Triple

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).

Phrase: Strömgren sphere | Statement: [H II region, relatedTo, Strömgren sphere]

Target entity: Strömgren sphere
Context triple: [H II region, relatedTo, Strömgren sphere]

• A. Milne–Eddington approximation
  The Milne–Eddington approximation is a simplified model of stellar atmospheres that assumes constant physical properties with depth to make the radiative transfer equations analytically tractable.
• 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. Rosseland
  Rosseland is a Norwegian surname most notably associated with astrophysicist Svein Rosseland, a pioneer in theoretical astrophysics and radiative transfer.
• 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. chosen
• G. Unsure - the case is ambiguous/there is not enough information to decide.

Target entity: Strömgren sphere
Target entity description: A Strömgren sphere is a region of ionized hydrogen gas surrounding a hot, young star, formed where the star’s ultraviolet radiation balances the recombination of electrons and protons in the surrounding interstellar medium.

• A. Milne–Eddington approximation
  The Milne–Eddington approximation is a simplified model of stellar atmospheres that assumes constant physical properties with depth to make the radiative transfer equations analytically tractable.
• 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. Rosseland
  Rosseland is a Norwegian surname most notably associated with astrophysicist Svein Rosseland, a pioneer in theoretical astrophysics and radiative transfer.
• 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. chosen