PowerPoint G557.7nmG EUV Na HeDHe+ La FPfoot print OH SAR(sub auroral red) Mg+280 nm


9 (1975) Herzberg II G(557.7nm) (0, v”)
CO2

Krasnoporsky 1980
(1975) O2(c, v’>1)O2*! CO2O2(c, v’>1)
G
2

IRA(0,0)H II (0, ” O2(c, v’>1) siglettriplet
557.7nmG

CO2 G


7
airglow after integration of as long as 21
days. Emissions extending vertically
from -20 to 70 pixel such as at 1216 are geocoronal emissions. The Venusian
airglow is seen at around y = 0. A
narcissistic ghost of the H I Ly-α due to
multiple reflection between the detector
and the grating appears at 783 .
(Nara 2018)
EUV
La
1216
La
1216
He
584
He
584
O+
833
O+
833

La 1216A (y=-20+70) y = 0 783A ( 2018)
8
Figure 5. The net intensity of the Venusian airglow (900-1200). The CO Hopfield-Birge (B 1Σ+ − X 1Σ+) (1,
0) bands, another Hopfield-Birge (C 1Σ+ − X 1Σ+) (0, 1) and (0, 2) bands, the N2 Birge-Hopfield (b 1Πu −
X1Σg +) (1, 3) band, and the Carroll-Yoshino (c4
′ 1Σu + − X 1Σg
+) (0, 0) and (0, 1) bands are also newly identified.
Vertical lines represent peaks of the observed spectrum. We refer to the NIST database for the atomic and ionic
emissions, and to Herzberg (1950) for the molecular emissions for the wavelength used in the labels for each
feature. The differences between the observed and reference (NIST and Herzberg (1950)) wavelengths are
usually less than 2 . (Nara 2018)
N2CO9.8eV11.1eV) CO25eV) S, Cl ( 2018)

CO Hopfield-Birge (B 1Σ+ − X 1Σ+) (1, 0)
CO Hopfield-Birge (C 1Σ+ − X 1Σ+) (0, 1) and (0, 2)
N2 Birge-Hopfield (b 1Πu − X1Σg +) (1, 3)
the Carroll-Yoshino (c4 ′ 1Σu
9
Potter & Morgan 1985
Na 1980 UV D UV
NaUV

20
13

14

16
He+ 30.4 nm 2000 GRL


/
10
19
557.7nmG630nmR O + e* O*
2 O + e* O++ e* + e* 2 O + e* O*+ e* + e* 2
O + hv(+ e* + e*
21

= = =
1km)

DE3
La H2 + e* H* + H + e*
10 5.9RJ 1.8 (56km/s) (400kV) (3MA)

27
NaD589.0-.6A
SNa
28
(46 +/- 5RJ 10”40 +/-5RJ
2-8 RJ SO 2018



UVO O2 + hv(UV) O + O O + O2 + M O3 +M
O3 + H OH*(v’≤ 9) + O2 OH* OH *’+ hv OH* + Q OH*” + Q
OH

630nm2eV)


33
E 80km
Es