Our original motivation for studying dust formation in core collapse supernovae (CCSNe) was the exciting discovery that some high redshift (z > 6) galaxies were dust rich. These galaxies are less than 1 Gyr old, and so a significant fraction of the observed dust must be coming from massive stars, which evolve quickly and return their material back to the interstellar medium through supernovae (SNe). Even still, the amount of dust required per star or SN is high, with theoretical models predicting that 0.1 - 1 solar masses of dust would be needed per CCSN, and many studies by our group and others found that only a small amount of new dust was forming in the SN ejecta. Typically, only about 0.01 - 0.0001 solar masses of dust have formed two or three years after the explosion. How is it that CCSNe have formed only a small amount of dust after three years, but SN 1987A has a dust mass that is several orders of magnitude larger after 25 years? To investigate the suggestion of continuous dust formation, we are using two Monte Carlo Radiative transfer codes to model dust in the circumstellar medium (CSM) and ejecta of SN 2010jl. MOCASSIN fits visible and IR SEDs, while DAMOCLES fits individual emission lines, in particular, H-alpha. When dust is present in the ejecta, the dust will preferentially extinguish emission from the far-side, red-shifted gas and result in a shift of the emission line profiles to the blue and a flattening of the profiles. Both codes estimate the mass of dust produced by SN 2010jl. I present estimates of both new and preexisting dust masses at each epoch for SN 2010jl. The preexisting dust, generated in the wind of the evolved star before it goes supernova, is located in the CSM and is on the order of 0.01-0.1 solar masses for SN 2010jl. The newly formed dust in the cooling ejecta of SN 2010jl is again only on the order of 0.00001-0.0001 solar masses in the first 4 years. This mass of new dust is increasing and may reach levels similar to that of SN 1987A if given enough time. We are continuing our longterm study of the dust mass of SN 2010jl.