A planetary system around the millisecond pulsar PSR1257 + 12

Wolszczan, A.; Frail, D. A.

doi:10.1038/355145a0

Cited by 1,389 publications

(959 citation statements)

References 22 publications

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“…These planets, contrary to the planets at sub-au orbital separations from single post-giant stars, are unlikely to have been involved in the CE that created today's close binary, but they must have been impacted by the ejection of the giant's envelope. It has been speculated that they may have formed in the aftermath of the CE binary interaction (Beuermann et al 2011), similarly to how the planets around pulsar PSR1257+12 (Wolszczan & Frail 1992) were formed after the supernova explosion.…”

Section: Introductionmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

127

100

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We present the results of hydrodynamic simulations of the interaction between a 10 Jupiter mass planet and a red or asymptotic giant branch stars, both with a zeroage main sequence mass of 3.5 M ⊙ . Dynamic in-spiral timescales are of the order of few years and a few decades for the red and asymptotic giant branch stars, respectively. The planets will eventually be destroyed at a separation from the core of the giants smaller than the resolution of our simulations, either through evaporation or tidal disruption. As the planets in-spiral, the giant stars' envelopes are somewhat puffed up. Based on relatively long timescales and even considering the fact that further inspiral should take place before the planets are destroyed, we predict that the merger would be difficult to observe, with only a relatively small, slow brightening. Very little mass is unbound in the process. These conclusions may change if the planet's orbit enhances the star's main pulsation modes. Based on the angular momentum transfer, we also suspect that this star-planet interaction may be unable to lead to large scale outflows via the rotation-mediated dynamo effect of Nordhaus and Blackman. Detectable pollution from the destroyed planets would only result for the lightest, lowest metallicity stars. We furthermore find that in both simulations the planets move through the outer stellar envelopes at Mach-3 to Mach-5, reaching Mach-1 towards the end of the simulations. The gravitational drag force decreases and the in-spiral slows down at the sonic transition, as predicted analytically.

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Section: Introductionmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

127

100

View full text Add to dashboard Cite

show abstract

“…In some cases planets may also form in the disk of material ejected during the coalescence and left in orbit around the central pulsar (Podsiadlowski, Pringle, & Rees 1991). Indeed the very first extrasolar planets were discovered in orbit around a millisecond pulsar, PSR B1257+12 (Wolszczan & Frail 1992). A merger of two magnetized WD might lead to the formation of a NS with extremely high magnetic field, and this scenario has been proposed as a source of GRBs (Usov 1992).…”

Section: Double White Dwarfsmentioning

confidence: 99%

“…This is one of the possible formation scenarios for the extraordinary planetary system discovered around the millisecond pulsar PSR B1257+12 (see Wolszczan 1999 for a recent update; Podsiadlowski 1993 for alternative planet formation scenarios). This system contains three confirmed Earth-mass planets in quasi-circular orbits (Wolszczan & Frail 1992;Wolszczan 1994). The planets have masses of 0.015/ sin i 1 M ⊕ , 3.4/ sin i 2 M ⊕ , and 2.8/ sin i 3 M ⊕ , where i 1 , i 2 and i 3 are the inclinations of the orbits with respect to the line of sight, and are at distances of 0.19 AU, 0.36 AU, and 0.47 AU, respectively, from the pulsar.…”

Section: The Final Fate: Collapse To a Neutron Star? Planets?mentioning

confidence: 99%

The Final Fate of Coalescing Compact Binaries: From Black Hole to Planet Formation

Rasio

2001

The Neutron Star—Black Hole Connection

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Abstract. Coalescing compact binaries are thought to be involved in a wide variety of astrophysical phenomena. In particular, they are important sources of gravitational radiation for both ground-based and space-based laser-interferometer detectors, and they may be sources of supernova explosions or gamma-ray bursts. Mergers of two white dwarfs may produce neutron stars with peculiar properties, including perhaps millisecond radio pulsars sometimes accompanied by planets (as observed in PSR 1257+12). According to a widely held belief, the coalescence of two neutron stars should produce a rapidly rotating black hole surrounded by an accretion disk or torus, but this is by no means certain. This review paper focuses on the final hydrodynamic coalescence and merger of double neutron stars and double white dwarfs, and addresses the question of the nature of the final merger products.

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“…Carbon-rich nebula created by the disruptions of carbon-rich stars or white dwarfs is a natural cradle for carbon planets, so planets around pulsars and white dwarfs are candidates of carbon planets. For example, the planets around pulsar PSR1257+12 (Wolszczan et al 1992) may be carbon-rich exoplanets. In the well-known β Pictoris debris disk (Roberge et al 2006), an exoplanet named β Pic b was discovered by Lagrange et al ( 2008), it is most likely a carbon-rich planet also because it is located in a carbon-rich environment.…”

Section: Carbon Modelmentioning

confidence: 99%

The silicate and carbon-rich models of CoRoT-7b, Kepler-9d and Kepler-10b

Gong¹,

Zhou²

2012

Res. Astron. Astrophys.

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Possible bulk compositions of the super-Earth exoplanets, are investigated by applying a commonly used silicate and a non-standard carbon model. Their internal structures are deduced using the suitable equation of state of the materials. The degeneracy problems of their compositions can be partly overcome, based on the fact that all three planets are extremely close to their host stars. By analyzing the numerical results, we conclude: 1) The iron core of CoRoT-7b is not more than 27% of its total mass within 1 σ mass-radius error bars, so an Earth-like composition is less likely, but its carbon rich model can be compatible with an Earth-like core/mantle mass fraction; 2) Kepler-10b is more likely with a Mercury-like composition, its old age implies that its high iron content may be a result of strong solar wind or giant impact; 3) the transiting-only superEarth Kepler-9d is also discussed. Combining its possible composition with the formation theory, we can place some constraints on its mass and bulk composition.

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A planetary system around the millisecond pulsar PSR1257 + 12

Cited by 1,389 publications

References 22 publications

Hydrodynamic simulations of the interaction between giant stars and planets

Hydrodynamic simulations of the interaction between giant stars and planets

The Final Fate of Coalescing Compact Binaries: From Black Hole to Planet Formation

The silicate and carbon-rich models of CoRoT-7b, Kepler-9d and Kepler-10b

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