Triple

T5537974
Position Surface form Disambiguated ID Type / Status
Subject Richard C. Tolman E145213 entity
Predicate knownFor P22 FINISHED
Object Tolman–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: Tolman–Oppenheimer–Volkoff limit | Statement: [Richard C. Tolman, knownFor, Tolman–Oppenheimer–Volkoff limit]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07 
Target entity: Tolman–Oppenheimer–Volkoff limit
Context triple: [Richard C. Tolman, knownFor, Tolman–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. 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.
  • D. 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.
  • 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_69c008fa64888190adae56c8f9ea4031 completed March 22, 2026, 3:21 p.m.
NER Named-entity recognition batch_69c01fb19cb8819088b21e8ebef63d8b completed March 22, 2026, 4:58 p.m.
NED1 Entity disambiguation (via context triple) batch_69c02817cb04819088df72950c791144 completed March 22, 2026, 5:34 p.m.
Created at: March 22, 2026, 3:34 p.m.