The internal constitution of the stars

Eddington, Arthur Stanley

Bibliographic data

Multivolume work

Persistent identifier:: 1876995513

Title:: Die Kunstdenkmäler der Rheinprovinz

Type of content:: Inventar

Year of publication:: 1891

Place of publication:: Düsseldorf; Hannover

Publisher of the original:: Druck und Verlag von L. Schwann

Identifier (digital):: 1876995513

Language:: German

Additional Notes:: Bände 1-20 erschienen ab 1891

Editor:: Clemen, Paul

Commissioning body:: Provinzialverband der Rheinprovinz

Publisher of the digital copy:: Technische Informationsbibliothek (TIB)

Document type:: Multivolume work

Volume

Persistent identifier:: 196111996X

Title:: Die Kunstdenkmäler des Kreises Euskirchen

Sub title:: mit 14 Tafeln und 120 Abbildungen im Text

Scope:: VII, 265 Seiten, XIV Tafeln

DOI:: 10.14463/KXP:196111996X

Year of publication:: 1900

Place of publication:: Düsseldorf

Publisher of the original:: Druck und Verlag von L. Schwann

Identifier (digital):: 196111996X

Illustration:: Illustrationen, Karten

Signature of the source:: a 4412(4,1-4)

Language:: German

Usage licence:: Public Domain Mark 1.0

Contributor:: Renard, Edmund

Adapter:: Clemen, Paul

Commissioning body:: Provinzialverband der Rheinprovinz

Publisher of the digital copy:: Technische Informationsbibliothek (TIB)

Place of publication of the digital copy:: Hannover

Year of publication of the original:: 2026

Document type:: Volume

Collection:: Architecture; Arts; Homeland and regional geography

Section

Title:: HOVEN.

Document type:: Multivolume work

Structure type:: Section

350 THE OUTSIDE OF A STAR The radiation pressure supports the atoms above the photosphere in the chromosphere; elements not subject to the strong radiation pressure do not rise to this level. Thus the difference of pressure is accounted for. Whilst this explanation also lays stress on the fact that the elements with strong principal lines show the deviation (since it is the absorption by these lines which makes them ascend to the chromosphere), it does not assume complete opacity above the photosphere—which was the objection to Fowler and Milne’s explanation. It is rather doubtful at present what the observed “intensity” of a line should be taken to signify. In the foregoing it has been supposed to be a measure of the blackness. Actually our information depends almost wholly on eye estimates of intensity, which presumably combine blackness and breadth. Now breadth depends on entirely different considerations from blackness. It would seem that photometric measurements of black ness at the centres of the lines are essential for a proper application of the theory, and the present use of eye estimates is a very uncertain make shift. What is the temperature referred to in these investigations? The absorbing material is in front of the photosphere and presumably nearer to the boundary temperature T 0 than to the effective temperature T e . The molecular speeds and the density of the radiation will correspond to a temperature near to T 0 ; but the quality of the radiation corresponds to T e or indeed to a temperature rather higher. The ionising power of the radia tion depends on its intensity for high frequencies, and this will be more nearly represented by T e than by T 0 . Probably T in the foregoing results may be considered to correspond fairly nearly to T e . Molecular Sjpectra. 244. In the reversing layers of cooler stars chemical compounds can exist and the molecules give rise to band spectra. For diatomic molecules such as cyanogen, CN, the structure of the bands has been unravelled, and a satisfactory theory of the distribution of intensity in the bands has been developed. So far as we are aware the only attempt to use the band spectra as a clue to the physical conditions in the reversing layer is contained in a paper by R. T. Birge*. The cyanogen band observed in the solar spectrum near 3883 A is composed of five overlapping series. Each series starts from a missing line labelled m = 0 and runs in both directions; the positive (“P”) branch runs towards the red, the successive lines being denoted by m = + 1, + 2, ... ; the negative (“P”) branch runs towards the violet and is denoted Astrophys. Journ. 55, p. 273.

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