A 421-d activity cycle in the BeX recurrent transient A0538-66 from MACHO monitoring

被引：26

作者：

Alcock, C ^{[1
]}

Allsman, RA

Alves, DR

Axelrod, TS

Becker, AC

Bennett, DP

Charles, PA

Cook, KH

Drake, AJ

Freeman, KC

Geha, M

Griest, K

Lehner, MJ

Marshall, SL

McGowan, KE

Minniti, D

Nelson, CA

Peterson, BA

Popowski, P

Pratt, MR

Quinn, PJ

Stubbs, CW

Sutherland, W

Tomaney, AB

Vandehei, T

Welch, DL

机构：

[1] Univ Calif Lawrence Livermore Natl Lab, Livermore, CA 94550 USA

[2] Univ Calif Berkeley, Ctr Particle Astrophys, Berkeley, CA 94720 USA

[3] Australian Natl Univ, Supercomp Facil, Canberra, ACT 0200, Australia

[4] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[5] Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

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

[7] Univ Washington, Dept Phys, Seattle, WA 98195 USA

[8] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA

[9] Univ Oxford, Nucl Phys Lab, Dept Astrophys, Oxford OX1 3RH, England

[10] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 90064 USA

[11] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA

[12] Univ Sheffield, Dept Phys, Sheffield S3 7RH, S Yorkshire, England

[13] Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile

[14] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[15] MIT, Ctr Space Res, Cambridge, MA 02139 USA

[16] European So Observ, D-85748 Garching, Germany

[17] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2001年 / 321卷 / 04期

关键词：

binaries : close; stars : individual : A0538-66; X-rays : stars;

D O I：

10.1046/j.1365-8711.2001.04041.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a similar to5-yr optical light curve of the recurrent Be/X-ray transient A0538-66 obtained as a by-product of the MACHO Project. These data reveal both a long-term modulation at P=420.8 +/-0.8 d and a short-term modulation at 16.6510 +/-0.0022 d which, within errors, confirms the previously found orbital period. Furthermore, the orbital activity is only seen at certain phases of the 421-d cycle, suggesting that the long-term modulation is related to variations in the Be star envelope.

引用

页码：678 / 684

页数：7

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