Infrared spectral variability of CVSO 1942. The blue, orange, and red lines are observations from JWST/MIRI (2024), Spitzer/IRS-LowRes (2005), and Spitzer/IRS-HiRes (2008), respectively. The best fit to the IRS-LowRes spectrum is shown as a black dashed line, which represents the combination of the photosphere (gray dotted line), the optically thin dust (brown solid line), and the outer wall (green solid line), as described in C. Espaillat et al. (2012). By adding a blackbody component with T=1400 K (pink solid line) to the 2005 Spitzer model, we can fit the JWST/MIRI observation. The purple and red vertical bars denote the range of observations with WISE W1 and W2, shown in Figure 2.