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11: : 「

885        890        895 910      915

915        920        925        930        935        940        945

垣ギ

940        045        950        955        960        965        970        975 1 5

1 0 5 0 20 15 10 5 0

970 975 980 985 990 - 995 1000 1005 Wavelength (A!

Fig. 3.1-5 VUV spectra from neon discharges.

N卜

¨

NO

¨

∞璧

¨

¨

59‐

¨

¨

西

¨

¨

¨

XN

¨

¨

1005      1010      1015 1020      1025

1050      1055

1065      1070      1075      1080      1035      1090      1095

1125 1130 tJfj"",;tlJln

,utfnu 1150

Fig. 3.1-6 VW spectra from neon discharges.

1155

¨ ¨ ¨

1095      1100      1105      1110      1115      1120      1125

N卜

︺F XN

60‐

4 3 2 1 0 20 15 10 5 0

1155      1160    1165      1170      1175      1180      1185

1185      1190      1195      1200      1205      1210    . 1215

1215      1220      1225      1230      1235      1240      1245

8 6 4 2 0 4 3 2 1

Ol  W              r

1240      1245      1250      1255      1260      1265      1270      1275 4

3 2 1 0

2260    2265 2230    2285    2290    2295

¨ ■0¨

X曽 ×

Wavelength (A)

Fig.3.1-7 VUV spectra from neon discharges.

61‐

1 5 1 0 5 0 100

80 60 4A 2A

E o

tr

() R 3 0 D 2+,

5 z a 8 r s

o

3 r o

+,' 6 0

6 4 E 4 0

30 20 1 0 0 1 4 1 2 1 0 8 6 4 2 0

Wavelength (A)

Fig. 3.2-1 VW spectra from argon discharges.

素 調 虫

355        360        365        370        375        380        385        390

¨

0■¨

●せ¨

¨

τ

375        380        385        390        395        400        405

¨

415        420        425        430        435        440        445        450

¨

ゆぶ

460        465        470        475        480        435        490        495

¨

υ

市鴇.

8 8¨需鶏黎

・ a

編 露 ¨¨ m ヽ

485        490        495        500        505        510        515        520

62‐

¨

¨

¨

¨ ¨

510      515

580 590

610      615

616        620        625        630        635        640        645

Wav el eng t h( A)

Fi g。3. 2. 2  VUV  s pec t r a■ om  ar gon  di s c har ges .

・碗課野確 ︒ん

¨

■ご

¨

τ τ

63‐

¨¨

嘔く

650 655 660 665 670

635        640

685        690        695

710        715        720

Wavelength (A)

Fig.3.2-3 VW spectra from argon discharges.

665        670        675

¨

ヽ﹁

お湯・卜 L続識ユ

690        695        700

ゴ ト ・ ・ 菱 多 税

710        715        720        725        730        735        740        745

¨

¨

萎 7

735        740        745        750        755        760        765        770

64‐

¨

トト

一一

TEORヽoョoo

o 9︶ぉ¨o一o

810        815        320        825        830        835

765        770        775        780        785        790

785        790        795 800        805        810        815        820

840        845

835        840        845        850        855        860

Wa v e : e ng t h( A)

F i g .3 。2 ‐4   V UV  s p e c tta   to m a r g o n  d i s c h a r g e s .

α

¨

¨

860        865        870        875        880        885        800        895

Φ

¨

濃 霧 梁 /

65‐

Ω

8 8 5         蜘         颯         鮒

6 05 ︒4 ︒3 ︒2 0

1 00 1 6

︲ 4

・ 2

・ 086420 ・ 086420 0 05 0

0 0

5 ︒

0 0

5 00  3 0 2 0 1 0 0

91o      915

985      990      995    v↓

: : t l ei l l 『 ( A) 1011      1015      102,

Fi g。3。2‐ 5  VUV  s pec t r a  hm  ar gon  di s c har ges 。 910

935

¨

960

Ъ

α

66¨

¨

150 100 50 0 1 120 100 30 60 20 0

1010      1015      1020      1025      1030

1035      1040      1045 1050      1055      1060      1065      1070

1060 1065        1070 1075        1080 1085        1090

1085      1090      1005      1100      1105      1110      1115      1120

30 25 20 15 10 5 0 120 100 80 60 4 0 20 0

3 2 1 0

1110      1115      1120      1125      1130      1135      1140      1145

Wav e: engt h( A)

F ig . 3 .2 ‐6   V UV  s p e c ta  to m a r g o n   d is c h a r g e S .

ё

¨

¨

轟 望 ガ

寸りXN電C

¨

翼N

67‐

1 6 1 4 1 2 1 0 8 6 4 2 0 2

0

1135 1140   1145      1150      1155      1160      1165      1170

¨

00 80 60 40 20 0 00 80 60 4 0 2 0 0 4 3 2 1 0

1160      1165      1170      1175 1180      1185      1190      1191

1185 1190      1195      1200      1205      1210    ′ 1215      1220

1210 1215      1220      1225      1230      1235      1240      1245

1245      1250      1255      1260      1265      1270      1275

wav e: engt h( A)

F i g 。3 . 2 口7   V UV   s p e c t r a   t o m  a r g o n   d i s c h a r g e s .

¨

涎N

¨

¨

Ж¨

¨

XN

XN

綺N

¨

■ど

68…

6 4 2 0

TEoRヽo讐ョooЪ二ぉ¨oo一E

●りX寸¨ Ъ

1275      1280      1285      1290 1295 1300 1305

1310      1315      1320

1335      1340      1345      1350      1355      1360      1365

1360    1365      1370      1375      1380      1385      1390      1395

1390 1395 1400 1405 141A 7415 1r.z0 1/'25 Wavelength (A)

Fig. 3.2-8 VUV spectra from argon discharges.

¨

Σ¨ ¨

69‐

¨

︵oEO崎Nヽoコ00

o Or︸ゝOLo¨

1430 1440 1445 1 0 1455

1455      1460 1465      1470      1475 1480 1485

1485      1490

1515      1520

1530      1535      1540      1545      1550      1555      1560 1565

Wave: engt h( A)

Fig.3.2-9 VUV spectra from argon discharges.

糞寸¨

詈: ヽ

≧ 8

0  1 ‐

>

0

トト¨

70‐

3.2. Identification of Ml lines of Al, Aro Ti and Fe

3.2.1. Introduction

Forbidden lines arising from magnetic dipole (M1) transitions of highly charged ions are interesting in diagnostic applications of magnetically confined fusion plasmas in addition to spectroscopic studies of the atomic struchre. These Ml lines are generated by electron transitions in ns2np* (*: I to 5) ground and nsnp (n:2,3) excited configurations between the fine structure states of highly charged ions. The wavelength of the Ml line is longer than that of an allowed (El) line in the same ionization stage. Some of the forbidden lines in highly charged ions of medium-Z impurities are emitted in the visible reglon. Spatial intensity profile and the Doppler broadening of such forbidden lines can be easily measured with the visible spectroscopy, which does not require any vacuum system and allows the use of optical fibers.

Several Ml transitions of highly charged ions have been studied in laboratory and astronomy plasmas 1371. The first measurement of the Ml transition in a fusion experimental device was made in the Princeton Large Torus tokamak t38]. Since then, many observations of the Ml lines from I\gh-Z elements larger than Z:21have been done in magretically confined plasmas to measure the wavelengths, impurity densities, ion temperatures and radial intensity profiles rnainly in the visible region 137 461. Although the Ml transitions with elements smaller than ZF28 have been also obserued from astronomy plasmas such as solar corona, nebula and several kinds of stars by using satellites in the visible and VUV region l:47-50l,the data quality from them are not quite enough, e.g., for the accurate determination of wavelength. Recently, the studies on the Ml transitions including argon (Z:18) have been extensively done in the Electron Beam Ion Trap (EBIT) t5l-55]. However, the data are rnainly limited to the visible range, because the intensity of

71‐

Ml lines from the EBIT is very weak and a long exposure time is required to take a good signal to noise ratio.

In the Large Helical Device (LID), to the contrary, argon discharges with high purity have been successfully operated without any instability and the argon emissions have been observed with strong intensities. Many Ml transitions of higNy charged argon ions were fonnd and identified in such argon discharges by analyzrng their Doppler broadening, temporal behavior and spatial intensity distribution [56]. Furthermore, the Ml transitions from metallic elements have been also observed by iqjecting the impurity pellet t571. The study on the Ml transition has bee,lr done not only in the visible region, but also in the VW region using a 3m normal incidence spectrometer, since those lines are very bright. The wavelengths of the argon Ml transitions are accurately determined in the visible and VUV ranges.

h this section, the wavelengths of the Ml transitions carefully determined from aluminurrU argon, titanium and iron spectral lines are presented and compared with previous experimental and theoretical works. Some of lines are newly identified in the present study.

3.2.2. Instrumentation

Vacuum ultraviolet (VW) spectra have been measured by using a space-resolved VW systern, which consists of a 3m normal incidence spectometer with a l200grooves/mm grating, charged-coupled device (CCD) detector (I024xl024pixels, l3pmxl3pm/pixel) and a pat of mirrors for view-angle adjustment [58, 59]. Extreme ultraviolet (EW) spectra have also been measured using a flat-field EUV spectrometer with the CCD detector t60].

Visible spectra have been measured using a 50cm Czerny-Turner type spectrometer (Chromex model 500is) equipped with CCD detector (l024x256pixels, 26ymx26prn/pixel).

Low-resolution l00grooves/mm gratings were selected for monitoring a wider spectral band.

High-resolution visible spectra have bee,n measured using a 1.33m Czerny-Turner tlpe

72‐

spectrometer equipped with an l8OOgrooves/mm grating and CCD detector t6ll. The visible emission was collected by a focusing lens and transmitted by optical fibers with a core diameter of 100pm. The fibers installed on the diagnostic port were a:raRged vertically for meas,rring vertical distributions of the LHD plasma poloidal cross-soction with a spatial resolution of 50 mm. The end of the fibers at the other side was coupled on the entrance slit of the visible spectrometer.

3。2。3.   I dent i r l c at i on  of Ml   t r ans i t i ons

(a) Arx 2s22p$ (F.tlke) (blArx z*zf(oJlksl

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