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On the Interaction between a Protoplanetary Disk and a Planet in an Eccentric Orbit: Application of Dynamical Friction
Earth and Planetary Astrophysics · Submitted 2 Jun 2011
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We have found that the timescale of the orbital evolution depends largely on the adopted disk model in the case of highly eccentric planets.
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
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The abstract, sentence by sentence
We present a new analytic approach to the disk-planet interaction that is especially useful for planets with eccentricity larger than the disk aspect ratio. We make use of the dynamical friction formula to calculate the force exerted on the planet by the disk, and the force is averaged over the period of the planet. The resulting migration and eccentricity damping timescale agrees very well with the previous works in which the planet eccentricity is moderately larger than the disk aspect ratio. The advantage of this approach is that it is possible to apply this formulation to arbitrary large eccentricity. We have found that the timescale of the orbital evolution depends largely on the adopted disk model in the case of highly eccentric planets. We discuss the possible implication of our results to the theory of planet formation.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a new analytic approach to the disk-planet interaction that is especially useful for planets with eccentricity larger than the disk aspect ratio. | contribution 0.99 | 0.88 | 0.09 | asserted 0.99 |
| s1 | We make use of the dynamical friction formula to calculate the force exerted on the planet by the disk, and the force is averaged over the period of the planet. | method 1.00 | 0.95 | 0.06 | asserted 0.99 |
| s2 | The resulting migration and eccentricity damping timescale agrees very well with the previous works in which the planet eccentricity is moderately larger than the disk aspect ratio. | result 0.99 | 0.76 | 0.20 | asserted 1.00 |
| s3 | The advantage of this approach is that it is possible to apply this formulation to arbitrary large eccentricity. | contribution 0.83 | 0.40 | 0.18 | asserted 0.54 |
| s4 | We have found that the timescale of the orbital evolution depends largely on the adopted disk model in the case of highly eccentric planets. | result 0.99 | 0.96 | 0.34 | asserted 1.00 |
| s5 | We discuss the possible implication of our results to the theory of planet formation. | interpretation 0.99 | 0.36 | 0.06 | hedged possibility 0.59 |
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The paper
Original abstract
We present a new analytic approach to the disk-planet interaction that is especially useful for planets with eccentricity larger than the disk aspect ratio. We make use of the dynamical friction formula to calculate the force exerted on the planet by the disk, and the force is averaged over the period of the planet. The resulting migration and eccentricity damping timescale agrees very well with the previous works in which the planet eccentricity is moderately larger than the disk aspect ratio. The advantage of this approach is that it is possible to apply this formulation to arbitrary large eccentricity. We have found that the timescale of the orbital evolution depends largely on the adopted disk model in the case of highly eccentric planets. We discuss the possible implication of our results to the theory of planet formation.
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References
How the literature uses it
6 arXiv papers cite this in 31 sentences
Papers citing it · 21 sentences without a confident label
Contests it 2 papers
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However, the approximation in Ref. [ref] fails to describe the contribution to DF from the near region, which is the dominant one in the supersonic regime.
The Gravity of Classical Fields: And Its Effect on the Dynamics of Gravitational Systems · Discussion · contest 0.92
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However, the approximation in Ref. [ref] fails at describing the contribution to the drag from the near region, which is the dominant one in supersonic motion.
Dynamical friction in slab geometries and accretion disks · Conclusions and outlook · contest 0.94
Uses its method or tool 1 paper
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If $a_p$, $e$ and $Σ$ vary slowly with time, that is, $da_p/dt ≪a_pω_p$, $de/dt≪eω_p$ and $dΣ/dt ≪Σω_p$, we can compute the temporal variation of $a_p$ and $e$ averaged over one orbit: [equation] To express the equation in terms of the true anomaly $f$, we performed the change of variable $t→f$, as both $_p$ and $_p$, and hence $P$ and $T$, are functions of $f$ [ref] .
Orbital evolution of highly eccentric bodies embedded in a ringed accretion disc · Timescales for $a_p$ and $e$ · 0.80
Compares with it 1 paper
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Our results are qualitatively similar to previous works [ref] , though these studies never use the same disk profile as ours.
Constraining accretion physics with gravitational waves from eccentric extreme-mass-ratio inspirals · Supersonic motion · 1.00
Cites it as background 3 papers
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In this context, Ref. [ref] obtained estimates for the dynamical friction under the assumption of a steady state, and using a two-dimensional approximation for the gaseous medium.
Dynamical friction in slab geometries and accretion disks · Introduction · 0.81
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First described by Chandrasekhar [ref] for a nonrelativistic Newtonian perturber moving through a cloud of noninteracting particles, it was then extended to different media (such as fluids [ref] ), different geometries (e.g., spherical or slab-like [ref] ), and including relativistic corrections [ref] .
Relativistic drag forces on black holes from scalar dark matter clouds of all sizes · Introduction · 0.88
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It is worth pointing out that an estimate for the steady DF acting on a particle moving in a straight line through a very thin disk was made previously by [ref] [ref] using a two-dimensional approximation to describe the disk.
The Gravity of Classical Fields: And Its Effect on the Dynamics of Gravitational Systems · Discussion · 0.80
What it cites · 1 sentence without a confident label
Cites as background 2 papers
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The disk-planet interaction when the planet was in an eccentric orbit was investigated by using non-linear numerical simulations by [ref] and more recently by [ref] using a fully radiative code.
Orbital evolution of eccentric planets in radiative discs · Gravitational Interaction between a Disk and an Eccentric Planet · 0.94
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Recently, [ref] have suggested that a disk surrounding a newly born protostar is gravitationally unstable, and therefore it may be possible to form a planet by gravitational instability [ref] .
Recurrent Planet Formation and Intermittent Protostellar Outflows Induced by Episodic Mass Accretion · Implication to Planet Formation Theory · 0.91
Discussion
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