Pith Number

pith:EEWGAKIU

pith:2026:EEWGAKIUHRQQLMF5B4NILHU2LH

not attested not anchored not stored refs resolved

The bound origin of low-mass stellar binaries

A. Generozov, D. Guszejnov, H.B. Perets, K.M. Kratter, M.Y. Grudi\'c, S.S.R. Offner

Simulations show that 70-80% of low-mass binaries form already gravitationally bound when the second star appears.

arxiv:2605.16657 v1 · 2026-05-15 · astro-ph.SR · astro-ph.GA

Open paper page JSON Open Graph Bundle Merged state Verified badge What is a Pith Number?

Add to your LaTeX paper

\usepackage{pith}
\pithnumber{EEWGAKIUHRQQLMF5B4NILHU2LH}

Prints a linked badge after your title and injects PDF metadata. Compiles on arXiv. Learn more · Embed verified badge

Record completeness

1 Bitcoin timestamp

2 Internet Archive

3 Author claim open · sign in to claim

4 Citations open

5 Replications open

✓ Portable graph bundle live · download bundle · merged state

The bundle contains the canonical record plus signed events. A mirror can host it anywhere and recompute the same current state with the deterministic merge algorithm.

Claims

C1strongest claim

≈70-80% of binaries are gravitationally bound from the moment the second star forms. Formation in multiples is the dominant mode of star formation, accounting for at least 57% of stars.

C2weakest assumption

The numerical simulations include all relevant physics and stellar feedback at sufficient resolution to correctly determine whether a newly formed pair is gravitationally bound at the instant the second star appears.

C3one line summary

Hydrodynamical simulations of Milky Way-like cluster formation find that most binaries are bound from formation, half are disrupted by the end of the star-formation epoch, and multiple formation accounts for at least 57% of stars.

References

65 extracted · 65 resolved · 3 Pith anchors

[1] The Evolution of Protostars: Insights from Ten Years of Infrared Surveys with Spitzer and Herschel 2014 · arXiv:1401.1809

[2] and Arzoumanian, Doris and Andr 2023

[3] Offner, S. S. R.et al.Inutsuka, S., Aikawa, Y., Muto, T., Tomida, K. & Tamura, M. (eds)The Origin and Evolution of Multiple Star Systems. (eds Inutsuka, S., Aikawa, Y., Muto, T., Tomida, K. & Tamura, 2023

[4] Chevance, M.et al.The Molecular Cloud Lifecycle.Space Sci. Rev.216, 50 (2020) 2020

[5] Bastian, N.et al.Evidence for environmentally dependent cluster disruption in M83.Mon. Not. R. Astron. Soc.417, L6–L10 (2011) 2011

Receipt and verification

First computed	2026-05-20T00:02:34.785001Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

212c6029143c6105b0bd0f1a859e9a59ce68ec456dd39109bcceaa36e5c02675

Aliases

arxiv: 2605.16657 · arxiv_version: 2605.16657v1 · doi: 10.48550/arxiv.2605.16657 · pith_short_12: EEWGAKIUHRQQ · pith_short_16: EEWGAKIUHRQQLMF5 · pith_short_8: EEWGAKIU

Agent API

Resolver JSON Graph JSON Events JSON Schema Signing key

Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/EEWGAKIUHRQQLMF5B4NILHU2LH \
  | 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: 212c6029143c6105b0bd0f1a859e9a59ce68ec456dd39109bcceaa36e5c02675

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "69d4396e000d13f7033fe67a909b490bad0486dde832b83715bd5dcdd7c8993c",
    "cross_cats_sorted": [
      "astro-ph.GA"
    ],
    "license": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
    "primary_cat": "astro-ph.SR",
    "submitted_at": "2026-05-15T21:52:54Z",
    "title_canon_sha256": "847af9b1fa90aab5763a1dc89dc7ee0a33a85d67030b9e8c47603cb74adf29f4"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2605.16657",
    "kind": "arxiv",
    "version": 1
  }
}