINY, ΔMDR JASMIN) New call soon Call for proposal by JAXA soon!! Missions of opportunity for foreign agency-led mission (10M$/year) Including competitively-chosen small-sized missions (sounding rockets, balloons) BepiColombo (ESA, 2016) JUICE (ESA, 2022) WFIRST(NASA, 2025) ATHENA(ESA, 2028) Medium-size mission w/ Epsilon for #3 (2 nd ) & # (due ) Strategic Large Missions for #2 slot Apr (TBD) NASA NewFrontiers

17 3 candidates for medium size mission under discussion in Japan and NGSPM EUVST; High-throughput UV-EUV spectroscopy (Reduced size from EUVST of SOLAR-C) Photon-counting X-ray telescope for high-energy imaging spectroscopy (following FOXSI-3 sounding rocket) 50cm class UV-Vis-IR spectro-polarimeter (Advanced SOT of Hinode, possibly incl. CLASP) 2016/09/09 19

18 Synergy of the Solar-C and DKIST/EST DKIST/EST: - ultra high resolution (<0.1 ) at photosphere and chromosphere - coronal polarimetry - various approach to access physical quantities, huge data amount Fundamental MHD processes that generate the elementary structures in solar atmosphere, and govern the cosmic plasma Solar-C: - seamless observation from the photosphere to the corona (needless to say about the synergy between EUV instruments and DKIST) - high precision in a large field of view, uniform data quality in space and in time (SUVIT) Connection between elementary processes and emergence of large scale structures & dynamics