What Can We Learn About theEjecta from Solar-B/EIS

P. F. Chen1,2, D. H. Brooks1,H. Isobe1, K. Shibata1
１．Kwasan Observatory, Kyoto University, Japan

2. Department of Astronomy, Nanjing University(南京大学), China

From Our Simulations
Chen & Shibata, 2000, ApJ, 545, 524

Chen, Wu, Shibata, & Fang
2002, ApJ, 572, L99

From the PIs
Scientific Objectives
 Flare & CME onset process
 Reconnection evidence
 ……

 Candidate Lines
Ca XVII, Fe X--XV, Fe XXIII, Fe XXIV, Si VII, Si X

VDEM & Forward Modeling VDEM (Velocity differential Emission Measure)

It is directly related to the flaring plasma properties
dsVDEM(v)  ne G(T ,  ) A( s)dv2

 Why Forward Modeling

1. Inversion Modeling is an ill-posed problem, andshould be combined with the Forward Modeling( resolution of SOHO/CDS is not high enough)2. To suggest the most suitable lines for thecorresponding phenomenon
Coronal Reconnection outflow &Moreton waves

Scenario

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejectaObserver

Ca XVIIslitIUnitsI3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe X

Observer

slit
I

Units
I
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe XI
Observerslit
IUnitsI
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe XIIObserver

slit
I

Units
I
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe XIIIObserver

slit
IUnitsI
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe XIV

Observerslit
IUnitsI
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Observer

Fe XV

slit
IUnitsI
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe XXIII

Observerslit
I

UnitsI3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Fe XXIV

Observer

slit
I

Units
I3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Si VIIObserver

slit
IUnitsI3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta
Si X

ObserverslitIUnits
I
3510-11 photons s-1
cmdetector-2 cmflare-2 Å-1

VDEM

1015 photons s-1 (km s-1)-1cmflare-2

Ｓｕｍｍａｒｙ
Across the reconnection point upwardly Ca XVII 192.8 Red shift

blue shift with apossible 2 peaks at the blue wing corresponding tothe slow shock pair

 Fe X 190.04 Besides a static component, one red peakturns to 1-2 blue peaks
 FeXV 284.2 strong line, besides a static component,
121 blue peaks

 Si X 258.4 strong line, besides a static component, 1-2 peaks at the blue wing from the erupting flux ropeand CME expansion

Future Research Contamination from other lines Jets at multiwavelengths
 To construct a G function which weakly depends on T,

a1G1+a2G2+a3G3+a4G4+a5G5+……