Triple

T476679
Position Surface form Disambiguated ID Type / Status
Subject Chandrasekhar limit E9076 entity
Predicate relatedConcept 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: [Chandrasekhar limit, relatedConcept, Oppenheimer–Volkoff limit]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07 
Target entity: Oppenheimer–Volkoff limit
Context triple: [Chandrasekhar limit, relatedConcept, 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. Schwarzschild radius
    The Schwarzschild radius is the critical distance from the center of a non-rotating, spherically symmetric mass at which its escape velocity equals the speed of light, defining the boundary of a black hole.
  • E. 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.
  • 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_69a2e7ff81708190b0507a24a997232c completed Feb. 28, 2026, 1:05 p.m.
NER Named-entity recognition batch_69a2f03cc63881908e75b457804cb858 completed Feb. 28, 2026, 1:40 p.m.
NED1 Entity disambiguation (via context triple) batch_69a4746deb4481908d88c50c86b58ee8 completed March 1, 2026, 5:16 p.m.
Created at: Feb. 28, 2026, 1:12 p.m.