{"paper":{"title":"$\\alpha\\beta q_\\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs","license":"http://creativecommons.org/licenses/by/4.0/","headline":"Nonlinear shocks usually dominate damping of planet-launched density waves, but cooling on orbital timescales rivals them for sub-thermal planets while viscosity needs high values to matter.","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Amelia J. Cordwell, Roman R. Rafikov","submitted_at":"2026-05-12T18:00:53Z","abstract_excerpt":"Planets embedded in protoplanetary discs are capable of creating a wide variety of substructures through gravitational interactions. This process is mediated through the excitation and damping of density waves which carry angular momentum across the disc. Therefore, to interpret observations of substructures, it is critical to understand the physical processes which lead to deposition of wave angular momentum to the disc fluid. In this study, we explore the relative efficiency of viscosity ($\\alpha$), cooling ($\\beta$), and non-linear wave evolution ($q_\\mathrm{th}$) in damping planet-generate"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"nonlinear wave evolution leading to shock formation is typically the most important cause of angular momentum deposition, but that cooling on timescales comparable to local orbital time reaches similar levels of importance for low mass planets (sub-thermal, q_th<1). On the contrary, linear wave damping due to viscosity is rather inefficient, requiring α ≳ 10^{-1.5} to noticeably affect damping of waves launched by thermal mass planets.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The hydrodynamic simulations capture all relevant damping physics without missing contributions from magnetic fields, realistic radiative transfer, or three-dimensional effects that could alter the relative importance of the three mechanisms.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Nonlinear shocks usually dominate damping of planet-launched density waves, but cooling on orbital timescales rivals them for sub-thermal planets while viscosity needs high values to matter.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"6fc33996f1fe6c5bd02c7ef76183b88a47ba3f1609d7c63a8223c298548f9058"},"source":{"id":"2605.12607","kind":"arxiv","version":1},"verdict":{"id":"c8bd6ac8-81fd-42f8-a4d8-9b1084ffb766","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-14T20:22:23.127479Z","strongest_claim":"nonlinear wave evolution leading to shock formation is typically the most important cause of angular momentum deposition, but that cooling on timescales comparable to local orbital time reaches similar levels of importance for low mass planets (sub-thermal, q_th<1). On the contrary, linear wave damping due to viscosity is rather inefficient, requiring α ≳ 10^{-1.5} to noticeably affect damping of waves launched by thermal mass planets.","one_line_summary":"Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The hydrodynamic simulations capture all relevant damping physics without missing contributions from magnetic fields, realistic radiative transfer, or three-dimensional effects that could alter the relative importance of the three mechanisms.","pith_extraction_headline":"Nonlinear shocks usually dominate damping of planet-launched density waves, but cooling on orbital timescales rivals them for sub-thermal planets while viscosity needs high values to matter."},"references":{"count":273,"sample":[{"doi":"10.1088/0004-637x/760/1/22","year":null,"title":"Angular Momentum Transport and Variability in Boundary Layers of Accretion Disks Driven by Global Acoustic Modes","work_id":"0ac9d16b-dafc-4d0b-ba13-76741a2ccecc","ref_index":2,"cited_arxiv_id":"1205.4009","is_internal_anchor":true},{"doi":"10.48550/arxiv.2203.09991","year":2023,"title":"534, Protostars and Planets VII","work_id":"fa74ff62-367f-4052-97aa-2ffd000b61a3","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1046/j.1365-8711.2001.04619.x","year":2001,"title":"2001, MNRAS, 322, 231, doi: 10.1046/j.1365-8711.2001.04022.x","work_id":"8bb90ab1-6c70-43ec-a616-cee37e93934d","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1086/178107","year":null,"title":"Radiatively Damped Density Waves in Optically Thick Protostellar Disks. , keywords =. doi:10.1086/178107 , adsurl =","work_id":"8c2d1514-a77a-46bd-a96c-390ce80f61d8","ref_index":6,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1088/0004-637x/703/1/845","year":null,"title":"On the horseshoe drag of a low-mass planet. I - Migration in isothermal disks","work_id":"92b7f439-87e3-4c67-ab9e-aeb8b02d6f55","ref_index":7,"cited_arxiv_id":"0907.4677","is_internal_anchor":true}],"resolved_work":273,"snapshot_sha256":"2c6a6db5f675b3bb520a377fd3ab59b1dee362e2be9cd650dfb94c3a96e1dfc1","internal_anchors":12},"formal_canon":{"evidence_count":2,"snapshot_sha256":"383db3699a8f0d1df4bb7d3c76d235fa67f80a32f82de73656a6e2c86a34722e"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}