Triple

T1263706
Position Surface form Disambiguated ID Type / Status
Subject Richard C. Tolman E12555 entity
Predicate notableWork P4 FINISHED
Object Tolman–Oppenheimer–Volkoff limit in relativistic stellar structure 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 in relativistic stellar structure | Statement: [Richard C. Tolman, notableWork, Tolman–Oppenheimer–Volkoff limit in relativistic stellar structure]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07 
Target entity: Tolman–Oppenheimer–Volkoff limit in relativistic stellar structure
Context triple: [Richard C. Tolman, notableWork, Tolman–Oppenheimer–Volkoff limit in relativistic stellar structure]
  • 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–Friedman–Schutz instability
    The Chandrasekhar–Friedman–Schutz instability is a gravitational-radiation-driven instability in rotating stars that can cause certain oscillation modes to grow by emitting gravitational waves.
  • C. Schwarzschild–Milne equations
    The Schwarzschild–Milne equations are fundamental integro-differential equations in radiative transfer theory that describe the propagation and scattering of radiation through a plane-parallel, absorbing and emitting medium.
  • D. 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.
  • E. Oppenheimer–Snyder model
    The Oppenheimer–Snyder model is a pioneering theoretical description of gravitational collapse in general relativity, providing one of the first rigorous treatments of how a massive star can form a black hole.
  • 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_69a4933352e08190ac617291985e76c0 completed March 1, 2026, 7:27 p.m.
NER Named-entity recognition batch_69a4bfc8d6908190a5b2cf1051cc6d5e completed March 1, 2026, 10:38 p.m.
NED1 Entity disambiguation (via context triple) batch_69ac9984c21c8190a1cec6c9d2df217a completed March 7, 2026, 9:32 p.m.
Created at: March 1, 2026, 7:50 p.m.