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.)
“The inner quantum number () differs from one component of
a multiple term to another, and also in the various series and systems,
according to the following scheme.
Series
Singlets
Doublets
Triplets
Quartets
Quintets
Sextets
Septets
1
s
j = 0
1
1
2
2
3
3
2
p
1
1,2
0,1,2
1,2,3
1,2,3
2,3,4
2,3,4
3
d
2
2,3
1,2,3
1,2,3,4
0,1,2,3,4
1,2,3,4,5
1,2,3,4,5
4
f
3
3,4
2,3,4
2,3,4,5
1,2,3,4,5
1,2,3,4,5,6
0,1,2,3,4,5,6
5
g
4
4,5
3,4,5
3,4,5,6
2,3,4,5,6
2,3,4,5,6,7
1,2,3,4,5,6,7
“Combinations occur only between terms for which differs by 0 or
± 1. If, however, in both cases, no radiation occurs. Lines
corresponding to a change of are found in strong magnetic
fields, and a very few in their absence.
“The combination of two multiple terms gives rise, therefore, to a
group of lines (which may number as many as eighteen). Such groups have
been called multiplets by Catalan. Their discovery has afforded
the key to the many-lined spectra....
“In such a group, those lines for which the changes in and ,
in passing from one term to the other, are of the same sign, are the
strongest, and those in which they are of opposite sign the weakest.
These intensity relations are of great assistance in picking out the
multiplets.
“Combinations between terms of different systems (consistent with
the foregoing rules) often occur. Such lines are usually, though not
always, faint....
“The serial number of the term (which is equivalent to the
total-quantum number) plays quite a subordinate rôle, being of
importance only when series formulae have to be calculated. An
extensive analysis of a spectrum is possible without it, though
determination of the limits of the series, and the ionization
potential, demands its introduction.”
[Pg 205]
III. MATERIAL USED IN CHAPTER VIII
THE line intensities quoted in Chapter VIII were derived from the
spectra of the stars enumerated below in Table XXXII. Successive
columns contain the Draper class, the name of the star, the Boss
number, the visual apparent magnitude, and the reduced proper motion H.
The stars within each class are arranged in order of right ascension.
TABLE XXXII
Class
Star
Boss
m
H
Class
Star
Boss
m
H
Cen
3054
3.3
1.7
Vel
2723
4.1
5.1
Phe
148
4.5
-0.5
Sgr
4832
2.7
0.0
For
474
4.7
0.1
Gru
5880
3.7
4.1
Eri
6ll
4.5
4.3
Eri
696
4.2
5.1
Dor
1081
3.5
2.1
Pic
1446
3.9
3.7
Vel
2356
2.0
1.9
Mus
3092
3.8
3.9
Car
2493
1.8
3.2
Pav
5315
3.6
2.1
Cen
3302
2.4
3.9
PsA
5916
1.3
4.1
TrA
3879
3.1
2.2
Hyi
458
3.0
5.0
Sgr
4645
2.0
2.7
Car
1622
0.9
-4.6
[Pg 206]
Car
2503
2.2
-0.7
Crv
3172
3.2
2.3
Boo
3722
3.0
4.3
Hyi
3622
5.5
4.6
Cir
3739
3.4
5.0
Cen
3623
2.3
6.7
TrA
4030
3.0
6.2
Lup
3864
3.5
4.0
Sco
4457
2.0
-2.6
Lib
3962
5.3
-1.2
Sco
4361
3.4
5.7
Apo
4168
3.9
4.6
Sgr
4874
3.0
1.0
Sco
4272
2.4
6.5
Vol
1917
4.0
0.6
Sgr
4568
3.1
4.6
CMi
2008
0.5
6.1
Sgr
4628
2.8
1.3
Pup
2153
2.9
2.9
Sgr
4665
2.9
4.4
Vel
2324
4.1
0.0
Sgr
4809
3.6
1.4
Oph
4421
4.4
5.4
Sgr
4857
3.4
5.5
Public-domain text, read in full here on John Shaqi.
Reviews
Reviews
No reviews yet
Be the first to share your thoughts on this work.
Elsewhere in the archive
Join the Discussion
Join the discussion
Sign in to leave a comment or review.
Sign InorCreate an account