Pith Number

pith:AV6VARRR

pith:2026:AV6VARRRBZOV5PFFAUU3ZN3VGQ

not attested not anchored not stored refs resolved

Accretion geometry and spectral evolution in 1A 1118-61: a comparison of the 2009 and 2026 outbursts

Aru Beri, Kinjal Roy, Phil Charles, Rahul Sharma

The cyclotron line energy in 1A 1118-61 stays nearly constant across a factor of 25 luminosity change between its 2009 and 2026 outbursts.

arxiv:2605.17455 v1 · 2026-05-17 · astro-ph.HE

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\usepackage{pith}
\pithnumber{AV6VARRRBZOV5PFFAUU3ZN3VGQ}

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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

A cyclotron line is detected in the two NuSTAR observations, with its energy remaining nearly constant despite a factor of ~25 change in luminosity; the 2026 outburst is systematically harder and brighter, suggesting significant difference in the accretion structure and emission regions between the two outbursts.

C2weakest assumption

That the spectral model of thermal Comptonization fully captures the emission physics without unaccounted components and that the 2009 and 2026 datasets are directly comparable despite possible differences in instrument calibration or outburst coverage.

C3one line summary

The 2026 outburst of 1A 1118-61 is brighter and spectrally harder than in 2009, with constant cyclotron line energy across large luminosity changes and QPO frequency suggesting magnetospheric instabilities.

References

63 extracted · 63 resolved · 5 Pith anchors

[1] Alpar, M. A., & Shaham, J. 1985, Nature, 316, 239, doi: 10.1038/316239a0 1985 · doi:10.1038/316239a0

[2] 2020, arXiv e-prints, 2010, arXiv:2010.09644 Astropy Collaboration, Robitaille, T 1996 · doi:10.1051/0004-6361/201322068

[3] 2022, MNRAS, 517, 4138, doi: 10.1093/mnras/stac2901 2022 · doi:10.1093/mnras/stac2901

[4] Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3 2021 · doi:10.3847/1538-3881/abd806

[5] Barthelmy, S. D., Barbier, L. M., Cummings, J. R., et al. 2005, Space Sci. Rev., 120, 143, doi: 10.1007/s11214-005-5096-3 2005 · doi:10.1007/s11214-005-5096-3

Formal links

2 machine-checked theorem links

Receipt and verification

First computed	2026-05-20T00:04:39.903482Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

057d5046310e5d5ebca50529bcb775340c3778718b518b8636ab9d9fa9274c0e

Aliases

arxiv: 2605.17455 · arxiv_version: 2605.17455v1 · doi: 10.48550/arxiv.2605.17455 · pith_short_12: AV6VARRRBZOV · pith_short_16: AV6VARRRBZOV5PFF · pith_short_8: AV6VARRR

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/AV6VARRRBZOV5PFFAUU3ZN3VGQ \
  | 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: 057d5046310e5d5ebca50529bcb775340c3778718b518b8636ab9d9fa9274c0e

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "691608e6764ae44b72089a51a6bba6e6583c719668e6e2dd38ff9561e7e637bc",
    "cross_cats_sorted": [],
    "license": "http://creativecommons.org/licenses/by-nc-nd/4.0/",
    "primary_cat": "astro-ph.HE",
    "submitted_at": "2026-05-17T13:55:28Z",
    "title_canon_sha256": "25e2fc2d4d9dd08290da63fcd0638f1d3cc6e329db974a5ffd0651dcf06f9aab"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2605.17455",
    "kind": "arxiv",
    "version": 1
  }
}