Resonant orbital evolution in the putative planetary system of PSR1257+12

Renu Malhotra, D. Black, A. Eck, A. Jackson

Research output: Contribution to journalArticle

31 Citations (Scopus)

Abstract

PERIODIC variations in the arrival times of pulses from the millisecond pulsar PSR1257+12 are most straightforwardly interpreted as indicating the presence of two planet-like companions orbiting the pulsar1. Rasio et al.2 have proposed that the planetary explanation is amenable to a simple test: the deduced parameters put the planets near an orbital resonance, in which case secular evolution of the orbits should be observable in a matter of years. Detection of such orbital evolution would yield the masses and orbital inclinations of the planets. Here we point out that if the masses of the two planets are more than ∼10 times greater than the minimum values (3.4 and 2.8 Earth masses) allowed by the observations, then their orbits will be in an exact 3:2 resonance. The character of the predicted orbital parameter perturbations is then markedly different from the periodic perturbations that result from only a near-resonance. The amplitude of the perturbations is much greater, and is very sensitive to the planet masses.

Original languageEnglish (US)
Pages (from-to)583-585
Number of pages3
JournalNature
Volume356
Issue number6370
StatePublished - Apr 16 1992
Externally publishedYes

Fingerprint

planetary systems
planets
orbitals
perturbation
orbits
pulsars
inclination
arrivals
pulses

ASJC Scopus subject areas

  • General

Cite this

Malhotra, R., Black, D., Eck, A., & Jackson, A. (1992). Resonant orbital evolution in the putative planetary system of PSR1257+12. Nature, 356(6370), 583-585.

Resonant orbital evolution in the putative planetary system of PSR1257+12. / Malhotra, Renu; Black, D.; Eck, A.; Jackson, A.

In: Nature, Vol. 356, No. 6370, 16.04.1992, p. 583-585.

Research output: Contribution to journalArticle

Malhotra, R, Black, D, Eck, A & Jackson, A 1992, 'Resonant orbital evolution in the putative planetary system of PSR1257+12', Nature, vol. 356, no. 6370, pp. 583-585.
Malhotra R, Black D, Eck A, Jackson A. Resonant orbital evolution in the putative planetary system of PSR1257+12. Nature. 1992 Apr 16;356(6370):583-585.
Malhotra, Renu ; Black, D. ; Eck, A. ; Jackson, A. / Resonant orbital evolution in the putative planetary system of PSR1257+12. In: Nature. 1992 ; Vol. 356, No. 6370. pp. 583-585.
@article{3ac174a25eae459a9f3ea9b43f198030,
title = "Resonant orbital evolution in the putative planetary system of PSR1257+12",
abstract = "PERIODIC variations in the arrival times of pulses from the millisecond pulsar PSR1257+12 are most straightforwardly interpreted as indicating the presence of two planet-like companions orbiting the pulsar1. Rasio et al.2 have proposed that the planetary explanation is amenable to a simple test: the deduced parameters put the planets near an orbital resonance, in which case secular evolution of the orbits should be observable in a matter of years. Detection of such orbital evolution would yield the masses and orbital inclinations of the planets. Here we point out that if the masses of the two planets are more than ∼10 times greater than the minimum values (3.4 and 2.8 Earth masses) allowed by the observations, then their orbits will be in an exact 3:2 resonance. The character of the predicted orbital parameter perturbations is then markedly different from the periodic perturbations that result from only a near-resonance. The amplitude of the perturbations is much greater, and is very sensitive to the planet masses.",
author = "Renu Malhotra and D. Black and A. Eck and A. Jackson",
year = "1992",
month = "4",
day = "16",
language = "English (US)",
volume = "356",
pages = "583--585",
journal = "Nature",
issn = "0028-0836",
publisher = "Nature Publishing Group",
number = "6370",

}

TY - JOUR

T1 - Resonant orbital evolution in the putative planetary system of PSR1257+12

AU - Malhotra, Renu

AU - Black, D.

AU - Eck, A.

AU - Jackson, A.

PY - 1992/4/16

Y1 - 1992/4/16

N2 - PERIODIC variations in the arrival times of pulses from the millisecond pulsar PSR1257+12 are most straightforwardly interpreted as indicating the presence of two planet-like companions orbiting the pulsar1. Rasio et al.2 have proposed that the planetary explanation is amenable to a simple test: the deduced parameters put the planets near an orbital resonance, in which case secular evolution of the orbits should be observable in a matter of years. Detection of such orbital evolution would yield the masses and orbital inclinations of the planets. Here we point out that if the masses of the two planets are more than ∼10 times greater than the minimum values (3.4 and 2.8 Earth masses) allowed by the observations, then their orbits will be in an exact 3:2 resonance. The character of the predicted orbital parameter perturbations is then markedly different from the periodic perturbations that result from only a near-resonance. The amplitude of the perturbations is much greater, and is very sensitive to the planet masses.

AB - PERIODIC variations in the arrival times of pulses from the millisecond pulsar PSR1257+12 are most straightforwardly interpreted as indicating the presence of two planet-like companions orbiting the pulsar1. Rasio et al.2 have proposed that the planetary explanation is amenable to a simple test: the deduced parameters put the planets near an orbital resonance, in which case secular evolution of the orbits should be observable in a matter of years. Detection of such orbital evolution would yield the masses and orbital inclinations of the planets. Here we point out that if the masses of the two planets are more than ∼10 times greater than the minimum values (3.4 and 2.8 Earth masses) allowed by the observations, then their orbits will be in an exact 3:2 resonance. The character of the predicted orbital parameter perturbations is then markedly different from the periodic perturbations that result from only a near-resonance. The amplitude of the perturbations is much greater, and is very sensitive to the planet masses.

UR - http://www.scopus.com/inward/record.url?scp=0000414198&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0000414198&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0000414198

VL - 356

SP - 583

EP - 585

JO - Nature

JF - Nature

SN - 0028-0836

IS - 6370

ER -