A search for line shape and depth variations in 51 Pegasi and τ Bootis

被引：15

作者：

Brown, TM

Kotak, R

Horner, SD

Kennelly, EJ

Korzennik, S

Nisenson, P

Noyes, RW

机构：

[1] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA

[2] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

来源：

ASTROPHYSICAL JOURNAL | 1998年 / 494卷 / 01期

基金：

美国国家科学基金会;

关键词：

line; profiles; planetary systems; stars; individual; (51; Pegasi; 7; Bootis); oscillations;

D O I：

10.1086/311168

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Spectroscopic observations of 51 Pegasi and tau Bootis show no periodic changes in the shapes of their line profiles; these results for 51 Peg are in significant conflict with those reported by Gray & Hatzes. Our detection limits are small enough to rule out nonradial pulsations as the cause of the variability in tau Boo, but not in 51 Peg. The absence of line shape changes is consistent with these stars' radial velocity variability arising from planetary mass companions.

引用

页码：L85 / L88

页数：4

共 13 条

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