A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation

Sigurd̵sson, Steinn; Richer, Harvey B.; Hansen, Brad M. S.; Stairs, I. H.; Thorsett, S. E.

doi:10.1126/science.1086326

Cited by 257 publications

(203 citation statements)

References 29 publications

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“…This planet, which has a minimum mass of ∼ 2.5 times the mass of Jupiter (M ), orbits ∼ 23 AU from the center of mass of PSR 1620-26, a radio pulsar binary comprised of a neutron star and a white dwarf in a ∼ 191 day stellar orbit (Lyne et al 1988, Sigurdsson 1993, Sigurdsson et al 2003. The most plausible model for its formation is accretion within a metal-rich disk produced by post-main sequence Roche lobe overflow (Lissauer 2004).…”

Section: Introductionmentioning

confidence: 99%

Terrestrial planet formation surrounding close binary stars

Quintana¹,

Lissauer²

2006

Icarus

114

107

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Most stars reside in binary/multiple star systems; however, previous models of planet formation have studied growth of bodies orbiting an isolated single star.Disk material has been observed around both components of some young close binary star systems. Additionally, it has been shown that if planets form at the right places within such disks, they can remain dynamically stable for very long times. We also provide formulae that can be used to scale results of planetary accretion simulations to various systems with different total stellar mass, disk sizes, and planetesimal masses and densities.

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Section: Introductionmentioning

confidence: 99%

Terrestrial planet formation surrounding close binary stars

Quintana¹,

Lissauer²

2006

Icarus

114

107

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“…They have masses as high as four Earth masses and are very close to their primary at distances of between 0.2 AU and 0.5 AU. Another planetary system detected orbiting a NS is the binary system of the ms-pulsar PSR B1620-26 and its white dwarf companion (Sigurdsson et al 2003;Sigurdsson & Thorsett 2005). A 2.5-Jupiter-mass object orbits the white dwarf and therefore the NS at 23 AU.…”

Section: Introductionmentioning

confidence: 99%

Searching for substellar companions of young isolated neutron stars

Posselt

Neuhäuser²,

Haberl

2009

A&A

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Context. Only two planetary systems orbiting old ms-pulsars have been discovered. Young radio pulsars and radio-quiet neutron stars cannot be analysed by the usually-applied radio-pulse-timing technique. However, finding substellar companions orbiting these neutron stars would be of significant importance: the companion may have had an exotic formation, its observation may also enable us to study neutron-star physics. Aims. We investigate the closest young neutron stars to Earth to search for orbiting substellar companions. Methods. Young, thus warm substellar companions are visible in the Near infrared, in which the neutron star itself is much fainter. Four young neutron stars are at sufficient speed to enable a common proper-motion search for substellar companions within few years. Results. For Geminga, RX J0720.4-3125, RX J1856.6-3754, and PSR J1932+1059 we found no comoving companion of masses as low as 12, 15, 11, and 42 Jupiter masses, respectively, for assumed ages of 1, 1, 1, and 3.1 Myr, and distances of 250, 361, 167, and 361 pc, respectively. Near infrared limits are presented for these four and five additional neutron stars for which we have observations for only one epoch. Conclusions. We conclude that young, isolated neutron stars rarely have brown-dwarf companions.

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“…This pulsar has a white dwarf companion star. The neutron star mass can be estimated to M * = 1.35 M (Thorsett & Arzoumanian 1999;Sigurdsson et al 2003). The planet is more distant from its star than in the case of PSR 1257+12 but the planetary radius is larger.…”

Section: A Unipolar Inductor In the Pulsar Windmentioning

confidence: 99%

Magnetic coupling of planets and small bodies with a pulsar wind

Mottez

Heyvaerts

2011

A&A

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Aims. We investigate the electromagnetic interaction of a relativistic stellar wind with a planet or a smaller body in orbit around the star. This may be relevant to objects orbiting a pulsar that are expected to hold a planetary system, such as PSR B1257+12 and PSR B1620-26, or to pulsars with suspected asteroids or comets. Methods. We extend the theory of Alfvén wings to relativistic winds. Results. When the wind is relativistic but slower than the total Alfvén speed, a system of electric currents carried by a stationary Alfvénic structure is driven by the planet or by its surroundings. For an Earth-like planet around a "standard" second pulsar, the associated current can reach the same magnitude as the Goldreich-Julian current that powers the pulsar's magnetosphere.

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A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation

Cited by 257 publications

References 29 publications

Terrestrial planet formation surrounding close binary stars

Terrestrial planet formation surrounding close binary stars

Searching for substellar companions of young isolated neutron stars

Magnetic coupling of planets and small bodies with a pulsar wind

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