Triple
T2707227
| Position | Surface form | Disambiguated ID | Type / Status |
|---|---|---|---|
| Subject | Oppenheimer–Volkoff limit |
E59370
|
entity |
| Predicate | distinguishedFrom |
P1612
|
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: [Oppenheimer–Volkoff limit, distinguishedFrom, Chandrasekhar limit]
NED1
Entity disambiguation (via context triple)
gpt-5-mini-2025-08-07
Target entity: Chandrasekhar limit Context triple: [Oppenheimer–Volkoff limit, distinguishedFrom, 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.
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.
-
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.
Bonnor–Ebert mass
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.
-
E.
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.
- 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_69ab4ac66bc88190b9e4afa5fc843f72 |
completed | March 6, 2026, 9:44 p.m. |
| NER | Named-entity recognition | batch_69abda725f24819090e8d936b3d2d5bc |
completed | March 7, 2026, 7:57 a.m. |
| NED1 | Entity disambiguation (via context triple) | batch_69afbbbc2eec819082f6e6e157d4efc7 |
completed | March 10, 2026, 6:35 a.m. |
Created at: March 6, 2026, 9:55 p.m.