J/A+A/376/1113 Line ratios for helium-like ions (Porquet+, 2001)
Line ratios for helium-like ions: Applications to collision-dominated plasmas.
Porquet D., Mewe R., Dubau J., Raassen A.J.J., Kaastra J.S.
<Astron. Astrophys. 376, 1113 (2001)>
=2001A&A...376.1113P 2001A&A...376.1113P
ADC_Keywords: Atomic physics
Keywords: X-rays: stars - atomic processes - stars: coronae - stars: late-type -
stars: activity - early-type stars: activity
Description:
The tables include data concerning six He-like ions: wavelengths,
transition probabilities, wavelengths at which the radiation
temperatures should be determined.
Line ratios (G and R, see definition in table 1 below) for six He-like
ions from Tables 3 to 69 for various parameters:
density (ne), temperature (Te), dilution factor (W), radiation
temperature (Trad), and spectral resolution.
Atomic data (appendix A) concerning the unresolved satellite lines are
displayed (from Tables A1 to A6).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
gline.dat 43 610 G line intensity ratio (tables 4 to 9)
rline.dat 44 21480 R line intensity ratios for W=0.5, 0.01, 0.01
(tables 10 to 69)
taba1-3.dat 74 47 Atomic data of the dielectronic satellite lines
(1s2l2l'-1s22l'') for Ne IX, Mg XI and Si XIII
(tables A1 to A3)
taba4-6.dat 73 262 Atomic data related to the dielectronic satellite
lines of type 1s2l nl'- 1s2nl'' for n=3 and 4
for Ne IX, Mg XI and Si XIII
(tables A4 to A6)
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Table 1: Wavelengths (in Å) of the three main lines of six He-like ions
------------------------------------------------------------------------
Type Label CV NVI OVII NeIX MgXI SiXIII
0.1nm 0.1nm 0.1nm 0.1nm 0.1nm 0.1nm
------------------------------------------------------------------------
resonance w 40.279 28.792 21.603 13.447 9.1681 6.6471
intercombination x 40.711 29.074 21.796 13.548 9.2267 6.6838
intercombination y 40.714 29.076 21.799 13.551 9.2298 6.6869
forbidden z 41.464 29.531 22.095 13.697 9.3134 6.7394
------------------------------------------------------------------------
Line ratios are defined as: G = (z+(x+y))/w, R = z/(x+y)
------------------------------------------------------------------------
Table 2: Update of the transition probabilities (in s-1)
for the six He-like ions
------------------------------------
Transition probability of
Ion z line y line
------------------------------------
CV 4.857E+01 2.900E+07
NVI 2.538E+02 1.380E+08
OVII 1.046E+03 5.800E+08
NeIX 1.090E+04 5.400E+09
MgXI 7.347E+04 3.448E+10
SiXIII 3.610E+05 1.497E+11
------------------------------------
Table 3: Wavelengths (in Å) at which the radiation temperature should
be determined
------------------------------------------------
Wavelengths
Transition CV NVI OVII NeIX MgXI SiXIII
------------------------------------------------
f->i 2280 1906 1637 1270 1033 864
6->r 3542 2904 2454 1860 1475 1200
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Byte-by-byte Description of file: gline.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Z [6,14] Atomic number of the ion (G1)
4- 10 E7.3 cm-3 Ne Electronic density
12- 15 F4.1 MK Te Electronic temperature
17- 18 I2 kK Trad Radiative temperature
20- 23 F4.2 --- G G ratio for Te & Trad, G=(z+(x+y))/w
25- 43 A19 --- Inst Spectral resolution for the calculations (G2)
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Byte-by-byte Description of file: rline.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Z [6,14] Atomic number of the ion (G1)
4- 7 F4.2 --- W Dilution factor of the radiation field (1)
9- 15 E7.1 cm-3 Ne Electronic density
17- 20 F4.1 MK Te Electronic temperature
22- 25 F4.1 kK Trad Radiative temperature
27- 34 E8.2 --- R R ratio for Te and Trad, R = z/(x+y)
36- 44 A9 --- Inst Spectral resolution used for the calculations (G2)
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Note (1): the dilution factor is given by
W = 0.5 * (1 - sqrt(1 - r*/r))
where r is the distance from the center of the stellar source of
radius r*.
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Byte-by-byte Description of file: taba1-3.dat taba4-6.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Z [10,14] Atomic number (G1)
4- 28 A25 --- Trans Blended satellite line transition
30- 33 A4 --- label Current name of the transition
35- 41 F7.4 0.1nm lambda Wavelength of the transition
43- 49 F7.4 10+12s-1 Ar Radiative probability
51- 57 F7.4 10+12s-1 sumAr Sum of the radiative probability
59- 66 F8.4 10+12s-1 Aa Auto-ionization probability
68- 74 F7.4 10+12s-1 F2(s) Line strength factor
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Global notes:
Note (G1): Ion considered:
Z= 6: C V
Z= 7: N VI
Z= 8: O VII
Z=10: Ne IX
Z=12: Mg XI
Z=14: Si XIII
Note (G2): Spectral resolution:
HETGS: High Energy Transmission Grating Spectrometer on board Chandra
MEG wavelength range 2.5-31Å
HEG wavelength range 1.2-15Å
LETGS: Low Energy Transmission Grating Spectrometer on board Chandra
Wavelength range 2-157Å
RGS: Reflection Grating Spectrometer on board XMM-Newton
Wavelength range 6-35Å
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Acknowledgements: Delphine Porquet
References:
Porquet & Dubau, Paper I 2000A&AS..143..495P 2000A&AS..143..495P
(End) Patricia Bauer [CDS] 18-Sep-2001