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Probing the 3D Structures of Supernovae through IR Signatures of CO and SiO

  • Authors: T. Mera, P. Hoeflich, C. R. Burns, C. Ashall, K. Medler, E. Fereidouni, W. B. Hoogendam, M. Shahbandeh, S. Shiber, C. M. Pfeffer, E. Baron, J. Lu, N. Morrell, E. Y. Hsiao, M. M. Phillips

T. Mera et al 2026 The Astrophysical Journal 1003 .

  • Provider: AAS Journals

Caption: Figure 4.

Demonstrating the sensitivity of each parameter on the CO fundamental band of Model P at day 385 (see Table 1), where the temperature profile has been optimized for each. Panel (A) shows the best-fit solution and continuum. Each of the following panels keeps the optimized parameters the same but shows the effect of: (B) the total molecular mass (M), (C) the inner temperature (T1), (D) the density structure (n), (E) the inner velocity edge (v1), (F) the width of the molecular region (Δv), (G) the clump density contrast (fc), (H) the clump size (rR), and (I) the clump shape (ϵ). Figures 6 and 7 show the ﹩{\chi }_{* }^{2}﹩ convergences of the fits.

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