Triple

T12177400
Position Surface form Disambiguated ID Type / Status
Subject Bonnor–Ebert mass E290122 entity
Predicate relatedTo P37 FINISHED
Object Bonnor–Ebert sphere E290122 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: Bonnor–Ebert sphere | Statement: [Bonnor–Ebert mass, relatedTo, Bonnor–Ebert sphere]
NED1 Entity disambiguation (via context triple) gpt-5-mini-2025-08-07 
Target entity: Bonnor–Ebert sphere
Context triple: [Bonnor–Ebert mass, relatedTo, Bonnor–Ebert sphere]
  • A. Bonnor–Ebert mass chosen
    The Bonnor–Ebert mass is the maximum mass a pressure-confined, self-gravitating gas sphere can have while remaining in stable hydrostatic equilibrium before collapsing under its own gravity.
  • B. Bok globules
    Bok globules are small, dense, and dark interstellar clouds of gas and dust that often serve as sites of early star formation.
  • C. 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.
  • 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. Tolman–Oppenheimer–Volkoff equation
    The Tolman–Oppenheimer–Volkoff equation is the general relativistic equation of hydrostatic equilibrium that describes the internal structure and pressure balance of spherically symmetric, non-rotating stars such as neutron stars.
  • 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_69d6ab4d6c00819095a9a7c35de83cfb completed April 8, 2026, 7:23 p.m.
NER Named-entity recognition batch_69d915fa6ff08190a1ddb3606c229cad completed April 10, 2026, 3:23 p.m.
NED1 Entity disambiguation (via context triple) batch_69f5f6ab19288190a882c842d74a2e30 completed May 2, 2026, 1:05 p.m.
Created at: April 8, 2026, 9:50 p.m.