Masses and orbital inclinations of planets in the PSR B1257+12 System

Maciej Konacki, Alexander Wolszczan

Research output: Contribution to journalArticle

85 Citations (Scopus)

Abstract

We present measurements of the true masses and orbital inclinations of the two Earth-mass planets in the PSR B1257+12 system, based on the analysis of their mutual gravitational perturbations detectable as microsecond variations of the arrival times of radio pulses from the pulsar. The 6.2 ms pulsar, PSR B1257+12, has been regularly timed with the Arecibo telescope since late 1990. Assuming the standard pulsar mass of 1.4 M, the derived masses of planets B and C are 4.3 ± 0.2 and 3.9 ± 0.2 M , respectively. The corresponding orbital inclinations of 53° ± 4° and 47° ± 3° (or 127° and 133°) imply that the two orbits are almost coplanar. This result, together with the known near 3 : 2 resonance between the orbits of the two planets, strongly supports the hypothesis of a disk origin of the PSR B1257+12 planetary system. The system's long-term stability is guaranteed by the low Earth-like masses of planets B and C.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume591
Issue number2 II
DOIs
StatePublished - Jul 10 2003

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inclination
planets
planet
orbitals
pulsars
orbits
planetary systems
arrival time
arrivals
perturbation
telescopes
radio
pulses

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

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title = "Masses and orbital inclinations of planets in the PSR B1257+12 System",
abstract = "We present measurements of the true masses and orbital inclinations of the two Earth-mass planets in the PSR B1257+12 system, based on the analysis of their mutual gravitational perturbations detectable as microsecond variations of the arrival times of radio pulses from the pulsar. The 6.2 ms pulsar, PSR B1257+12, has been regularly timed with the Arecibo telescope since late 1990. Assuming the standard pulsar mass of 1.4 M⊙, the derived masses of planets B and C are 4.3 ± 0.2 and 3.9 ± 0.2 M ⊕, respectively. The corresponding orbital inclinations of 53° ± 4° and 47° ± 3° (or 127° and 133°) imply that the two orbits are almost coplanar. This result, together with the known near 3 : 2 resonance between the orbits of the two planets, strongly supports the hypothesis of a disk origin of the PSR B1257+12 planetary system. The system's long-term stability is guaranteed by the low Earth-like masses of planets B and C.",
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Masses and orbital inclinations of planets in the PSR B1257+12 System. / Konacki, Maciej; Wolszczan, Alexander.

In: Astrophysical Journal, Vol. 591, No. 2 II, 10.07.2003.

Research output: Contribution to journalArticle

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T1 - Masses and orbital inclinations of planets in the PSR B1257+12 System

AU - Konacki, Maciej

AU - Wolszczan, Alexander

PY - 2003/7/10

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N2 - We present measurements of the true masses and orbital inclinations of the two Earth-mass planets in the PSR B1257+12 system, based on the analysis of their mutual gravitational perturbations detectable as microsecond variations of the arrival times of radio pulses from the pulsar. The 6.2 ms pulsar, PSR B1257+12, has been regularly timed with the Arecibo telescope since late 1990. Assuming the standard pulsar mass of 1.4 M⊙, the derived masses of planets B and C are 4.3 ± 0.2 and 3.9 ± 0.2 M ⊕, respectively. The corresponding orbital inclinations of 53° ± 4° and 47° ± 3° (or 127° and 133°) imply that the two orbits are almost coplanar. This result, together with the known near 3 : 2 resonance between the orbits of the two planets, strongly supports the hypothesis of a disk origin of the PSR B1257+12 planetary system. The system's long-term stability is guaranteed by the low Earth-like masses of planets B and C.

AB - We present measurements of the true masses and orbital inclinations of the two Earth-mass planets in the PSR B1257+12 system, based on the analysis of their mutual gravitational perturbations detectable as microsecond variations of the arrival times of radio pulses from the pulsar. The 6.2 ms pulsar, PSR B1257+12, has been regularly timed with the Arecibo telescope since late 1990. Assuming the standard pulsar mass of 1.4 M⊙, the derived masses of planets B and C are 4.3 ± 0.2 and 3.9 ± 0.2 M ⊕, respectively. The corresponding orbital inclinations of 53° ± 4° and 47° ± 3° (or 127° and 133°) imply that the two orbits are almost coplanar. This result, together with the known near 3 : 2 resonance between the orbits of the two planets, strongly supports the hypothesis of a disk origin of the PSR B1257+12 planetary system. The system's long-term stability is guaranteed by the low Earth-like masses of planets B and C.

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