Session 8. Next Generation Solar Physics
Mission special session (17:35-18:40)• Purpose: Share the latest status among thecommunity
1. The NGSPM-SOT report and Japanesecontributions to the NGSPM T. Shimizu (JAXA)
2. US contributions to the NGSPM
D. McKenzie (NASA)3. Questions and discussions

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Session 8. NGSPM splinter session
Wednesday, 12 September from 17:50 to 18:50
Purpose: Understand the mission plans and consider
coordination among the missions to achieve NGSPM
science goals.
1. Solar-C_EUVST
S. Imada, H. Warren
2. MUSE
T. Tarbell3. FOXSI
H. Hudson
4. PhOENiXS. Ishikawa
5. Discussions for coordination led by D. McKenzie
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The NGSPM-SOT report andJapanese contributions tothe NGSPM concept
Hinode 12
10-13 September 2018
@Granada, Spain

Toshifumi SHIMIZU
ISAS/JAXA, Japanshimizu@solar.isas.jaxa.jp
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Next Generation Solar Physics Mission –Science Objectives Team (NGSPM-SOT)• A study team was formed as a means of improving
international coordination in solar physics, and developing amultilateral solar physics mission concept for the next decade.
• Motivated by the original Solar-C situation happened in 2015.

• This advisory team was chartered by NASA, JAXA, and ESA inJune 2016.
• Developed and documented scientific objectives andpriorities for an NGSPM concept• within the resources and framework by the agencies.
• with community inputs, via white papers• The NGSPM-SOT final report was delivered to the agencies inJuly 2017.
http://hinode.nao.ac.jp/SOLAR-C/SOLAR-C/Documents/NGSPM_report_170731.pdf
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NGSPM-SOT members

NASA appointed Members• David McKenzie, NASA, Marshall Space Flight Center• Ted Tarbell, Lockheed Martin Solar and Astrophysics Laboratory• John Raymond, Smithsonian Astrophysical Observatory• Sarah Gibson, High-Altitude Observatory
ESA appointed Members• Luis Ramon Bellot Rubio - Instituto de Astrofisica de Andalucia, Spain• Mats Carlsson - UiO Institute of Theoretical Astrophysics, Norway• Lyndsay Fletcher - University of Glasgow, UK• Sami Solanki - Max-Planck-Institut für Sonnensystemforschung, Germany
JAXA appointed Members• Kiyoshi Ichimoto, Kyoto University/NAOJ• Kanya Kusano, Nagoya University• Hirohisa Hara, NAOJ
• Toshifumi Shimizu, ISAS/JAXA, team chair

Experts added later for assessing helioseismology related objectives• Laurent Gizon, Max-Planck-Institut für Sonnensystemforschung, Germany• Takashi Sekii, NAOJ
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5Two venues of scientific objectives
Physical mechanisms
on elemental (small) scales
Chromospheric spicules

Global-scale processes
affecting/involving large
fractions of atmosphere

From high latitude
Sunspot
Coronal structures

Away from Sun-Earth line(c) NASA/MSFCà Probing beyond the current resolution
chosen for near-term NGSPM
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à Global, multi-vantage observations
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I. Formation mechanisms of the hot anddynamic outer solar atmosphereI-5. Sources of solar windI-1. Formation of chromosphericfine-scale structures & influenceI-2. Test nanoflare heating
I-3. Test wave heating

I-4. Role of flux emergence in heating
I-6. Formation of prominences

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II. Mechanisms of large-scale solar eruptions
and fundations for prediction
II-1. Measure energy build-up

II-5. Formation of sunspots

II-2. Identify the trigger
mechanismII-4. Processes of fastmagnetic reconnection
II-6. Particle acceleration andflare energy transport
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II-3. Evolution & propagation of CME

8III. Mechanisms driving the solar cycle andirradiance variation
III-1. Flow structures in the convection zone
III-2. Locate & trace global magnetic flux
III-3. Quantify turbulence in the dynamo
III-4. Mechanism of irradiance variations
III-5. Explore the deep internal structure
For these key objectives, transformative progress would be made possible with
“global” observations from sustained, vantage points away from the Earth-Sun line
But implementation schemes likely exceed the resources available for aNGSPM on the timescale of the next decade.
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9Physical mechanisms on elemental scales• In many sub-objectives in objectives I and II, progress
will be substantially benefit from observations withincreased resolution.
• A higher-resolution focus for NGSPM will be richscientifically with game-changing discoveries, as shownby the results of recent high-resolution investigations
as Hi-C rocket, IRIS and Hinode.
• Based on the resources that are likely to be available inthe near term, the SOT recommends the path for theNext Generation mission should be probing elementalscale processes, using highest-ever resolution.

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Notional instrument set for elemental science• A minimum set of instruments with which NGSPM can address
the greatest number of sub-objectives and maximize the science
return of the mission.
Higher priority of instruments
in order from the top0.3” coronal/TR spectrograph (T-9)
seamless plasma diagnostics
through the atmosphere0.2”-0.6” coronal imager (T-7)
0.1” – 0.3” chromospheric imager
and magnetograph (T-4)
0.1” photospheric magnetograph (T-1)
0.1” chromospheric spectrograph (T-5)
Magnetic and velocity fields
at chromosphere2018/5/24

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Mission concepts
1. Large mission design• 3 instruments (T-09, T07, and T-01/04/05) on a single platform.
• Opportunity: JAXA strategic Large mission (戦略的中型)• Significant scientific and operational advantages: launch &operations simultaneously and integrated, instrument design
optimized, save the total costs• Not easy to start the project.

2. Constellation of small/med-class missions• To form a constellation of satellites to realize 3 instruments (T-09,T07, and T-01/04/05).
• Opportunity: JAXA Epsilon (公募型⼩型), NASA SMEX/MIDEX• Increase the possibility that some of the instruments are launched as
early as possible.
• Scientific synergy limited unless significant overlap in observing timeof the missions
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JAXA opportunities 2010
Strategic Large Missions(300M$ class) for JAXA-led
flagship science mission
with HIIA /III vehicle(3 in ten years)

2020

2030

Hitomi (2016)
XRISM - Hitomi revival(2020)#1: MMX - Phobos/Deimos (2024)#2: LiteBIRD, Solar-Sail, (Solar-C) (2027)#3: SPICA (2029)
No 2nd opportunity of proposal for #2: April 2018

Competitively-chosen
medium-sized focusedmissions (<150M$ class)with Epsilon rocket(every 2 year)

Hisaki(2013)

Note: 1$= 100 yen
Missions of opportunity forforeign agency-led missions(10M$/year)
Including competitively-chosen small-sized
missions (sounding rockets, balloons)
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Arase (2016)#1: SLIM(2020)#2: Destiny+(2022)#3(2024)#4 (2026)

NGSPM T-09
(S-C_EUVST)#3 (2nd) for 2024 and #4(1st) for 2026 launch

BepiColombo (ESA, 2018)
JUICE (ESA, 2022)
WFIRST(NASA, 2025)
ATHENA(ESA, 2028)
NASA NewFrontiers2016
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Solar-C_EUVST

EUV High-Throughput Spectroscopic Telescope• Corresponding to 0.3” coronal/TR spectrograph (T-9)• Science objectives: (1) To understand how fundamental
processes lead to the formation of the solar atmosphere and thesolar wind, and (II) to understand how the solar atmospherebecomes unstable and release the energy.
An EUV coronal/TR spectrograph tomeasure how mass and energy aretransferred through the atmosphere• Seamless temperature coverage fromchromosphere to corona and flare plasma(17-128nm)• High spatial resolution (0.4”)• High-throughput, much improved temporalresolution (0.5-10s).
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Solar-C_EUVST

EUV High-Throughput Spectroscopic Telescope• This mission concept proposal was submitted to a JAXA call forcompetitive M-class mission candidates this January.
• One of 6 submitted proposals• down-selected to proceed to the next study phase!
• Final down-selection for slot #3 (FY24 launch) by Dec 2019

• S-JASMINE …. Astrometry, down-selected in 2016
• Solar-C_EUVST• HiZ-GUNDAM … gamma-ray bursts for star formation history in early
universe and electromagnetic wave couterparts of gravitational wave
sources, down-selected with S-C_EUVST• High-throughput, much improved temporal
resolution (0.5-10s).
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Solar-C_EUVST

EUV High-Throughput Spectroscopic Telescope• JAXA: EUVST unit structure and mirror assembly, spacecraft bus, rocketvehicle and managing the overall development program.
• The EUVST instrument will be developed as an international collaboration
among Japan, US, and European countries.
(28cm in diameter)

Length ~ 3.2 m• For details, science talks by Shin Imada & Harry Warren tomorrow.
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Notional instrument set for elemental science
EUVST with good spectroscopic capabilities and MUSE with high temporal
resolution in their high spatial (0.4”) resolution has significant synergy,
according to the NGSPM-SOT report.
Higher priority of instruments
in order from the top0.3” coronal/TR spectrograph (T-9)
seamless plasma diagnostics
through the atmosphere0.2”-0.6” coronal imager (T-7)
0.1” – 0.3” chromospheric imager
and magnetograph (T-4)
0.1” photospheric magnetograph (T-1)
0.1” chromospheric spectrograph (T-5)
Magnetic and velocity fields
at chromosphere2018/5/24

Solar-C_EUVST during the next solar
maximum (2025)
NASA SMEX mission
MUSE in phase A
Spectro-polarimetry:
CLASP (UV), Sunrise-3 balloon(1m),ground-based DKIST (4m) àConsider to re-propose 1m-classtelescope to L-class proposal
opportunity (for a launch in early2030’s)
17Possible additional instruments for NGSPM• Next-highest priority instrument for elementalscale science objectives• Addition of T-10 (high-energy spectroscopic imager)• Non-thermal and superhot emissions in flares andnanoflare heating.

• Two proposed missions• FOXSI in phase A study for NASA SMEX
• PhoENiX (Physics of Energetic and Non-thermal Plasmas
in the X-region) concept proposal … not selected in 2018,
but would propose again for #4 & #5 (2026/2028)

These missions provide non-thermal information
and would complement Solar-C_EUVST, although
lower spatial resolution.
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Summary• Next generation solar physics mission(s) are eagerly
wanted in middle 2020s.
• The NGSPM-SOT report to JAXA, NASA and ESA

http://hinode.nao.ac.jp/SOLAR-C/SOLAR-C/Documents/NGSPM_report_170731.pdf• Science priorities are given to understanding of physicalmechanisms on elemental (small) scales• Recommended three instruments (T-9, T-7, T-4/1/5 inorder) as the highest priority.

• Ongoing efforts at JAXA and NASA are investigating
how near term competitive missions may form aconstellation to address science goals of NGSPM.
• Japan-led Solar-C_EUVST as T-9.

• T-4/1/5• Ground-based large telescopes (DKIST, EST etc)

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