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X-ray observations of SN1006 Koyama, K . Kyoto University. Palmieri et al (1972) Ballon : The first X-ray detection Winkler and Laird : OSO7 The spectrum Photon index =2.3 or kT = 4 keV Becker et al (1980) SSS, OSO8 : Crab Like spectrum : Photon index = 2.2 (no emission line)

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Presentation Transcript
slide1

X-ray observations of SN1006

Koyama, K.Kyoto University

Palmieri et al (1972) Ballon : The first X-ray detection

Winkler and Laird : OSO7 The spectrum Photon index =2.3or kT = 4 keV

Becker et al (1980) SSS, OSO8 : Crab Like spectrum : Photon index=2.2

(no emission line)

Vartanian et al.1985 (GSPC: Balloon) Detection of OVII line =

Thermal Plasma (0.1-0.2 keV)

Koyama et al. 1987 (GSPC: Tenma) : Steeper Power law Photon index- 3.3

NEI Plasma kT 1.9 keV

Spectroscopy

Suzaku

Thermal vs Non-Thermal

Morphology

Chandra: 

Very Thin Filaments

slide2
日本の記録:明月記

藤原定家 (1162-1241) が過去の記録をまとめる。

実際に観測し、

記録したのは

安倍吉昌 (?-1019)

清明の次男・陰陽頭

slide3
中国の記録

宋会要輯稿

五月一日(1006年5月30日)司天監言

先四月二日(5月1日)夜初更,見大星,

色黄,出庫楼東、騎官西,漸漸光明,

測在氐三度。

宋史天文志

景徳三年四月戊寅(5月6日),

周伯星見,出氐南騎官西一度,

状如半月,有芒角,煌煌然可以鉴物,

历庫楼東,八月,随天轮入浊,

十一月,復見在氐。

slide4
各国の記録

明月記(Japan): 寛弘三年四月二日(= 5/1)…如螢惑(=火星)

Ibn al-Jawzi (Baghdad) :  A large star similar to Venus

appeared to the left of qibla.

at the beginning of the month of

Sha’ban (=5/3).

Ali ibn Ridwan(Egypt) : 2and a half to 3 times as large as Venus.

The intensity of its light was a little

more than a quarter of that moonlight.

(5/5?)

宋史天文志(China) : 景徳三年四月戊寅(=5/6)…如半月

-2等級

-4等級

1/4 moon, -8等級

-10等級

参考: 満月= -12.6等級、金星= 最大-4.6等級

slide5

Ia型絶対等級(極大) = -20

距離 = 7100光年 = 2.2kpc

→ 視等級 ~ -9

slide7

SN1006南東部

プラズマ成分の様子を調べる

→ 非熱的X線放射がなく、熱的

放射で明るい南西部からスペク

トルを抽出

O band image

O

Ne

Mg

Si

S

Ar

Ca

Fe

S以上は初めて検出!

Ia型SNRでありながら、これまで

Feなどの重元素の存在はX線で

は未確認だった

黒: XIS-BI

赤: XIS-FI(3台の平均)

slide8

重元素輝線の中心エネルギー

重い元素ほど低い電離状態!

Fe輝線のまわりを電離非平衡

(NEI)プラズマモデルで fitting

kTe = 5.84 (2.77-39) [keV]

net = 5.6 (2.4-8.8) x 109 [cm-3 s]

・ 高温成分の存在

・ 極めて低電離(Ne状程度)

RCW86に類似

黒: BI

赤: FI

slide9

低エネルギー側のスペクトルの謎

酸素輝線のエネルギー

He状 Kα ~ 570eV

He状 Kβ ~ 670eV

H状 Lyα ~ 650eV

730eV

920eV

575eV

672eV

He-Kβdominant!!

820eV

電離度大

高温

730eV lineを入れて酸素

輝線の周辺だけで fitting

極めて低電離な状態なら

このスペクトルを説明可能

kTe = 1.5 [keV]

nte = 4x109 [cm-3s]

best fit

thermal x ray from snrs

Oxygen ionization fraction vs. electron temp.

He-like H-like Fully ionized

1 10 100 103 104

Electron temperature (eV)

Oxygen ionization fraction vs. net (for kTe=1.5keV)

He-like H-like Fully ionized

106 107 108 109 1010 1011 1012

net (cm-3 s)

Thermal X-ray from SNRs

Ionization

Neutral

He-like ion H-like ion

Non-equilibrium ionization (NEI)

Low density, Yong Age

Te ≠ Tz

Ionization equilibrium

requires ~103 years !

Neutral

slide11

C VI

N VI

Fe L

3s2p 3d2p

730 eV 820eV

O VII

1

O VIII

Suzaku/XIS1

XMM-Newton

MOS1

Intensity (arb.)

0.1

Ne IX

O VIII

O VII

ASCA/SIS

0.6

0.4

0.8

Energy (keV)

slide12

730eV

4:1

820eV

730eV

920eV

575eV

672eV

820eV

3:2

730eV

OVII, Kα, Kβ, Kγ, Kδ

820eV

Fe-l Line の謎: 3s2p (730), 3d2p (820)

slide13

SN1006

なぜか Si, S

のラインが太い

Cas A(SN1006

よりあとの観測)

では見られない

Instrumental

ではない。

Si S

Cas A

slide14

SN1006

2-componets

nt ~ 109

~ 1011

Mg Si S

slide15

Chandra

image

SWrim

Chandra

image

Erim

Nrim

Erim

Nrim

SWrim

宇宙線加速効率とプラズマ密

度間の相関を観測的に証明

slide16

Chandra: Thin Filaments (Bamba et al.)

In this region,

electron returns

back (small: quick,

large: slow)

The Efficiency of

Particle

Acceleration

NR: High ER: Low?

A ping-pong

ball gets

speed (energy)

by a rallyin a

moving wall

shock

slide17

SWrim

密度大

Erim

Nrim

hard soft