The next-generation space solar observatory:

The SOLAR-C Mission

H. Hara National Astronomical Observatory of Japan

JAXA SOLAR-C WG 2015 Nov 4

APSPM in Seoul National University

SOLAR-C Proposals 2015

•  AssumeJAXA+ESA+Europe+USACollabora4on;Targetlaunchyearin2023

•  1stJAXAStrategicMediumMission:– AO:2014Dec26(AnnouncementofOpportunity)– ProposedbySolar-CWG(2015Feb16)

•  4thESAMedium-classMission:– AO:2014Aug19– ProposedbyEPICconsor4um(2015Jan16)

•  EPIC(EuropeanPar4cipa4onInSolar-C)2

BasicProblemsinHelio-Physics1.Originoflarge-scale

explosion

2.Hea4ngofchromosphereandcorona,

Solarwindaccelera4on

3.Magne4ccycle

PlannedsatellitesolarobservatoryledbyJAXASOLAR-CWG

Firstdetermines3Dmagne4cstructuresfromunprecedentedobserva4onsforelucida4ngbasicproblemsinHelio-Phys.

Keywords:-ChromosphericBmeasurements-0.1”–0.3”spa4alresolu4on-〜1shigh-cadenceobserva4ons-highresolu4onspectroscopy

SOLAR-C

(0.1”=70km)1.  Tounderstandtheplasmadynamicsasasystemthatconnectsthesolarsurfacetothesolarcoronaandinterplanetaryspace

2.  Toinves4gatetheelementaryprocessesthattakeplaceuniversallyincosmicplasmas,thebothofwhichalsocontributetothecomprehensionandthepredic4onofsolarac4vitythatcouldgiveimpactontheearthandthehumansociety.

Solar-C Project View

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BasicProblemsinHelio-Physics

2.Originoflarge-scaleexplosion

1.Hea4ngofchromosphereandcorona,

Solarwindaccelera4on

3.Magne4ccycle

PlannedsatelliteSolarobservatorypreparedbyJAXASOLAR-CW.G.

Firstdetermines3Dmagne4cstructuresfromunprecedentedobserva4onsforelucida4ngbasicproblemsinHelio-Phys.

Keywords:-ChromosphericBmeasurements-0.1”–0.3”spa4alresolu4on-〜1shigh-cadenceobserva4ons-highresolu4onspectroscopy

Science Objectives

(0.1”=70km)

SOLAR-C

1.  Inves4gatetheforma4onmechanismsofthechromosphere,thecorona,andthesolarwind

2.  Understandthephysicaloriginoflargescalesolarerup4onstoextractthealgorithmforpredic4on

3.  Revealthemechanismofsolarspectralirradiancevaria4onoftheclimatechangeoftheearth

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Solar-C Approach�Observations of All from photosphere to corona seamlessly

as a system

•  Resolvetheelementalstructuresofsolaratmospheresandobservetheirchangeswithnecessarycadences,

•  Determinetheproper4esandevolu4onofthe3Dmagne4cfieldB,measuringphotosphericandchromosphericB,andes4ma4ngcoronalBfromtheformerinforma4on,

•  Observeallthetemperatureregimesoftheatmosphereseamlesslyandsimultaneously,and

•  Obtainspectroscopicinforma4onondynamicsofelementaryprocessestakingplaceinsolaratmosphere.

SOLAR-Cwill

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Solar-C Science Cases: �I: Forma4onmechanismsof

chromosphere,corona,andsolarwind

•  Understandforma4onmechanismofspiculesandtheirinfluenceinthecorona.

•  Verifythenanoflarehypothesis.•  Verifythewavehea4ng.•  Understandthemagne4cstructure

atthesourceregionsofsolarwindsandtheiraccelera4onmechanism.

•  Understandtheprominenceforma4onmechanism.

SOLAR-Cwill

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CausallinkageinSolarAtmosphereObservations of All from photosphere to corona seamlessly

HinodeHiCCirtain et al. 2012

Photosphere

Chromopshere

0

L

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Solar-C Science Cases: �II: Mechanismoflarge-scalesolarerup4ons

andalgorithmforpredic4on

•  MeasureenergybuildupprocessesinflaringandCMEregions.

•  Iden4fythetriggermechanismofsolarflaresandCMEs.

•  Clarifythemechanismsofdestabilizinganderup4ngoftheen4resystem.

•  Understandtheprocessesoffastmagne4creconnec4on.

SOLAR-Cwill

Hinode

Emergenceofasmallbipole8

Magnetic ReconnectionStudyofaFundamentalPhysicalProcess

Haraetal.(2011)

Takasaoetal.(2012)

~3”

Shibataetal.(1995)

Yohkoh Hinode & SDO SOLAR-CSpectroscopy

Imaging

wHigh-resolution (0.3”) imaging & spectroscopy in chromosphere-corona

wHigher sensitivity (>×10) than Hinode in spectroscopy

wGrowth of sheet structure by high-cadence (>×5) obs.

wMHD shock structure for heating outflows

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Solar-C Science Cases: �III: Mechanismofsolarspectralirradiancevaria4on

thatcouldinfluencetheclimatechangeoftheearth

SOLAR-Cwill

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•  UnderstandtheUVirradiancein4nymagne4cstructures.

•  Constructamodelcapabletoreproducetotalandspectralsolarirradiancebyincorpora4ngfinescalemagne4cstructures.

Solar-C Science objectives (proposed in 2015)I. Formation mechanism of chromosphere, corona and solar wind

I-1 Spicule FootpointBtopology,shock,twistI-2 Nano-flarehea4ng Tinybrightening,non-thermalplasmaI-3 Wavehea4ng Wavemode,energyflux,dissipa4on

I-4 Solarwindaccelera4on BtopologyinCH,AlfvenwaveincoronaI-5 Prominence Bfieldstructure,masscircula4on

II. Physical origin of large-scale eruptions and algorithm for prediction

II-1 Energystorage Photo./chrom.BfieldmapsII-2 Triggermechanism Emergingflux,interac4onwithchrom.B

II-3 Mechanismofexplosion Largescaledynamics,currentsystem

II-4 Physicsoffastreconnec4on Currentsheet,plasmoid,shock

III. Mechanism of solar spectral irradiance variation

III-1 MechanismofUVemission UVemissionsatfinescaleBstructureIII-2 TSS/SSImodeling TSI/SSI,full-diskBmap

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Requirements �(not all shown)

•  Spatial resolution: Photosphere (Ph.) / Chromosphere (Ch.): 0.1”, Ch. B: 0.3”, Transition Region (TR)/Corona: 0.3”

•  Temporal resolution: 1.0 sec •  FOV: Ph./Ch.: >40”×40” for 0.1” resol., >160”×130” for 0.2” resol. TR/Corona: >240” ×240” •  Photometric sensitivity: Ph./Ch.: < 1%, TR/Corona: < 5% •  Line of sight V: < 0.1 km/s for Ph./Ch., < 1 km/s for TR/Corona •  Mag. Fields B: Photosphere BL< 2 G, BT< 70 G Chromosphere: BL< 10 G

•  Simultaneous observations of photosphere to corona for targets •  Continuity of observations: > 3hr for fine scale, < 2 weeks for AR •  Mission life: > 3 yrs near solar activity maximum

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SOLAR-C Spacecraft

SUVIT:SolarUV-Visible-IRTelescopeEUVST:EUVSpectroscopicHCI:High-resolu4onCoronalImager

EUVST(EUVSpectrograph)

HCI

SUVIT/FG

SUVIT/SP

SUVIT/IUSUVIT/UBIS

SunSensor

Hinode

50cmdia.telescope

SUVIT/TA1.4mdiametertelescope

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SOLAR-C payload

Spectro-polarimeter(SP)

Filtergraph(FG)

EUVST(EUVSpectrograph)+IM(IrradianceMonitor)

HCI(HighResolu4onCoronalImager)

SUVITSolarUV-Visible-IRTelescope

UBISUltravioletBroadbandImager

1.4mdiametertelescope

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Regions to be observed by SOLAR-C

Corona

Chromosphere

Photosphere

fromphotosphere

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EUVST0.3”res.

280”x280”

HCI0.3”res.

410”x410”

SUVIT0.1”res.

184”x184”

SOLAR-C: Field of View (FOV)

SUVITUBIS FG SP

Hi-Res.

WideFOV

184”x184”184”x143”

61”x61”70”x70”

120”x120”

USP

UBI

FeI525CaII854HeI1083

MgII280CaII393CN388CH430Cont.432225,260

FeI525NaI589FeI617HI656CaII854HeI1083

1storderbandλ1:17–22nmλ2:69–85nmλ3:92–109nmλ4:112–128nm

HeII30.4FeIX17.1FeXVIII9.4

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Proposed International Task Share

-  JAXA strategic medium mission -  ESA Cosmic Vision II, M4 -  US Heliophysics Decadal Survey

SUVIT-TA (JAXA, ESA)

EUVST (ESA) + IM (Irradiance Monitor)

SUVIT-FG (NASA)SUVIT-SP　(JAXA, ESA)

HCI (NASA)

SUVIT-UBIS (ESA)

Launcher: JAXA S/C bus: JAXA, ESA

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Coordinated Observations

Credit:ESA/AOES

SolarOrbiter

Credit:NASA/JHUAPL

(Daniel K. Inouye Solar Telescope)

DKIST

SolarDynamicObservatoryoramissionoffull-diskobserva9ons

SOLAR-C18

SOLAR-C Proposals 2015

•  AssumeJAXA+ESA+Europe+USACollabora4on;Targetlaunchyearin2023

•  1stJAXAStrategicMediumMission:– AO:2014Dec26(AnnouncementofOpportunity)– ProposedbySolar-CWG(2015Feb16)

•  4thESAMedium-classMission:– AO:2014Aug19– ProposedbyEPICconsor4um(2015Jan16)

•  EPIC(EuropeanPar4cipa4onInSolar-C)19

Phase of JAXA Science Project

WG

PhaseA-1

PhaseA-2

PhaseB/C/D/E

PrePhaseA

Pre-Project1

Pre-Project2

Project

MDR(MissionDefini4onReview)

Time

AO(AnnouncementofOpportunity)

Reviews

Reviews

Reviews

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MDR Results•  EPIC:notselectedbyESA(2015Jun5).•  SOLAR-CProposaltoJAXA

–  Fivemissions(threeScienceandtwoEngineeringmissions)proposedfortheJAXA1stStrategicMission

–  1stpriorityrecommenda4onamongthreeSciencemissionsunderacondi4on(=visibilityforinterna4onaltaskshare)byScienceAdvisoryCommimee.

–  Noneamongfivewasselected.SamplereturnfromMarssatellitehasselectedasCandidatefor1stStrategicMission.

– didnotpassMDR(2015Sep)because•  thecondi4onofinterna4onaltaskshareisnotsa4sfied.•  somescience/technicalfeasibilityisnotwellverified.

– AssessmentofEvalua4onCommimee(EC):•  Re-studybyWGwithcarefulconsidera4onofmissionsize

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Japanese Space Solar Observations1980 1990 2000 2010 2020 2030

Hinotori (Hard X-rays, γ-rays)

Yohkoh (SXR, HXR, γ-rays）

Hinode （Visible, EUV, soft X-rays）

SOLAR-C

Launch

SOLARMAXSOLARMAXSOLARMAX SOLARMAX SOLARMAX

SoundingRocket(sincelate1960’s)

Spacecrao

S520-5CN S520-22CN LaunchCLASP

Planning

Development

Operation

Yohkoh

Hinode

Planning

Hinotori

SOLAR-C （ UV, Visible, NIR, EUV ）

I II

Toward Updated Proposal•  TargetMissionSize:

–  CostReduc4onwithFocusedScienceàSmallerSUVITwithbandselec4ons,simplerEUVST,low-costcoronalimager– Affordablesize:JAXA+Europe+ESAMoO+NASAMoO:–  Synergywithothermission/facility(SOLO,DKIST,..)

•  Promo4onofinterna4onalcollabora4on:–  SetupScienceandTechnologyDefini4onTeaminNASA–  SeekforESAMoO

•  EffortonmovingfromWGtoPre-Project–  Re-defini4onofSolar-Csciencetargets–  Improvescienceandtechnicalfeasibilitybyfurtherstudies

MissionsofOpportunity

Tightlylinked

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Summary•  SOLAR-C is a mission to understand the causal

linkage between solar magnetic fields and active phenomena on the Sun and in the heliosphere.

•  SOLAR-C equips three major payloads to elucidate fundamental problems in Helio-physics

by high-resolution (0.1”−0.3”) imaging & spectroscopy with temporally stable chromospheric magnetometry.

•  JAXA SOLAR-C WG is updating the SOLAR-C mission proposal with more focused science for a coming opportunity (2nd Strategic Mission) with US and European institutes.

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