Triple

T476658
Position Surface form Disambiguated ID Type / Status
Subject Chandrasekhar limit E9076 entity
Predicate contrastsWith P278 FINISHED
Object Oppenheimer–Volkoff limit
The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.
E59370 NE FINISHED

How this triple was built (4 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, contrastsWith, Oppenheimer–Volkoff limit]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07
Target entity: Oppenheimer–Volkoff limit
Context triple: [Chandrasekhar limit, contrastsWith, Oppenheimer–Volkoff limit]
  • A. 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.
  • B. 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.
  • C. 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.
  • D. 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.
  • E. Bardeen black hole model
    The Bardeen black hole model is a theoretical proposal of a regular (non-singular) black hole solution in general relativity that avoids the central singularity by coupling gravity to nonlinear electrodynamics.
  • F. None of above. chosen
  • G. Unsure - the case is ambiguous/there is not enough information to decide.
NEDg Description generation gpt-5.1
Instruction
Generate a one-sentence description of the target entity. 
You are given a context triple in the form (subject, predicate, object), where the object is the target entity. 
# Instructions
Use the triple to infer relevant information about the entity. Describe the entity based on what is most defining, well-known. 
Avoid repeating the information from the triple, unless really essential.
# Response Format
Return only the sentence: "Description: [one-sentence description of the target entity]"
Input
Entity: Oppenheimer–Volkoff limit
Triple: [Chandrasekhar limit, contrastsWith, Oppenheimer–Volkoff limit]
Generated description
The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.
NED2 Entity disambiguation (via description) gpt-5-mini-2025-08-07
Target entity: Oppenheimer–Volkoff limit
Target entity description: The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.
  • A. 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.
  • B. 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.
  • C. 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.
  • D. 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.
  • E. Bardeen black hole model
    The Bardeen black hole model is a theoretical proposal of a regular (non-singular) black hole solution in general relativity that avoids the central singularity by coupling gravity to nonlinear electrodynamics.
  • F. None of above. chosen

Provenance (5 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_69a46802cf108190a71d45f1ad3262e2 completed March 1, 2026, 4:23 p.m.
NEDg Description generation batch_69a4686a1c448190943fb889cd26c715 completed March 1, 2026, 4:25 p.m.
NED2 Entity disambiguation (via description) batch_69a468c9f5008190b431bc4bd374ab78 completed March 1, 2026, 4:26 p.m.
Created at: Feb. 28, 2026, 1:12 p.m.