OBSERVATIONAL LIMITS ON COMPANIONS TO G29-38

被引：19

作者：

KLEINMAN, SJ

NATHER, RE

WINGET, DE

CLEMENS, JC

BRADLEY, PA

KANAAN, A

PROVENCAL, JL

CLAVER, CF

WATSON, TK

YANAGIDA, K

DIXSON, JS

WOOD, MA

SULLIVAN, DJ

MEISTAS, E

LEIBOWITZ, EM

MOSKALIK, P

ZOLA, S

PAJDOSZ, G

KRZESINSKI, J

SOLHEIM, JE

BRUVOLD, A

ODONOGHUE, D

KATZ, M

VAUCLAIR, G

DOLEZ, N

CHEVRETON, M

BARSTOW, MA

KEPLER, SO

GIOVANNINI, O

HANSEN, CJ

KAWALER, SD

机构：

[1] FLORIDA INST TECHNOL,DEPT PHYS & SPACE SCI,MELBOURNE,FL 32901

[2] VICTORIA UNIV WELLINGTON,DEPT PHYS,WELLINGTON,NEW ZEALAND

[3] INST THEORET PHYS & ASTRON,VILNIUS 2600,LITHUANIA

[4] TEL AVIV UNIV,DEPT PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL

[5] JAGIELLONIAN UNIV,ASTRON OBSERV,PL-30244 KRAKOW,POLAND

[6] CRACOW PEDAGOG UNIV,MT SUHORA OBSERV,PL-30084 KRAKOW,POLAND

[7] UNIV TROMSO,INST MATEMAT REALFAG,N-9000 TROMSO,NORWAY

[8] UNIV CAPE TOWN,DEPT ASTRON,RONDEBOSCH 7700,SOUTH AFRICA

[9] OBSERV MIDI PYRENEES,F-31400 TOULOUSE,FRANCE

[10] OBSERV PARIS,F-92195 MEUDON,FRANCE

[11] UNIV LEICESTER,DEPT PHYS,LEICESTER LE1 7RH,LEICS,ENGLAND

[12] UNIV FED RIO GRANDE SUL,INST FIS,BR-91501970 PORTO ALEGRE,RS,BRAZIL

[13] UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309

[14] CNPQ,LAB NACL ASTROFIS,RIO JANEIRO,BRAZIL

来源：

ASTROPHYSICAL JOURNAL | 1994年 / 436卷 / 02期

关键词：

BINARIES; GENERAL; STARS; INDIVIDUAL; (G29-38); LOW-MASS; BROWN DWARFS; OSCILLATIONS; WHITE DWARFS;

D O I：

10.1086/174965

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Recent interest in the variable (DAV) white dwarf G29-38 has been stirred by a tentative report of a radial velocity variation that may be due to an unseen companion. Earlier evidence for a brown dwarf in the system has come from an observed infrared excess in the star's spectrum. For asteroseismological reasons, we have accumulated more than five seasons of high-speed photometric data on the star. By measuring the phase of an isolated, stable frequency in the power spectrum, we show the measured variation is not due (at least in its entirety) to an orbital companion. Because any orbital radial velocity variation must result in a systematic phase variation, the data we present can be used to place stringent limits on the types of companions the system may contain.

引用

页码：875 / 884

页数：10

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