Transformation of a Star into a Planet in a Millisecond Pulsar Binary

被引：117

作者：

Bailes, M. ^{[1
,2
,3
]}

Bates, S. D. ^{[4
]}

Bhalerao, V. ^{[5
]}

Bhat, N. D. R. ^{[1
,2
]}

Burgay, M. ^{[6
]}

Burke-Spolaor, S. ^{[7
]}

D'Amico, N. ^{[6
,9
]}

Johnston, S. ^{[7
]}

Keith, M. J. ^{[7
]}

Kramer, M. ^{[4
,8
]}

Kulkarni, S. R. ^{[5
]}

Levin, L. ^{[1
,2
,7
]}

Lyne, A. G. ^{[4
]}

Milia, S. ^{[6
,9
]}

Possenti, A. ^{[6
]}

Spitler, L. ^{[1
,2
]}

Stappers, B. ^{[4
]}

van Straten, W. ^{[1
,2
]}

机构：

[1] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[2] Swinburne Univ Technol, ARC Ctr All Sky Astrophys CAASTRO, Hawthorn, Vic 3122, Australia

[3] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[4] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[5] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA

[6] Osservatorio Astron Cagliari, Ist Nazl Astrofis, I-09012 Capoterra, Italy

[7] Commonwealth Sci & Ind Res Org CSIRO Astron & Spa, Australia Telescope Natl Facil, Epping, NSW 1710, Australia

[8] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[9] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy

来源：

SCIENCE | 2011年 / 333卷 / 6050期

基金：

美国国家科学基金会; 澳大利亚研究理事会;

关键词：

NEUTRON-STAR; PSR J2051-0827; RADIO PULSAR; WHITE-DWARF; DISCOVERY; MASS; COMPANION; EVOLUTION; SYSTEM; DONORS;

D O I：

10.1126/science.1208890

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Millisecond pulsars are thought to be neutron stars that have been spun-up by accretion of matter from a binary companion. Although most are in binary systems, some 30% are solitary, and their origin is therefore mysterious. PSR J1719-1438, a 5.7-millisecond pulsar, was detected in a recent survey with the Parkes 64-meter radio telescope. We show that this pulsar is in a binary system with an orbital period of 2.2 hours. The mass of its companion is near that of Jupiter, but its minimum density of 23 grams per cubic centimeter suggests that it may be an ultralow-mass carbon white dwarf. This system may thus have once been an ultracompact low-mass x-ray binary, where the companion narrowly avoided complete destruction.

引用

页码：1717 / 1720

页数：4

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