Stellar atmospheres : $b A contribution to the observational study of high temperature in the reversing layers of starsPayne-Gaposchkin, Cecilia
Science
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.)
7
none
; ; ;
Possibly an enhanced line accounts
for maximum near ?
8
(?)
;
Mg accounts for maximum at
9
(?)
Unblended
10
(?)
Ti, -5
Probably unblended
11
;
Maximum at due to Fe
12
?
; V,
Blended with Ti. See Note 1
13
?
; ;
Fe predominates. Maximum uncertain
14
;
Rise at due to Fe. In band
15
;
Rowland gives no Ti. Other lines account
for later maximum. In band
16
?
; ;
Maximum undetermined. In band
17
Unblended
18
(?)
; ;
Cr accounts for strength in
V
1
; V,
Ti and Ti+ lines blended. V probably obliterated
2
none
Unblended
3
none
Ti, ;
V probably effective at low temperatures, as these
are the ultimate lines
4
none
N;
Cr
1
Unblended
2
none
Nd? ;
Unblended
3
none
; ; ;
Cr probably predominates
4
none
; Cr ?
Cr predominates
5
none
Unblended
Mn
1
none
Unblended
2
none
;
Fe predominates?
3
none
; ; Zr, -1
4
none
; Mn ?
Mn predominates
5
none
Mn-Fe ?
6
none
Fe-Mn ?
[Pg 129]
7
Fe, ; ;
Mn predominates?
8
Fe-Mn 6
9
; Co, ; ;
V, Ca ?
Fe
1
Mn-Fe
Effectively unblended
2
()
,
No. 2 the weaker line, Mn+ affects
the line at and before , producing maximum at .
See No. 27
3
none
Fe-Mn, 3 ?
Effectively unblended
4
none
Sc, Fe? 3; ; V,
Y+ accounts for maximum at
5
-
Sr+
Due entirely to Sr+
6
?
; ; -3
Maximum at due to Fe+
7
Unblended
8
Unblended
9
()
; ;
Ti+ () causes maximum at
; possibly Cr () causes
rise at
10
()
; ;
Ti predominates?
11
; ; Ti,
Fe probably predominates
12
none
;
Ca produces rise in late classes?
13
Unblended. Rise at unexplained
14
Fe ?
Unblended. Rise at unexplained, unless due
to second Fe line
15
;
Rise at unexplained. See No. 25
16
;
17
; -3
Maximum at due to unknown
line?
18
;
19
;
20
; ;
Fe predominates
21
; ? 3; ; -1,
1, 1
22
; Ti, ;
Rise at due to Ca?
23
;
No. 23 the weaker line
24
; ;
No. 24 the strongest line
25
See No. 15. Rise at unexplained
26
?
;
27
;
The stronger line. Responsible also
for the maximum of line 2
28
; ; ; ;
Rise at due to V
29
none
; ;
Cr and Mn predominate. Cr (ultimate)
line responsible for rise at
[Pg 130]
30
;
Maximum at due to Fe+
31
;
Ca produces rise at
32
; ;
Rise at unexplained
33
Sr+
Due entirely to Sr+
34
-
; Fe? 3; V-Fe?;
35
?
; Fe, -3; ;
; -, 1; Fe-Cr 3
Too heavily blended
36
Co ?; ;
Maximum at unexplained. Rise
at due to Ti (ultimate line)
37
Cr, La, Mn, Ni, ;
Ti, Fe2; Al?; Fe2
See Rowland, p. 37. An Fe+ line
responsible
11
; ;
39
none
; Fe, ; Nd?
Rise at unexplained
40
()
;
Rise at probably due to Ag
41
; ; -3; -3
Maximum certainly due to Fe+.
Neutral Fe causes rise in cool classes
42
; -3; -1; -1N
Maximum due to ionized iron
43
;
Maximum due to Fe+; later rise
perhaps due to Mn
Zn
1
Unblended
2
Unblended
Sr
1
none
;
Fe probably predominates, except
perhaps at the lowest temperatures
2
; Sr ?; Fe ?
Fe probably strong, but Sr responsible
for part of maximum at
3
Fe, ; ; ;
La, Nd? ;
;
Maximum uncertain owing to heavy
blending
Y
1
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