Triple

T561903
Position Surface form Disambiguated ID Type / Status
Subject Karl Schwarzschild E13469 entity
Predicate knownFor P22 FINISHED
Object Schwarzschild criterion
The Schwarzschild criterion is a condition in astrophysics that determines when a star’s interior becomes convectively unstable, leading to energy transport by bulk motion of stellar material.
E70353 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: Schwarzschild criterion | Statement: [Karl Schwarzschild, knownFor, Schwarzschild criterion]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07
Target entity: Schwarzschild criterion
Context triple: [Karl Schwarzschild, knownFor, Schwarzschild criterion]
  • 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. 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.
  • C. 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.
  • D. 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.
  • 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. 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: Schwarzschild criterion
Triple: [Karl Schwarzschild, knownFor, Schwarzschild criterion]
Generated description
The Schwarzschild criterion is a condition in astrophysics that determines when a star’s interior becomes convectively unstable, leading to energy transport by bulk motion of stellar material.
NED2 Entity disambiguation (via description) gpt-5-mini-2025-08-07
Target entity: Schwarzschild criterion
Target entity description: The Schwarzschild criterion is a condition in astrophysics that determines when a star’s interior becomes convectively unstable, leading to energy transport by bulk motion of stellar material.
  • 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. 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.
  • C. 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.
  • D. 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.
  • 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. 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_69a4933edcf08190b35ecfd6014caee6 completed March 1, 2026, 7:27 p.m.
NER Named-entity recognition batch_69a49a700e608190b235246df057bd9b completed March 1, 2026, 7:58 p.m.
NED1 Entity disambiguation (via context triple) batch_69a4e9bd6c44819094ba815966ca7937 completed March 2, 2026, 1:37 a.m.
NEDg Description generation batch_69a4ea332c2081909a615287ad0629be completed March 2, 2026, 1:38 a.m.
NED2 Entity disambiguation (via description) batch_69a4eadfefec81908fc3c2522fe79969 completed March 2, 2026, 1:41 a.m.
Created at: March 1, 2026, 7:32 p.m.