| From [[https://www.iaea.org/publications/8505/neutron-generators-for-analytical-purposes|INTERNATIONAL ATOMIC ENERGY AGENCY, Neutron Generators for Analytical Purposes, IAEA Radiation Technology Reports No. 1, IAEA, Vienna (2012)]] | | {{phylabs:lab_courses:supplemental-material:fun:fig_7.png}} | | //FIG. 7. Neutron capture cross-sections of the stable nuclides.// |

| From [[https://doi.org/10.1073/pnas.1812905116 | Growth model interpretation of planet size distribution]] | {{phylabs:lab_courses:supplemental-material:fun:growth_model_interpretation_of_planet_size_distribution_fig_2.png?900px}} | | Blowup of Fig. 1. Radius gap at 2 $R_⊕$ separates two distinctive groups of RV planets (1.4–1.9 and 2–3 $R_⊕$ ). Their smooth kernel mass distributions on the bottom x axis show a significant offset, with truncation of the super-Earths (yellow) and sub-Neptunes (purple) at ∼10 and ∼20 $M_⊕$ , respectively. The histogram on the left y axis compares the results of Monte-Carlo simulation (light blue) with the observations (yellow). Two sets of H${}_{2}$O M–R curves (blue, 100 mass% H${}_{2}$O; cyan, 50 mass% H${}_{2}$O; cores consist of rock and H${}_{2}$O ice in 1:1 proportion by mass) are calculated for an isothermal fluid/steam envelope at 300, 500, 700, and 1,000 K, sitting on top of ice VII-layer at the appropriate melting pressure. A set of mass–radius curves (upper portion of the diagram) is calculated for the same temperatures assuming the addition of an isothermal 2 mass% H${}_{2}$-envelope to the top of the 50 mass% H${}_{2}$O-rich cores. |

| Originally seen in [[https://www.npr.org/2025/07/08/nx-s1-5157748/ohio-oil-gas-wells-plug]] | | {{phylabs:lab_courses:supplemental-material:fun:oil_well_bonds.png}} | | Does not really facilitate any kind of comparison other than ranking by total cost. |