Pith Number

pith:CJCP7JKQ

pith:2026:CJCP7JKQITAK53GLS25TRQMNLK

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Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion

Anders Johansen (University of Copenhagen / Lund University), Wladimir Lyra (New Mexico State University)

A narrow range of pebble sizes lets the streaming instability form planetesimals while pebble accretion builds cold giants, super-Earths and rocky embryos together.

arxiv:2604.25816 v1 · 2026-04-28 · astro-ph.EP

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4 Citations open

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Claims

C1strongest claim

We identify an optimum Stokes number range between St=0.01 and St=0.03 where all three planetary classes form and where the streaming instability is triggered for a slightly elevated pebble metallicity. We derive analytically that the mass of the largest planetesimals formed by the streaming instability is of similar magnitude to the threshold mass beyond which pebble accretion becomes efficient, if planetesimals form in the earliest phases of protoplanetary disc evolution.

C2weakest assumption

The models assume that pebble metallicity can be locally elevated enough to trigger the streaming instability and that disc evolution proceeds without strong pressure bumps or rapid gas loss that would alter the pebble flux timing; these are stated as explored parameters but the central ranges depend on them remaining within the simulated bounds.

C3one line summary

An optimal Stokes number window of 0.01-0.03 allows streaming instability to form planetesimals and pebble accretion to build all three main planet classes, with cold gas giants needing the lowest turbulence and largest discs.

References

154 extracted · 154 resolved · 0 Pith anchors

[1] doi:10.1051/0004-6361/202245252 2023 · doi:10.1051/0004-6361/202245252

[2] doi:10.3847/2041-8213/acdb5f 2023 · doi:10.3847/2041-8213/acdb5f

[3] Bai, X.-N. & Stone, J. M.\ 2010, , 722, 2, 1437. doi:10.1088/0004-637X/722/2/1437 2010 · doi:10.1088/0004-637x/722/2/1437

[4] New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit 2015 · doi:10.1051/0004-6361/201425481

[5] Monthly Notices of the Royal Astronomical Society475(4), 5618–5658 (2018) 2018 · doi:10.1093/mnras/sty169

Receipt and verification

First computed	2026-06-24T14:15:58.921571Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

1244ffa55044c0aeeccb96bb38c18d5a95bef839be0ec4274a6bcd7fe6192ba3

Aliases

arxiv: 2604.25816 · arxiv_version: 2604.25816v1 · doi: 10.48550/arxiv.2604.25816 · pith_short_12: CJCP7JKQITAK · pith_short_16: CJCP7JKQITAK53GL · pith_short_8: CJCP7JKQ

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Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/CJCP7JKQITAK53GLS25TRQMNLK \
  | 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: 1244ffa55044c0aeeccb96bb38c18d5a95bef839be0ec4274a6bcd7fe6192ba3

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "9fb34beac15b913a5738857f8c5c4377ae998d44f8468f18b5b478dce206f325",
    "cross_cats_sorted": [],
    "license": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
    "primary_cat": "astro-ph.EP",
    "submitted_at": "2026-04-28T16:25:46Z",
    "title_canon_sha256": "eee40b80d2b07301db41d0f7bb6136d570416ba5f9ff3a496a57a034bea5c9a4"
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  "source": {
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    "kind": "arxiv",
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}