Pith Number

pith:RCOIRK4T

pith:2026:RCOIRK4TAFLVPG6ONHCOVBH5SP

not attested not anchored not stored refs resolved

Red novae, their progenitors, and remnants

Institut dEstudis Espacials de Catalunya), Nadejda Blagorodnova (University of Barcelona, Tomasz Kaminski (Nicolaus Copernicus Astronomical Center of Polish Academy of Sciences)

Red novae are the visible result of non-compact binary star coalescence.

arxiv:2605.17005 v1 · 2026-05-16 · astro-ph.SR · astro-ph.HE

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Add to your LaTeX paper

\usepackage{pith}
\pithnumber{RCOIRK4TAFLVPG6ONHCOVBH5SP}

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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

Red novae are now widely interpreted as the outcome of binary coalescence involving non-compact stars, providing a rare opportunity to directly observe the dynamical phases of stellar mergers and their immediate aftermath.

C2weakest assumption

The observed properties of cool slowly expanding ejecta, red evolution, and dust formation are taken as sufficient to identify these transients as merger events rather than other classes of optical transients.

C3one line summary

A synthesis of observational data on red novae as stellar merger events, including outburst properties, progenitor diversity, and long-term remnants.

References

299 extracted · 299 resolved · 139 Pith anchors

[1] SiO production in interstellar shocks. , keywords =

[2] The Millimeter-Wave Spectrum of AlOH. , keywords =. doi:10.1086/187013 , adsurl = · doi:10.1086/187013

[3] An observational study of dust nucleation in Mira ($o$ Ceti): I. Variable features of AlO and other Al-bearing species · doi:10.1051/0004-6361/201628664

[4] Optical and IR Telescope Instrumentation and Detectors , year = 2000, editor = 2000 · doi:10.1117/12.395433

[5] Instrument Design and Performance for Optical/Infrared Ground-based Telescopes , year = 2003, editor = 2003 · doi:10.1117/12.458957

Formal links

2 machine-checked theorem links

Receipt and verification

First computed	2026-05-20T00:03:35.598758Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

889c88ab930157579bce69c4ea84fd93e307b7056348acf6ec0df2bd7278166b

Aliases

arxiv: 2605.17005 · arxiv_version: 2605.17005v1 · doi: 10.48550/arxiv.2605.17005 · pith_short_12: RCOIRK4TAFLV · pith_short_16: RCOIRK4TAFLVPG6O · pith_short_8: RCOIRK4T

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/RCOIRK4TAFLVPG6ONHCOVBH5SP \
  | 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: 889c88ab930157579bce69c4ea84fd93e307b7056348acf6ec0df2bd7278166b

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "e8806d474b72d10f1af09464508cd26b7f4e8d2232f636a95bb353c0dfdae337",
    "cross_cats_sorted": [
      "astro-ph.HE"
    ],
    "license": "http://creativecommons.org/licenses/by/4.0/",
    "primary_cat": "astro-ph.SR",
    "submitted_at": "2026-05-16T14:06:02Z",
    "title_canon_sha256": "174f7fd07e8161bc9baf52c26427dd34d623a4334dc0781b808d110971735865"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2605.17005",
    "kind": "arxiv",
    "version": 1
  }
}