The Relation Between Absolute Magnitude and Reduced Proper Motion, and the Mean Errors in the Spectroscopic Absolute Magnitudes, for Stars of Spectral Classes G and K.

Citations Over Time

Abstract

A study has been made of the corrections to be applied to the spectroscopic absolute magnitudes (Mi) for the case in which the stars are to be grouped on a neutral or im- partial basis of grouping. The stars studied are of spectral types Go--G7 and G8-K2. They have been grouped both on the basis of M~ itself and on the basis of H = m + 5 log j~, a quantity which is correlated with the absolute magnitude (M). In this study the spectroscopic distinction between giants and dwarfs has not been utilized, and some of the regression effects studied by Russell and Miss Moore are thus partly obliterated. Mean values and dispersions in the absolute magnitude have been derived for the two methods of grouping with the aid of Schlesinger's list of trigonometric paralaxes. The systematic errors are found to be small, and the two methods of grouping give practical- ly the same resuks. The dispersion in M~ has been found in most cases to have been underestimated. The mean error of the individual value of M5 has been found to be between 0.5 and o.6 mags. Formulae are derived for the computation of mean absolute magnitudes from trigono- metric parallaxes, for the derivation of the dispersion in M, and for the determination of mean errors in the individual values of M~. The existence of giants and dwarfs is clearly shown when the grouping is made on the basis of H. There are distinct discontinuities in the functional relationship between M and H, the presence of which is obviously independent of the relative proportions of stars of different apparent magnitudes and proper motions used in the investigation

Related Papers

• → Absolute magnitude calibration for red clump stars(2013)7 cited
• → The Distribution of Absolute Magnitudes among Stars Brighter than the Sixth Apparent Magnitude(1932)4 cited
• → What is Absolute About Absolute Magnitude Estimation?(2014)1 cited
• → The Distribution of Absolute Magnitudes among K Stars Brighter than the Sixth Apparent Magnitude as Determined from Parallactic and Peculiar Velocities(1931)1 cited
• → The Distribution of Absolute Magnitudes among M Stars Brighter than the Sixth Apparent Magnitude as Determined from Parallactic and Peculiar Velocities(1930)