Stellar atmospheres : $b A contribution to the observational study of high temperature in the reversing layers of starsPayne-Gaposchkin, Cecilia
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Stellar atmospheres : $b A contribution to the observational study of high temperature in the reversing layers of stars
Payne-Gaposchkin, Cecilia
Astrophysics; Stars -- Spectra; Stars -- Temperature; Thesis (Ph. D.)
Ionized strontium is represented in stellar spectra by the
and the series. The former contains
the important absolute magnitude lines 4215, 4077, which are first seen
at about , and reach a maximum[330] near . They appear
to have “abnormal” intensities in certain stars,[331] and in the
stars are often the finest and sharpest lines in the spectrum. This
behavior suggests a high-level origin, but “stationary Strontium,”
[Pg 82]
although suggested by Plaskett[332] as likely to occur, has not yet
been observed.
YTTRIUM (39)
Numerous lines of yttrium[333] are found in the solar spectrum. The
lines of the ionized atom are somewhat stronger than the lines of the
neutral atom. The lines of the neutral element which can be identified
in the solar spectrum are contained in the following table.
TABLE XV
Series
Wave-Lenght
Int.
Attribution
Int.
Wave-Lenght
3620.94
20
Y?
00
3621.110
3592.91
10
Y
0
3593.040
3552.69
3
-
-
4128.32
30
00
4128.46
4039.83
5
Y
00
4040.013
4047.65
8
Y
4047.823
4102.38
20
Y
0
4102.541
4167.52
10
00
4167.737
4077.39
20
La, Y
?
4077.498
The multiplets at 4174, etc., and at 4674,
etc., and the multiplets, do not appear in the solar
spectrum. None of the above lines is strong enough to be seen in the
spectra of the stars.
IONIZED YTTRIUM
[Pg 83]
Four of the multiplets attributed to ionized yttrium[334] are
satisfactorily identified in the solar spectrum. The wave-lengths and
identifications are contained in Table XVI, p. 83. The arrangement is
as in Table XI.
TABLE XVI
Series
Wave-Lenght
Int.
Attribution
Int.
Wave-Lenght
*
3710.30
100
Y
3
3710.431
3832.87
20
3833.026
*
3774.33
50
Y
3
3774.473
3878.27
4
1
3878.334
3818.37
10
Y
1
3818.487
*
3788.69
30
2
3788.839
3600.72
50
Y
3
3600.880
3548.99
20
Y?
2
3549.151
3664.59
20
Y
2
3664.760
3611.05
30
Y, Mg?
2
3611.189
3584.51
10
Y
2
3584.660
3628.70
10
Y, Mg?
2
3628.847
3601.91
20
Y
1
3602.060
4309.61
20
1
4309.792
4235.71
6
0
4235.894
4199.283
3
00
4199.434
4398.03
15
In zircon *
1
4398.178
4358.72
8
Y-Zr
0
4358.879
4422.60
10
Fe, Y
3
4422.741
5087.42
10
Y?
1
5087.601
4982.12
3
000
4982.319
5320.77
1
-
-
5205.71
10
Y
0
5205.897
5119.10
3
00
5119.292
5289.81
2
000
5289.988
5200.41
8
V
0
5200.590
* But not Zr.
ZIRCONIUM (40)
The ultimate lines of the zirconium atom[335] are all found in the
solar spectrum, far into the ultra-violet.
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