Abstract

The anomalous spin period second derivative of the binary millisecond pulsar PSR 1620-26 in the globular cluster M4 (Backer 1993; Backer, Sallmen, & Foster 1993; Thorsett, Arzoumanian, & Taylor 1993) is best explained by a sub-Jovian mass planet in a moderately eccentric ∼7 AU orbit about the pulsar binary (Lyne et al. 1987; McKenna & Lyne 1988; Gross, Kulkarni, & Lyne 1988; Phinney 1993a). We consider formation scenarios for PSR 1620-26. A planet scavenged from a single main-sequence star during an exchange encounter naturally produces systems such as PSR 1620-26. The position of the pulsar just outside the core of M4 is shown to fit naturally with the preferred formation scenario and permit a planet to have survived in the inferred orbit about the binary. It is possible that the orbital eccentricity of the binary was induced by the planet. A confirmation of a planet in eccentric orbit about PSR 1620-26 would strongly suggest that planets form unbiquitously around low-mass main-sequence stars, even stars of low metallicity.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume415
Issue number1 PART 2
DOIs
StatePublished - Sep 20 1993

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planets
planet
pulsars
main sequence stars
orbits
eccentric orbits
eccentrics
globular clusters
eccentricity
encounters
metallicity
stars
orbitals

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

@article{af0cece919cd4a928ef727b4b0646e48,
title = "Genesis of a planet in messier 4",
abstract = "The anomalous spin period second derivative of the binary millisecond pulsar PSR 1620-26 in the globular cluster M4 (Backer 1993; Backer, Sallmen, & Foster 1993; Thorsett, Arzoumanian, & Taylor 1993) is best explained by a sub-Jovian mass planet in a moderately eccentric ∼7 AU orbit about the pulsar binary (Lyne et al. 1987; McKenna & Lyne 1988; Gross, Kulkarni, & Lyne 1988; Phinney 1993a). We consider formation scenarios for PSR 1620-26. A planet scavenged from a single main-sequence star during an exchange encounter naturally produces systems such as PSR 1620-26. The position of the pulsar just outside the core of M4 is shown to fit naturally with the preferred formation scenario and permit a planet to have survived in the inferred orbit about the binary. It is possible that the orbital eccentricity of the binary was induced by the planet. A confirmation of a planet in eccentric orbit about PSR 1620-26 would strongly suggest that planets form unbiquitously around low-mass main-sequence stars, even stars of low metallicity.",
author = "Steinn Sigurdsson",
year = "1993",
month = "9",
day = "20",
doi = "10.1086/187028",
language = "English (US)",
volume = "415",
journal = "Astrophysical Journal",
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number = "1 PART 2",

}

Genesis of a planet in messier 4. / Sigurdsson, Steinn.

In: Astrophysical Journal, Vol. 415, No. 1 PART 2, 20.09.1993.

Research output: Contribution to journalArticle

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AU - Sigurdsson, Steinn

PY - 1993/9/20

Y1 - 1993/9/20

N2 - The anomalous spin period second derivative of the binary millisecond pulsar PSR 1620-26 in the globular cluster M4 (Backer 1993; Backer, Sallmen, & Foster 1993; Thorsett, Arzoumanian, & Taylor 1993) is best explained by a sub-Jovian mass planet in a moderately eccentric ∼7 AU orbit about the pulsar binary (Lyne et al. 1987; McKenna & Lyne 1988; Gross, Kulkarni, & Lyne 1988; Phinney 1993a). We consider formation scenarios for PSR 1620-26. A planet scavenged from a single main-sequence star during an exchange encounter naturally produces systems such as PSR 1620-26. The position of the pulsar just outside the core of M4 is shown to fit naturally with the preferred formation scenario and permit a planet to have survived in the inferred orbit about the binary. It is possible that the orbital eccentricity of the binary was induced by the planet. A confirmation of a planet in eccentric orbit about PSR 1620-26 would strongly suggest that planets form unbiquitously around low-mass main-sequence stars, even stars of low metallicity.

AB - The anomalous spin period second derivative of the binary millisecond pulsar PSR 1620-26 in the globular cluster M4 (Backer 1993; Backer, Sallmen, & Foster 1993; Thorsett, Arzoumanian, & Taylor 1993) is best explained by a sub-Jovian mass planet in a moderately eccentric ∼7 AU orbit about the pulsar binary (Lyne et al. 1987; McKenna & Lyne 1988; Gross, Kulkarni, & Lyne 1988; Phinney 1993a). We consider formation scenarios for PSR 1620-26. A planet scavenged from a single main-sequence star during an exchange encounter naturally produces systems such as PSR 1620-26. The position of the pulsar just outside the core of M4 is shown to fit naturally with the preferred formation scenario and permit a planet to have survived in the inferred orbit about the binary. It is possible that the orbital eccentricity of the binary was induced by the planet. A confirmation of a planet in eccentric orbit about PSR 1620-26 would strongly suggest that planets form unbiquitously around low-mass main-sequence stars, even stars of low metallicity.

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