Triple

T365119
Position Surface form Disambiguated ID Type / Status
Subject Chandrasekhar–Friedman–Schutz instability E7942 entity
Predicate relatedTo P37 FINISHED
Object Chandrasekhar limit E9076 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: Chandrasekhar limit | Statement: [Chandrasekhar–Friedman–Schutz instability, relatedTo, Chandrasekhar limit]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07 
Target entity: Chandrasekhar limit
Context triple: [Chandrasekhar–Friedman–Schutz instability, relatedTo, Chandrasekhar limit]
  • A. Chandrasekhar limit chosen
    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. Chandrasekhar number
    The Chandrasekhar number is a dimensionless quantity in magnetohydrodynamics that measures the relative importance of magnetic forces compared to viscous forces in a conducting fluid.
  • 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_69a2e7e880008190a6ad7e06e5d03007 completed Feb. 28, 2026, 1:04 p.m.
NER Named-entity recognition batch_69a2ebe6c1b4819083335e880c205ed6 completed Feb. 28, 2026, 1:21 p.m.
NED1 Entity disambiguation (via context triple) batch_69a3e8668b848190b68d19819ac134df completed March 1, 2026, 7:19 a.m.
Created at: Feb. 28, 2026, 1:08 p.m.