On the Survival of Short‐Period Terrestrial Planets

Mardling, Rosemary A.; Lin, D. N. C.

doi:10.1086/423794

Cited by 68 publications

(66 citation statements)

References 38 publications

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“…That the existence of Jupiter and Saturn affects the formation of Earth and the rest of the inner solar system, particularly in the vicinity of the asteroid belt, is well established (Wetherill 1992;Lecar & Franklin 1997;Chambers & Cassen 2002;Levison & Agnor 2003;Mardling & Lin 2004). The distribution of extrasolar planetary masses is securely predicted to show a similar bimodality (e.g., Ida & Lin 2004), due to the rapid timescale on which runaway accretion of giant planet envelopes occurs (Pollack et al 1996), so a coupling between the observed properties of the giant and terrestrial planets in the same system is expected.…”

Section: Discussionmentioning

confidence: 99%

“…This schedule probably precedes the final stages of terrestrial planet formation. Chambers & Cassen (2002), Levison & Agnor (2003), and Mardling & Lin (2004) have studied in detail the effect of the giant planet configuration and its evolution on the formation of terrestrial planets. If, conversely, eccentricity is the endpoint of gravitational scattering among several massive planets, then the dynamics involved in the scattering process will usually involve multiple rearrangements of the planets prior to stabilization (usually by ejection) and establishment of a ''final'' configuration.…”

Section: Introductionmentioning

confidence: 99%

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Predictions for the Correlation between Giant and Terrestrial Extrasolar Planets in Dynamically Evolved Systems

Veras

Armitage

2006

ApJ

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The large eccentricities of many giant extrasolar planets may represent the endpoint of gravitational scattering in initially more crowded systems. If so, the early evolution of the giant planets is likely to be more restrictive of terrestrial planet formation than would be inferred from the current, dynamically quiescent configurations. Here we study statistically the extent of the anticorrelation between giant planets and terrestrial planets expected in a scattering model. We use marginally stable systems of three giant planets, with a realistic range of planetary masses, as a simple model for the initial conditions prior to scattering, and we show that after scattering the surviving planets reproduce well the known extrasolar planet eccentricities beyond a > 0:5 AU. By tracking the minimum periastron values of all planets during the evolution, we derive the distribution of orbital radii across which strong perturbations (from crossing orbits) are likely to affect low-mass planet formation. We find that scattering affects inner planet formation at orbital separations less than 50% of the final periastron distance, q fm , of the innermost massive planet in approximately 30% of the realizations and can occasionally influence planet formation at orbital separations less than 20% of q fm . The domain of influence of the scattering massive planets increases as the mass differential between the massive planets decreases. Observational study of the correlation between massive and terrestrial extrasolar planets in the same system has the potential to constrain the origin of planetary eccentricity.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Predictions for the Correlation between Giant and Terrestrial Extrasolar Planets in Dynamically Evolved Systems

Veras

Armitage

2006

ApJ

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“…Of course, there is little evolution if the orbit starts close to circular, but the presence of much larger planets in close proximity suggests that a finite eccentricity would be excited by secular perturbations anyway, resulting in tidal evolution (e.g. Mardling & Lin 2004). Thus, we need to consider the fact that the currently observed configuration could be the result of substantial tidal migration if we wish to infer something about the origin and evolution of this planetary system.…”

Section: Tidal Evolution In the Classical Secular Approximationmentioning

confidence: 99%

On the potentially dramatic history of the super-Earth ρ 55 Cancri e

Hansen

Zink

2015

Monthly Notices of the Royal Astronomical Society

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We demonstrate that tidal evolution of the inner planet ('e') of the system orbiting the star ρ 55 Cancri could have led to passage through two secular resonances with other planets in the system. The consequence of this evolution is excitation of both the planetary eccentricity and inclination relative to the original orbital plane. The large mass ratio between the innermost planet and the others means that these excitations can be of substantial amplitude and can have dramatic consequences for the system organisation. Such evolution can potentially explain the large observed mutual inclination between the innermost and outermost planets in the system, and implies that tidal heating could have substantially modified the structure of planet e, and possibly reduced its mass by Roche lobe overflow. Similar inner secular resonances may be found in many multiple planet systems and suggest that many of the innermost planets in these systems could have suffered similar evolutions.

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“…Tides raised by Neptune on its moons help to constrain the planet's quality factor to 10 3.95 < Q < 10 4.56 (Zhang & Hamilton 2008). For M dwarfs, Q dM is assumed to be of order 10 5 , whereas for rigid bodies like Earth 20 Q 500 (Ray et al 2001;Mardling & Lin 2004, and references therein). For BDs, however, Q is even more uncertain, thus we will handle it as a free parameter in our procedures.…”

Section: Tidal Modelsmentioning

confidence: 99%

Tidal effects on brown dwarfs: application to the eclipsing binary 2MASS J05352184-0546085

Heller¹,

Jackson²,

Barnes

et al. 2010

A&A

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Context. 2MASS J05352184−0546085 (2M0535−05) is the only known eclipsing brown dwarf (BD) binary, and so may serve as a benchmark for models of BD formation and evolution. However, theoretical predictions of the system's properties seem inconsistent with observations: i) the more massive (primary) component is observed to be cooler than the less massive (secondary) one; ii) the secondary is more luminous (by ≈10 24 W) than expected. Previous explanations for the temperature reversal have invoked reduced convective efficiency in the structure of the primary, connected to magnetic activity and to surface spots, but these explanations cannot account for the enhanced luminosity of the secondary. Previous studies also considered the possibility that the secondary is younger than the primary. Aims. We study the impact of tidal heating to the energy budget of both components to determine if it can account for the observed temperature reversal and the high luminosity of the secondary. We also compare various plausible tidal models to determine a range of predicted properties. Methods. We apply two versions of two different, well-known models for tidal interaction, respectively: i) the "constant-phase-lag" model; and ii) the "constant-time-lag" model and incorporate the predicted tidal heating into a model of BD structure. The four models differ in their assumptions about the rotational behavior of the bodies, the system's eccentricity and putative misalignments ψ between the bodies' equatorial planes and the orbital plane of the system. Results. The contribution of heat from tides in 2M0535−05 alone may only be large enough to account for the discrepancies between observation and theory in an unlikely region of the parameter space. The tidal quality factor Q BD of BDs would have to be 10 3.5 and the secondary needs a spin-orbit misalignment of 50 • . However, tidal synchronization time scales for 2M0535−05 restrict the tidal dissipation function to log(Q BD ) 4.5 and rule out intense tidal heating in 2M0535−05. We provide the first constraint on Q for BDs. Conclusions. Tidal heating alone is unlikely to be responsible for the surprising temperature reversal within 2M0535−05. But an evolutionary embedment of tidal effects and a coupled treatment with the structural evolution of the BDs is necessary to corroborate or refute this result. The heating could have slowed down the BDs' shrinking and cooling processes after the birth of the system ≈1 Myr ago, leading to a feedback between tidal inflation and tidal heating. Observations of old BD binaries and measurements of the Rossiter-McLaughlin effect for 2M0535−05 can provide further constraints on Q BD .

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On the Survival of Short‐Period Terrestrial Planets

Cited by 68 publications

References 38 publications

Predictions for the Correlation between Giant and Terrestrial Extrasolar Planets in Dynamically Evolved Systems

Predictions for the Correlation between Giant and Terrestrial Extrasolar Planets in Dynamically Evolved Systems

On the potentially dramatic history of the super-Earth ρ 55 Cancri e

Tidal effects on brown dwarfs: application to the eclipsing binary 2MASS J05352184-0546085

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