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Incoming links: HD 149026 b
Bun'ei Sato 2026-11-05
Bun'ei Sato coauthored the discovery study of the transiting planet HD 149026 b. Combining a transit radius with a radial-velocity mass made its high bulk density informative about planetary interior models. The inference depends on both measured quantities and the assumed composition model.[ref]
The N2K Consortium. II. A Transiting Hot Saturn Around HD 149026 With a Large Dense Core by Bun'ei Sato and others. author list and the described study’s abstract or introductory account
HD 149026 b Created 2026-10-05 Updated 2026-11-05
HD 149026 b is a transiting, roughly Saturn-mass exoplanet whose small measured radius made it an early test of giant-planet composition. The discovery combined Doppler spectroscopy at two observatories with ground-based exoplanet transit photometry: the first constrains mass, the second radius and orbital inclination. The original exoplanet interior models required a substantial inventory of elements heavier than hydrogen and helium to reproduce the measured compactness.[ref]
The N2K Consortium. II. A Transiting Hot Saturn Around HD 149026 With a Large Dense Core by Bun'ei Sato and others. Abstract: radial-velocity observations, three complete transits, and the mass-radius interpretation
The inferred concentration of heavy material is a model result, rather than an image of a planetary core. Its partition between a central core and the surrounding envelope depends on the assumed equation of state, age, and temperature; this illustrates exoplanet interior-composition degeneracy.
Past exam of the mathematics course of the University of Cambridge 2018 iii Paper 315 4 d Solution Created 2026-10-03 Updated 2026-10-14
A mass-radius curve of solar-composition substellar objects must specify age, irradiation and composition. For a mature, weakly irradiated hydrogen–helium sequence, the qualitative mass-radius relation has three main trends:
- At low giant-planet masses, weak compression allows a rough scaling at nearly fixed mean mass density. Radius rises toward a broad maximum around one to a few Jupiter masses.
- Through massive gas giants and brown dwarfs, radii remain near Jupiter's and eventually decline as compression and electron degeneracy pressure become important. A nonrelativistic degenerate stellar polytrope gives the approximate polytropic mass-radius relation ; finite thermal pressure and real equations of state flatten and modify this idealized scaling.
- Above the hydrogen-burning minimum mass, sustained hydrogen burning supplies the energy that supports a rising low-mass main-sequence branch. For near-solar composition, the threshold is around Jupiter masses (about solar masses), with composition-dependent variation. Red dwarfs then have radii increasing with mass, approximately linearly over part of the low-mass sequence.
The conventional deuterium-burning mass near Jupiter masses marks a commonly used giant-planet/brown dwarf classification scale, not a sharp discontinuity in radius or a universal formation boundary. Young brown dwarfs are larger and cool by contraction; irradiation, a heavy-element core and hot-Jupiter radius inflation shift planets away from a single solar-composition curve.
The drawing is a qualitative mature sequence, not an interpolation of a specified evolutionary model grid. Three relevant observations, using representative historical measurements, are:
- Inflated radii: HD 209458 b has a radius around at a mass around , illustrating hot-Jupiter radius inflation relative to a simple mature unirradiated sequence. Early transit photometry measured its unusually large radius.
- Compact metal-enriched planets: HD 149026 b was measured near and . Its small radius for its mass and irradiation implies substantial heavy-element enrichment in interior models, showing the importance of composition in the planetary mass-radius relation; see the discovery analysis.
- Jupiter-like sizes at substellar masses: CoRoT-3b was measured near but only , supporting the broad near-constant-radius region extending into brown dwarf masses. Its measured mass and radius also illustrate why mass alone does not establish a formation history.