The Astrophysical journal . od for the Determination of the Exponential Constant of the Emission Function. F. Paschen and H. Wanner 300 viii CONTENTS PAGE On the Visible Spectrum of Nova Sagittarii. W. W. Campbell 308The Variable Velocity of . Pegasi in the Line of Sight. W. 310 The Xariarle Velocity of e Draconis in the Line of Sight. W. \V. Campbell 311 A Comparison of the Visual Hydrogen Spectra of the Orion Nebula AND of A Geissler Tube. - 312 Photographic Extinction. Egon v. Oppolzer - - - 317 The Absolute Determination of the Radiation of Heat with the Electric Co
The Astrophysical journal . od for the Determination of the Exponential Constant of the Emission Function. F. Paschen and H. Wanner 300 viii CONTENTS PAGE On the Visible Spectrum of Nova Sagittarii. W. W. Campbell 308The Variable Velocity of . Pegasi in the Line of Sight. W. 310 The Xariarle Velocity of e Draconis in the Line of Sight. W. \V. Campbell 311 A Comparison of the Visual Hydrogen Spectra of the Orion Nebula AND of A Geissler Tube. - 312 Photographic Extinction. Egon v. Oppolzer - - - 317 The Absolute Determination of the Radiation of Heat with the Electric Compensation Pyrheliometer with Examples of the Application of this Lnstrument. Knut Angstrom 332 On the Pressure in the Spark. Eduard Haschek and Heinrich Mache - - 347 Minor Contributions and Notes : The Yerkes Observatory of the Lniversitv of Chicago, Bulletin No 10 : Period and Elongation Distance of the Fifth Satellite of Jupiter, George E. Hale, 358 ; Bulletin No. i i : Heat Radiation of the Stars, George £. Hale, X o < w THE ASTROPHYSICAL JOURNAL AN INTERNATIONAL REVIEW OF SPECTROSCOPYAND ASTRONOMICAL PHYSICS voLUMEix JANUARY 1899 NUMBER ON THE SPECTRUM OF a AQUILAE AND ITSVELOCITY IN THE LINE OF SIGHT. By H. C. In No. 2924 of AstronomiscJie Nachricliten (July 1889), Pro-fessor Scheiner called attention to the peculiarity of the spectrum(of type I) of a Aquilae — that very faint and somewhat diffusebands can be detected, in addition to the broad hydrogen was later able to show that these bands agree in positionwith groups of lines in spectra of the second type. He suggests*two explanations, along different lines, for the peculiarity of thespectrum. For one, we may imagine that in consequence ofdecided cooling and condensation the constitution of the star hasalready reached considerable similarity with that of the Sun, andin such a manner that a few of the specially prominent metalliclines have not gradually appeared, but that the absorbing atm
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