Relevant bibliographies by topics / Planet-disc interaction

Academic literature on the topic 'Planet-disc interaction'

Author: Grafiati
Published: 9 March 2023
Last updated: 10 March 2023

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Journal articles on the topic "Planet-disc interaction"

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Ragusa, Enrico, Giovanni Rosotti, Jean Teyssandier, Richard Booth, Cathie J. Clarke, and Giuseppe Lodato. "Eccentricity evolution during planet–disc interaction." Monthly Notices of the Royal Astronomical Society 474, no. 4 (December 1, 2017): 4460–76. http://dx.doi.org/10.1093/mnras/stx3094.

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Friebe, Marc F., Tim D. Pearce, and Torsten Löhne. "Gap carving by a migrating planet embedded in a massive debris disc." Monthly Notices of the Royal Astronomical Society 512, no. 3 (March 11, 2022): 4441–54. http://dx.doi.org/10.1093/mnras/stac664.

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ABSTRACT When considering gaps in debris discs, a typical approach is to invoke clearing by an unseen planet within the gap, and derive the planet mass using Wisdom overlap or Hill radius arguments. However, this approach can be invalid if the disc is massive, because clearing would also cause planet migration. This could result in a calculated planet mass that is incompatible with the inferred disc mass, because the predicted planet would in reality be too small to carve the gap without significant migration. We investigate the gap that a single embedded planet would carve in a massive debris disc. We show that a degeneracy is introduced, whereby an observed gap could be carved by two different planets: either a high-mass, barely migrating planet, or a smaller planet that clears debris as it migrates. We find that, depending on disc mass, there is a minimum possible gap width that an embedded planet could carve (because smaller planets, rather than carving a smaller gap, would actually migrate through the disc and clear a wider region). We provide simple formulae for the planet-to-debris disc mass ratio at which planet migration becomes important, the gap width that an embedded planet would carve in a massive debris disc, and the interaction time-scale. We also apply our results to various systems, and in particular show that the disc of HD 107146 can be reasonably well-reproduced with a migrating, embedded planet. Finally, we discuss the importance of planet–debris disc interactions as a tool for constraining debris disc masses.
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Lufkin, G., T. Quinn, J. Wadsley, J. Stadel, and F. Governato. "Simulations of gaseous disc-embedded planet interaction." Monthly Notices of the Royal Astronomical Society 347, no. 2 (January 11, 2004): 421–29. http://dx.doi.org/10.1111/j.1365-2966.2004.07208.x.

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Rein, Hanno. "Planet-disc interaction in highly inclined systems." Monthly Notices of the Royal Astronomical Society 422, no. 4 (April 10, 2012): 3611–16. http://dx.doi.org/10.1111/j.1365-2966.2012.20869.x.

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De Val-Borro, M., R. G. Edgar, P. Artymowicz, P. Ciecielag, P. Cresswell, G. D'Angelo, E. J. Delgado-Donate, et al. "A comparative study of disc-planet interaction." Monthly Notices of the Royal Astronomical Society 370, no. 2 (August 1, 2006): 529–58. http://dx.doi.org/10.1111/j.1365-2966.2006.10488.x.

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Ida, Shigeru, Takayuki Muto, Soko Matsumura, and Ramon Brasser. "A new and simple prescription for planet orbital migration and eccentricity damping by planet–disc interactions based on dynamical friction." Monthly Notices of the Royal Astronomical Society 494, no. 4 (May 4, 2020): 5666–74. http://dx.doi.org/10.1093/mnras/staa1073.

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ABSTRACT During planet formation, gravitational interaction between a planetary embryo and the protoplanetary gas disc causes orbital migration of the planetary embryo, which plays an important role in shaping the final planetary system. While migration sometimes occurs in the supersonic regime, wherein the relative velocity between the planetary embryo and the gas is higher than the sound speed, migration prescriptions proposed thus far describing the planet–disc interaction force and the time-scales of orbital change in the supersonic regime are inconsistent with one another. Here we discuss the details of existing prescriptions in the literature and derive a new simple and intuitive formulation for planet–disc interactions based on dynamical friction, which can be applied in both supersonic and subsonic cases. While the existing prescriptions assume particular disc models, ours include the explicit dependence on the disc parameters; hence, it can be applied to discs with any radial surface density and temperature dependence (except for the local variations with radial scales less than the disc scale height). Our prescription will reduce the uncertainty originating from different literature formulations of planet migration and will be an important tool to study planet accretion processes, especially when studying the formation of close-in low-mass planets that are commonly found in exoplanetary systems.
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Toci, Claudia, Giuseppe Lodato, Valentin Christiaens, Davide Fedele, Christophe Pinte, Daniel J. Price, and Leonardo Testi. "Planet migration, resonant locking, and accretion streams in PDS 70: comparing models and data." Monthly Notices of the Royal Astronomical Society 499, no. 2 (September 25, 2020): 2015–27. http://dx.doi.org/10.1093/mnras/staa2933.

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ABSTRACT The disc surrounding PDS 70, with two directly imaged embedded giant planets, is an ideal laboratory to study planet–disc interaction. We present 3D smoothed particle hydrodynamics simulations of the system. In our simulations, planets, which are free to migrate and accrete mass, end up in a locked resonant configuration that is dynamically stable. We show that features observed at infrared (scattered light) and millimetre (thermal continuum) wavelengths are naturally explained by the accretion stream on to the outer planet, without requiring a circumplanetary disc around Planet c. We post-processed our near-infrared synthetic images in order to account for observational biases known to affect high-contrast images. Our successful reproduction of the observations indicates that planet–disc dynamical interactions alone are sufficient to explain the observations of PDS 70.
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Chen, Jhih-Wei, and Min-Kai Lin. "Dusty disc–planet interaction with dust-free simulations." Monthly Notices of the Royal Astronomical Society 478, no. 2 (May 4, 2018): 2737–52. http://dx.doi.org/10.1093/mnras/sty1166.

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Stoll, Moritz H. R., Giovanni Picogna, and Wilhelm Kley. "Planet-disc interaction in laminar and turbulent discs." Astronomy & Astrophysics 604 (July 27, 2017): A28. http://dx.doi.org/10.1051/0004-6361/201730668.

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Muñoz, D. J., K. Kratter, V. Springel, and L. Hernquist. "Planet–disc interaction on a freely moving mesh." Monthly Notices of the Royal Astronomical Society 445, no. 4 (October 29, 2014): 3475–95. http://dx.doi.org/10.1093/mnras/stu1918.

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Dissertations / Theses on the topic "Planet-disc interaction"

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UBEIRA, GABELLINI MARIA GIULIA. "THE ROLE OF (SUB-)STELLAR COMPANIONS ON THE DYNAMICAL EVOLUTION OF PROTOPLANETARY DISCS." Doctoral thesis, Università degli Studi di Milano, 2020. http://hdl.handle.net/2434/798394.

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The study of planet formation has become progressively more important in the last few years given the great number of diverse exoplanets recently discovered. It is, indeed, only by studying extrasolar planetary systems embedded in their natal (protoplanetary) discs that we can make statistical studies of the range of outcomes of the planet formation process. In particular, the discs that present a cavity (transitional discs) or a gap in the dust radial profile are related to disc clearing mechanisms by young giant planets. In this Thesis, we analyze observations taken with the most advanced telescopes (ALMA and VLT/SPHERE) combining multi-wavelength observations to discriminate between different formation processes in systems with disc sub-structures. We provide a general overview on protoplanetary discs and planets/binaries, followed by the description of dust and gas dynamics and thermal disc structure. Moreover, we describe the two most accredited scenarios of planet formation: core accretion and gravitational instability. In the second part of the Thesis, we present a work on the dust and gas cavity of the disc around CQ Tau observed with ALMA together with thermochemical models and hydro-dynamical simulations, which provide insight on a massive planet responsible for the clearing of such disc structure. Secondly, we describe an analysis done on a survey of 22 Herbig and F/G type stars imaged by SPHERE that confirms that the large near-infrared excess observed in the SEDs of Group I Herbig stars can be explained by the presence of a large gap in their discs. We spatially resolve spirals in HD 100453, HD 100546, CQ Tau; ring-like disc in HD 169142 and HD 141569; and single inclined thin disc in AK Sco and T Cha. We compare the results with ALMA and PDI observations and with simulations. Moreover, we detect and confirm the presence of a novel gravitationally bound companion to the young MWC 297 star. Finally, we describe a novel routine that exploits the known radial variation of stellar artifacts with wavelength together with the spectral slope of the star.
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RAGUSA, ENRICO. "THE EVOLUTION OF BINARY SYSTEMS IN GASEOUS ENVIRONMENTS." Doctoral thesis, Università degli Studi di Milano, 2018. http://hdl.handle.net/2434/604177.

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Systems where a binary, that is two gravitationally bound objects orbiting their centre of mass, interacts with the surrounding gas or dust are extremely common in the Universe and involve a wide variety of different astrophysical objects (star + star, black hole + black hole, star + planet, or planet + moon). Among them, protoplanetary systems and black hole binaries (BHBs) are currently capturing the attention of the scientific community. Despite their very different nature and EM appearance, both protoplanetary and BHB systems are characterized by the presence of a gaseous accretion disc surrounding the binary. As a consequence, the dynamics of these systems is very similar and can be described in one unique theoretical framework: the disc-satellite interaction theory. This project is meant to deepen our knowledge of the theory of circumbinary discs, approaching it in a multidisciplinary way from both the protoplanetary and the BHBs perspective.
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Lin, Min-Kai. "Dynamical instabilities in disc-planet interactions." Thesis, University of Cambridge, 2012. https://www.repository.cam.ac.uk/handle/1810/245135.

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Protoplanetary discs can be dynamically unstable due to structure induced by an embedded giant planet. In this thesis, I discuss the stability of such systems and explore the consequence of instability on planetary migration. I present semi-analytical models to understand the formation of the unstable structure induced by a Saturn mass planet, which leads to vortex formation. I then investigate the effect of such vortices on the migration of a Saturnmass planet using hydrodynamic simulations. I explain the resulting nonmonotonic behaviour in the framework of type III planetary migration. I then examine the role of disc self-gravity on the vortex instabilities. It can be shown that self-gravity has a stabilising effect. Linear numerical calculations confirms this. When applied to disc-planet systems, modes with small azimuthal wavelengths are preferred with increasing disc selfgravity. This is in agreement the observation that more vortices develop in simulations with increasing disc mass. Vortices in more massive discs also resist merging. I show that this is because inclusion of self-gravity sets a minimal vortex separation preventing their coalescence, which would readily occur without self-gravity. I show that in sufficiently massive discs vortex modes are suppressed. Instead, global spiral instabilities develop. They are interpreted as disturbances associated with the planet-induced structure, which interacts with the wider disc leading to instability. I carry out linear calculations to confirm this physical picture. Results from nonlinear hydrodynamic simulations are also in agreement with linear theory. I give examples of the effect of these global modes on planetary migration, which can be outwards, contrasting to standard inwards migration in more typical disc models. I also present the first three-dimensional computer simulations examining planetary gap stability. I confirm that the results discussed above, obtained from two-dimensional disc approximations, persist in three-dimensional discs.
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Bitsch, Bertram [Verfasser], and Wilhelm [Akademischer Betreuer] Kley. "Planet-Disc Interactions in Fully Radiative Discs / Bertram Bitsch ; Betreuer: Wilhelm Kley." Tübingen : Universitätsbibliothek Tübingen, 2012. http://d-nb.info/1162843217/34.

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Hammer, Michael, Kaitlin M. Kratter, and Min-Kai Lin. "Slowly-growing gap-opening planets trigger weaker vortices." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623939.

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The presence of a giant planet in a low-viscosity disc can create a gap edge in the disc's radial density profile sharp enough to excite the Rossby wave instability. This instability may evolve into dust-trapping vortices that might explain the `banana-shaped' features in recently observed asymmetric transition discs with inner cavities. Previous hydrodynamical simulations of planet-induced vortices have neglected the time-scale of hundreds to thousands of orbits to grow a massive planet to Jupiter size. In this work, we study the effect of a giant planet's runaway growth time-scale on the lifetime and characteristics of the resulting vortex. For two different planet masses (1 and 5 Jupiter masses) and two different disc viscosities (alpha= 3 x 10-4 and 3 x 10-5), we compare the vortices induced by planets with several different growth time-scales between 10 and 4000 planet orbits. In general, we find that slowly-growing planets create significantly weaker vortices with lifetimes and surface densities reduced by more than 50 per cent. For the higher disc viscosity, the longest growth time-scales in our study inhibit vortex formation altogether. Additionally, slowly-growing planets produce vortices that are up to twice as elongated, with azimuthal extents well above 180. in some cases. These unique, elongated vortices likely create a distinct signature in the dust observations that differentiates them from the more concentrated vortices that correspond to planets with faster growth time-scales. Lastly, we find that the low viscosities necessary for vortex formation likely prevent planets from growing quickly enough to trigger the instability in self-consistent models.
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Smullen, Rachel A., and Kaitlin M. Kratter. "The Fate of Debris in the Pluto-Charon System." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/624509.

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The Pluto-Charon system has come into sharper focus following the flyby of New Horizons. We use N-body simulations to probe the unique dynamical history of this binary dwarf planet system. We follow the evolution of the debris disc that might have formed during the Charon-forming giant impact. First, we note that in situ formation of the four circumbinary moons is extremely difficult if Charon undergoes eccentric tidal evolution. We track collisions of disc debris with Charon, estimating that hundreds to hundreds of thousands of visible craters might arise from 0.3-5 km radius bodies. New Horizons data suggesting a dearth of these small craters may place constraints on the disc properties. While tidal heating will erase some of the cratering history, both tidal and radiogenic heating may also make it possible to differentiate disc debris craters from Kuiper belt object craters. We also track the debris ejected from the Pluto-Charon system into the Solar system; while most of this debris is ultimately lost from the Solar system, a few tens of 10-30 km radius bodies could survive as a Pluto-Charon collisional family. Most are plutinos in the 3: 2 resonance with Neptune, while a small number populate nearby resonances. We show that migration of the giant planets early in the Solar system's history would not destroy this collisional family. Finally, we suggest that identification of such a family would likely need to be based on composition as they show minimal clustering in relevant orbital parameters.
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