Triple

T12177250
Position Surface form Disambiguated ID Type / Status
Subject Tolman–Oppenheimer–Volkoff equation E290118 entity
Predicate relatedTo P37 FINISHED
Object Oppenheimer–Volkoff limit E59370 NE FINISHED

How this triple was built (2 steps)

Every LLM step that produced this triple, in pipeline order — named-entity classification, the disambiguation choices (the exact options shown, with the pick highlighted), and the generated description. The batch + timestamp of each is in the Provenance table below.

NER Named-entity recognition gpt-5-mini
Instruction
Given a phrase, classify it is english named entity (e.g., persons, organizations, works of art) in Latin script, or not (e.g., literals, dates, URLs, verbose phrases). For disambiguation, the statement where the phrase occurs as object is also given. Please return a JSON object with `phrase` (string, the phrase being analyzed) and `is_ne` (boolean, indicating whether the phrase is a Named Entity).
Input
Phrase: Oppenheimer–Volkoff limit | Statement: [Tolman–Oppenheimer–Volkoff equation, relatedTo, Oppenheimer–Volkoff limit]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07 
Target entity: Oppenheimer–Volkoff limit
Context triple: [Tolman–Oppenheimer–Volkoff equation, relatedTo, Oppenheimer–Volkoff limit]
  • A. Oppenheimer–Volkoff limit chosen
    The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.
  • B. Chandrasekhar limit
    The Chandrasekhar limit is the maximum mass a white dwarf star can have before collapsing under its own gravity, playing a crucial role in determining its ultimate fate as a neutron star or black hole.
  • C. Eddington limit
    The Eddington limit is the maximum luminosity a star or accreting object can have before radiation pressure overcomes gravity and drives away its outer layers.
  • D. Tolman–Oppenheimer–Volkoff equation
    The Tolman–Oppenheimer–Volkoff equation is the general relativistic equation of hydrostatic equilibrium that describes the internal structure and pressure balance of spherically symmetric, non-rotating stars such as neutron stars.
  • E. Bonnor–Ebert mass
    The Bonnor–Ebert mass is the maximum mass a pressure-confined, self-gravitating gas sphere can have while remaining in stable hydrostatic equilibrium before collapsing under its own gravity.
  • F. None of above.
  • G. Unsure - the case is ambiguous/there is not enough information to decide.

Provenance (3 batches)

The batch behind each pipeline step, in order, with when it ran. Timestamps are batch-level — stages were processed in waves, so the object chain (NER → NED1 → NEDg → NED2) reads in order, but predicate / elicitation batches can sit in a different wave.

Step Stage Batch ID Status When
creating Elicitation batch_69d6ab4d6c00819095a9a7c35de83cfb completed April 8, 2026, 7:23 p.m.
NER Named-entity recognition batch_69d915fa6ff08190a1ddb3606c229cad completed April 10, 2026, 3:23 p.m.
NED1 Entity disambiguation (via context triple) batch_69f5f6ab19288190a882c842d74a2e30 completed May 2, 2026, 1:05 p.m.
Created at: April 8, 2026, 9:50 p.m.