波長　（ Å ）

温度　(K)

CC

D上

での

光子

数( /sec/ pi xel/ 10

4 4EM

)

CHIANTI DB(Feldman)

SXT Temperature analysis based of Chianti spectrum DB

Masumi ShimojoNSRO/NAO

2002/03/22 太陽・宇宙プラズマゼミ @ 国立天文台・三鷹

1: Introduction Temperature Analysis using SXT Data　（ Filter Ratio Method)

SpectrumDatabase

Model Spectrum

Affective Area of Yohkoh/SXT

Model

ObservationTemperature Temperature

of Coronaof Corona

?

• The emission model – The model of emission line

– The model of Free-Free, Free-bound emission

• The model abundance of Solar Corona• The model of ionization equilibrium

2: X-ray Spectrum Database (1)

Structure of Spectrum Database

• Mewe Spectrum Database (Mewe et al., 1985)

– Standard spectrum database of Yohkoh/SXT– Abundance : Meyer Coronal Abundance (1985)

– Ionization Eq. ： Arnaud & Rothenflug (1985)

• CHIANTI Spectrum Database (Dere, et al., 2001)

– Developed by NRL, Cambridge, Arcetri Obs.

– Standard spectrum database of SOHO/CDS,SUMER

– Abundance ： Select from Meyer, Feldman (1992), Waljeski (19

94) – Ionization Eq. ： Select from Arnaud & Rothenflug,

Arnaud & Raymond (1992), Mazzotta et al. (1998)

2: X-ray Spectrum Database (2)

• The strength of Fe XVII line based on Mewe DB is largare than that based on CHIANTI.

3: Difference between Mew/CHIANTI (1)

１： Emission Model

Wavelength　（ Å）

Temp.　(K)

CC

D上

での

光子

数( /sec/ pi xel/ 10

4 4EM

)

Mewe DB

CC

D上

での

光子

数( /sec/ pi xel/ 10

4 4EM

)Temp.　

(K) Wavelength　（ Å）

CHIANTI DB

Abundance ： Meyer CoronalIonization Eq. ： Arnaud & RothenflugSXT filter : AlMg filter

Fe XVII

MeweCHIANTI (Meyer)

3: Difference between Mew/CHIANTI (2)

２： Abundance Model　　　（ Contribution of Fe line ）

The Contribution of Fe line is >40% @3-8MK

3: Difference between Mew/CHIANTI (3)

２： Abundance Model

Coronal abundance

(Fludra & Schmelz 1999)

H (Meyer)

H (Feldman)

H (Waljeski)FeFeldman ＝ 3.3×Fe Meyer

FeWaljeski ＝ 8.1×Fe Meyer

• Since the abundance of Fe in Feldman model (CHIANTI) is three times larger than that in Meyer model (Mewe), the strength of Fe line base on CHIANTI(Feldman) is larger than that based on Mewe.

3: Difference between Mew/CHIANTI (4) ２： Abundance Model

Wavelength　（ Å）Temp.(K)

Phot on N

u mber on C

CD

( /sec/ pi xel/ 104 4E

M)

Mewe DB(Meyer)

Wavelength　（ Å）Temp.　

(K)

Phot on N

u mber on C

CD

( /sec/ pi xel/ 104 4E

M)

CHIANTI DB(Feldman)

Ionization Eq. ： Arnaud & RothenflugSXT filter : AlMg filter

3: Difference between Mew/CHIANTI (5)

3 ： Ionization Equilibrium

Arnaud & Raymond 1992

Dashed line： Arnaud & RothenflugSolid line： Arnaud & Raymond

Fe XVII

106 107温度　（ K)

Fe XVIIMazzotta et al., 1998

dashed： Arnaud & Raymondsolid：Mazzotta et al.

MeweCHIANTI(Arnaud & Rothenflug)

CHIANTI(Mazzotta et al.)

3: Difference between Mew/CHIANTI (6)

Mewe / Thin AlMewe / Thick AlCHIANTI / Thin Al

CHIANTI / Thick Al

Mewe / Thin AlMewe / Thick AlCHIANTI / Thin Al × 10

CHIANTI / Thick Al × 10

CHIANTI (Feldman + Mazzotta et al.)Mewe

Temperature Analysi sbased on Mewe

4:Which one re-produce the Corona spectrum ?

CHIANTIDatabase

Filter Ratio

Temperature analyasis based on CHIANTI

4 : SXT 温度解析への影響 (1) 1 ： Hara et al., 1992

Temperature Analysis using all X-ray filets of SXT

4:Which one re-produce the Corona spectrum ?

5 :The way to the DEM analysis (1)

Temperature analysisBased onCHIANTI

Molde DEM

Observation

?Real

• Differential Emission Measure (DEM)

– The possibility DEM analysis using Yohkoh/SXT⇒ Strong, et al. 1991

(using Mewe)

5 :The way to the DEM analysis (2)

dTTdTdT

VnddVnEM )(

)( 22

Strong, et al. ,1991, Adv. Space Res. 5, 73

DEM

[Withbroe-Sylwester Method]

• Strong, et al., 1991 used the same methode• We use the SXT temperature responses that are calcula

ted using CHIANTI Database with Feldman abundance model and Mazzotta ionization model. 。

5 :The way to the DEM analysis (3)

1) (Eq. )(

)(

)()( )()1(

ii

ii

ic

i

nn

TW

TWFF

TT

2) (Eq. 1

)()(

)()(

)()(

0

2)(

0

)(

)(

i

ici

ni

ni

nii

FF

dTTTf

dTTTf

TTfW

)0 : (i),filter of response emperature T :

DEMon BasedCount Calculated : filter(i), usingCount : DEM, :

（parameterf

FF

i

ici

Withbroe, 1975

Sylwester, Schrijver and Mewe, 1980

Fludra and Sylwester, 1986

• Test calculation model DEM ⇒ SXT Count ⇒ DEM-Resolver ⇒ Result DEM

5 : Simulation using model DEM

Compare Result DEM with model DEM

Model

ＤＥＭ

Reult

ＤＥＭ

• ＮＯＡＡ６９１９ (Hara, et al. 1992)

5 :Observation result (1)

Al.1 Al12

SXT TEEM: Al.1/Al12 | Temperature MAP

5

12

2)(2 )(

)(k

i i

nici FF

n

The result of Filter ratio Method

SXT-DEM / Mewe

DEM by CDS/SOHOLandi & Landini, 1998

DEM by CDS× １００

DEM by SXT<MEWE>

5 : Observation result (2)

DEM ∝ T-4.95±0.25

SXT-DEM / CHIANTI Ver. 3

DEM by CDS/SOHOLandi & Landini, 1998

DEM by CDS× １００

DEM by SXT<CHIANTI>

5 : Observation result (3)

Al.1

Transient Brightening• NOAA6919 • 18-Nov-91 05:36～　（ sub-C class flare)

Preliminary Results