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Phosphine Depletion in Brown Dwarf Atmospheres Explained due to Metal Phosphide Formation

  • Authors: Rongzhang Yin, Yan Li, Yanzhang Li, Sara Seager

Rongzhang Yin et al 2026 The Astrophysical Journal Letters 1002 .

  • Provider: AAS Journals

Caption: Figure 2.

Comparison of predicted PH3 equilibrium abundances in the presence and absence of metal phosphides ([Fe/H] = −0.5). (a) Predicted PH3 equilibrium abundances in the absence of metal phosphides. (b) Predicted PH3 equilibrium abundances in the presence of metal phosphides. The gray dotted lines show the PH3 abundance contours in panel (a). The white dashed lines represent the condensation lines of the corresponding metal phosphides in panel (b). The pink and orange dashed–dotted lines represent the condensation lines (solid or liquid phase) of Fe and Ni elements, respectively. The solid lines are the TP profiles of three brown dwarfs: brown dwarf Sonora (red), WISE 0855 (yellow) and Wolf 1130C (blue). The three blue lines are the median (center line) and ±1σ uncertainty boundaries (side lines) for the TP profiles of Wolf 1130C.

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