Download Das Sternsystem: Zweiter Teil by K. G. Malmquist (auth.), F. C. Henroteau, H. Ludendorff, K. PDF

By K. G. Malmquist (auth.), F. C. Henroteau, H. Ludendorff, K. G. Malmquist, F. J. M. Stratton (eds.)

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The same systematic variation with spectral type was found by GYLLENBERG (§ 11, table VIII). The investigation of GYLLENBERG and MALMQUIST gave values consistent with those obtained before (§ 11, table IX) except for the M-stars for which the constant K is reduced to +1,0 km/sec. FREUNDLICH and v. D. PAHLEN3 also find a small value, +1,9 kmfsec and GERASIMOVIC 4 finds a negative, but small value of the K-term for the M-stars. The K-term may be due to different causes: to the use of inaccurate normal wave-lengths in the reduction of the spectrograms, to causes within the stars, to the EINSTEIN effect or to a real motion of the stars.

In the eighth and ninth columns the galactic longitude (L) and latitude (B) of the apex are given. The galactic system of Coordinates is that used by PICKERING and CHARLIER and defined through the following position of the galactic pole: 1X = 190°, ~ = +28°. For the transformation formulas, see CHARLIER1 • The tenth column gives the velocity of the sun in km per sec, and the eleventh the K-term expressed in the same unit. Leaving out of consideration the earlier determinations, the agreement between the results is very satisfactory.

Solar Motion and Spectral Type (GYLLENBERG). Type No. Stars A B 284 291 237 208 486 85 286°,2 ± 2°,9 261 ,s ± 4 ,8 262 ,s ± 6 ,6 279 ,s ± 7 ,4 273 ,3 ± 5 ,2 270 ,0 ± 12 ,4 A F G K M D I +25°,5 ± 2 °,41 14 ,s ± 3 ,4 17 ,3 ± 5 ,7 . 23 ,8 ± 6 ,51 31 ,1 ± 4 ,s 28 ,4 ± 10 ,8 1 5 kmjsec K km/sec 22,1 ± 0,9 19,7 ± 1,4 19,5 ± 2,0 18,8 ± 2,2 19,5 ± 1,6 21,0±3,7 +4,3 +0,1 +0,2 -0,8 +3,6 +5,3 The solutions were performed by the aid of the weighted group method; not only the velocity of the sun but also the coordinates of the apex are obtained.

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