Triple
T93522
| Position | Surface form | Disambiguated ID | Type / Status |
|---|---|---|---|
| Subject | Subrahmanyan Chandrasekhar |
E1879
|
entity |
| Predicate | knownFor |
P22
|
FINISHED |
| Object |
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.
|
E9076
|
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: Chandrasekhar limit | Statement: [Subrahmanyan Chandrasekhar, knownFor, Chandrasekhar limit]
NED1
Entity disambiguation (via context triple)
gpt-5-mini-2025-08-07
Target entity: Chandrasekhar limit Context triple: [Subrahmanyan Chandrasekhar, knownFor, Chandrasekhar limit]
-
A.
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.
-
B.
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.
-
C.
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.
-
D.
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.
-
E.
Subrahmanyan Chandrasekhar
Subrahmanyan Chandrasekhar was an Indian-American astrophysicist and Nobel laureate renowned for his work on stellar structure and evolution, particularly the Chandrasekhar limit for white dwarfs.
- 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: Chandrasekhar limit Triple: [Subrahmanyan Chandrasekhar, knownFor, Chandrasekhar limit]
Generated description
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.
NED2
Entity disambiguation (via description)
gpt-5-mini-2025-08-07
Target entity: Chandrasekhar limit Target entity description: 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.
-
A.
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.
-
B.
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.
-
C.
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.
-
D.
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.
-
E.
Subrahmanyan Chandrasekhar
Subrahmanyan Chandrasekhar was an Indian-American astrophysicist and Nobel laureate renowned for his work on stellar structure and evolution, particularly the Chandrasekhar limit for white dwarfs.
- 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_69a24d1a97dc819094e6c021fe9b05a7 |
completed | Feb. 28, 2026, 2:04 a.m. |
| NER | Named-entity recognition | batch_69a24fd28e988190bde699647ee5b16b |
completed | Feb. 28, 2026, 2:15 a.m. |
| NED1 | Entity disambiguation (via context triple) | batch_69a266ebb994819085fb84dd1d2d25ad |
completed | Feb. 28, 2026, 3:54 a.m. |
| NEDg | Description generation | batch_69a267b740388190a321023aa52a539a |
completed | Feb. 28, 2026, 3:57 a.m. |
| NED2 | Entity disambiguation (via description) | batch_69a2685dc64c8190bd611985d1bc27a3 |
completed | Feb. 28, 2026, 4 a.m. |
Created at: Feb. 28, 2026, 2:07 a.m.