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

Malhotra, Renu; Black, David C.; Eck, A.; Jackson, A. A.

doi:10.1038/356583a0

Cited by 69 publications

(33 citation statements)

References 7 publications

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“…The planets' masses were initially known only from the Keplerian mass functon--i.e, only the m sin i were known. If we had been viewing the planetary system close to face-on (sin i < 0.1), the masses of the planets would have had to have been so large that their mutual interactions would have been strong enough to make their angles librate, locking them in resonance (Malhotra et al 1992). This would already have been noticed in the pulsar timing (Wolszczan 1993), so sin i > 0.1 and the planets are not locked in the 3:2 resonance.…”

Section: Gravitational Wavesmentioning

confidence: 99%

Binary and Millisecond Pulsars

Phinney¹,

Kulkarni²

1994

Annu. Rev. Astron. Astrophys.

265

237

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Section: Gravitational Wavesmentioning

confidence: 99%

Binary and Millisecond Pulsars

Phinney¹,

Kulkarni²

1994

Annu. Rev. Astron. Astrophys.

265

237

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“…The Grand Tack model, a scenario proposed to explain the current architecture of the inner solar system, asserts that Jupiter and Saturn were once captured into a 3:2 MMR while embedded in the nascent solar nebula (Walsh et al 2011;Pierens et al 2014). Furthermore, the first extrasolar planetary system ever confirmed, around PSR 1257+12 (Wolszczan & Frail 1992;Wolszczan 1994), includes two planets whose orbits are tightly coupled and are very close to residing within the 3:2 MMR (Malhotra et al 1992;Goździewski et al 2005;Callegari et al 2006).…”

Section: Introductionmentioning

confidence: 99%

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

Armstrong

Santerne

Veras

et al. 2015

A&A

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Aims. The K2 mission has recently begun to discover new and diverse planetary systems. In December 2014, Campaign 1 data from the mission was released, providing high-precision photometry for ∼22 000 objects over an 80-day timespan. We searched these data with the aim of detecting more important new objects. Methods. Our search through two separate pipelines led to the independent discovery of K2-19b and c, a two-planet system of Neptune-sized objects (4.2 and 7.2 R ⊕ ), orbiting a K dwarf extremely close to the 3:2 mean motion resonance. The two planets each show transits, sometimes simultaneously owing to their proximity to resonance and the alignment of conjunctions. Results. We obtained further ground-based photometry of the larger planet with the NITES telescope, demonstrating the presence of large transit timing variations (TTVs), and used the observed TTVs to place mass constraints on the transiting objects under the hypothesis that the objects are near but not in resonance. We then statistically validated the planets through the PASTIS tool, independently of the TTV analysis.

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“…It was recognized independently by Malhotra et al (1992) and Razio et al (1992) that if the companion interpretation was correct, then one should be able to observe the consequences of the mutual gravitational perturbation of the companions on each others motion within a few years. The predicted perturbations have apparently been confirmed by A Wolszczan (1994, personal communication).…”

Section: A Funny Thing Happened On the Way To The Forummentioning

confidence: 98%

Completing the Copernican Revolution: The Search for Other Planetary Systems

Black¹

1995

Annual Review of Astronomy and Astrophysics

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The past few decades have witnessed significant advances in our understanding of how stars form, and there has been an associated increase in our knowledge of conditions and phenomena in the early solar system. These have led to the formulation of a paradigm for the origin of the solar system that is sufficiently complete that its basic elements can be tested directly through observations. A simple, but profound, consequence of the paradigm is that most if not all stars should be accompanied by planetary systems. The accuracy of instruments that can be used in such searches has improved to the point that Jupiter-like companions to a number of nearby stars could be detected. However, the results to date are that no other planetary systems have been detected, and the absence of detection is becoming statistically significant, particularly as it relates to the existence of brown dwarf companions to main-sequence stars.

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

Cited by 69 publications

References 7 publications

Binary and Millisecond Pulsars

Binary and Millisecond Pulsars

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

Completing the Copernican Revolution: The Search for Other Planetary Systems

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