The Ca II-Mv correlation (Wilson-Bappu effect) calibrated by Hipparcos parallaxes

被引：15

作者：

Wallerstein, G ^{[1
]}

Machado-Pelaez, L ^{[1
]}

Gonzalez, G ^{[1
]}

机构：

[1] Univ Washington, Dept Astron, Seattle, WA 98195 USA

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 1999年 / 111卷 / 757期

关键词：

D O I：

10.1086/316332

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have used Hipparcos parallaxes to derive absolute visual magnitudes of G, K, and M stars with Ca II emission line widths previously measured by O. C. Wilson. A linear relationship similar to the one derived originally by Wilson & Bappu and improved by Lutz & Kelker was found from M-v = + 7 to -2. For stars brighter than M-v = -2 a substantial number of stars show Ca II emission lines that are broader than expected from the linear fit. Most of those stars are bright giants and supergiants of type G. In appendices we show some sample Ca II profiles and identify emission lines of Fe II as well as the H epsilon line in some stars.

引用

页码：335 / 341

页数：7

共 23 条

[21] HIGH-RESOLUTION IUE OBSERVATIONS OF THE FLARE STAR AD LEONIS - IMPLICATIONS FOR THE MG-II WILSON-BAPPU EFFECT
AMBRUSTER, CW
PETTERSEN, BR
SUNDLAND, SR
ASTRONOMY & ASTROPHYSICS, 1989, 208 (1-2) : 198 - 200
[22] EMISSION CORES IN H- AND K-LINES .3. WILSON-BAPPU EFFECT
ATHAY, RG
SKUMANICH, A
ASTROPHYSICAL JOURNAL, 1968, 152 (1P1): : 141 - +
[23] THEORETICAL TEMPERATURE MINIMA FOR ARCTURUS (K2-IIIP), A POSSIBLE EXPLANATION OF THE WILSON-BAPPU EFFECT
ULMSCHNEIDER, P
SCHMITZ, F
HAMMER, R
ASTRONOMY & ASTROPHYSICS, 1979, 74 (02) : 229 - 234

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