Pith Number

pith:56SMOWRR

pith:2026:56SMOWRRVGNTS2RCDMPRCDCZOB

not attested not anchored not stored refs resolved

$\alpha\beta q_\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs

Amelia J. Cordwell, Roman R. Rafikov

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.

arxiv:2605.12607 v1 · 2026-05-12 · astro-ph.EP

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\pithnumber{56SMOWRRVGNTS2RCDMPRCDCZOB}

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Record completeness

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4 Citations open

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Claims

C1strongest 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.

C2weakest 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.

C3one 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.

References

273 extracted · 273 resolved · 12 Pith anchors

[2] Angular Momentum Transport and Variability in Boundary Layers of Accretion Disks Driven by Global Acoustic Modes · doi:10.1088/0004-637x/760/1/22

[4] 534, Protostars and Planets VII 2023 · doi:10.48550/arxiv.2203.09991

[5] 2001, MNRAS, 322, 231, doi: 10.1046/j.1365-8711.2001.04022.x 2001 · doi:10.1046/j.1365-8711.2001.04619.x

[6] Radiatively Damped Density Waves in Optically Thick Protostellar Disks. , keywords =. doi:10.1086/178107 , adsurl = · doi:10.1086/178107

[7] On the horseshoe drag of a low-mass planet. I - Migration in isothermal disks · doi:10.1088/0004-637x/703/1/845

Formal links

2 machine-checked theorem links

Receipt and verification

First computed	2026-05-18T03:10:00.712964Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

efa4c75a31a99b396a221b1f110c59706e1e094734d93c8d9c696a93e67aa606

Aliases

arxiv: 2605.12607 · arxiv_version: 2605.12607v1 · doi: 10.48550/arxiv.2605.12607 · pith_short_12: 56SMOWRRVGNT · pith_short_16: 56SMOWRRVGNTS2RC · pith_short_8: 56SMOWRR

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Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/56SMOWRRVGNTS2RCDMPRCDCZOB \
  | jq -c '.canonical_record' \
  | python3 -c "import sys,json,hashlib; b=json.dumps(json.loads(sys.stdin.read()), sort_keys=True, separators=(',',':'), ensure_ascii=False).encode(); print(hashlib.sha256(b).hexdigest())"
# expect: efa4c75a31a99b396a221b1f110c59706e1e094734d93c8d9c696a93e67aa606

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "afcd1fa6fc675f1295b0ce29007f96741ac08bb2f8e63cfdd4d7354caf14994e",
    "cross_cats_sorted": [],
    "license": "http://creativecommons.org/licenses/by/4.0/",
    "primary_cat": "astro-ph.EP",
    "submitted_at": "2026-05-12T18:00:53Z",
    "title_canon_sha256": "8cb8744842ae780d81bee729a5e79107b3cab7b74b01b8d742256c126afe291d"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2605.12607",
    "kind": "arxiv",
    "version": 1
  }
}