WISEA J044634.16-262756.1

J0446B shows stronger and broader H-alpha emission, likely from weak accretion of 2.5 × 10⁻¹¹M_☉/yr. The disk was also detected with ALMA, which will be described in a future work. The dust mass was estimated to be 0.1 M_🜨 from ALMA, which is quite low when compared to younger disks. A research team used JWST MIRI to observe J0446B. The researchers found a large number of molecules in the inner disk of this red dwarf. The researchers detected 9 hydrocarbons (methyl radical, methane, acetylene [C₂H₂ and ¹³CCH₂], ethylene, ethane, propyne, diacetylene, and benzene),^[4][5][2] two nitrogen-bearing species (hydrogen cyanide and cyanoacetylene), two isotopes of carbon dioxide (¹²CO₂ and ¹³CO₂), molecular hydrogen and two noble gases (neon and argon). Weak emission of the water molecule is also present. Additionally the spectrum showed amorphous silicate (modelled with olivine) and crystalline silicate of forsterite. Molecular hydrogen and neon is usually only found in young disks with ages of a few million years. This indicates that the disk in J0446B contains primordial gas. Other works in the past tried to explain Peter Pan disks with other scenarios, such as the collision of planetesimals, but the presence of molecular hydrogen and neon excludes these scenarios for J0446B. The line strength of neon and argon indicate that the main ionizing source are soft x-ray and UV photons coming from J0446. The disk is very carbon-rich, which was also seen in other late M-dwarf disks with Spitzer and JWST. J0446B has the highest acetylene to water line ratio detected for an M-dwarf. Theories suggest that the inner disk will first become water-rich due to inwards drift of icy pebbles and then will become carbon-rich, as outer gas flows inwards. The carbon-rich inner disk of J0446B indicates that it represents the final stage of this evolution.^[2]

A long-lived disk can provide more time for planetary cores to form via the core-accretion process. Disk gas dampens orbital eccentricity and facilitates planet migration. This can result in compact planetary systems with resonant chains, such as the TRAPPIST-1 system. The high carbon content in the gaseous disk could lead to carbon-rich atmospheres. This could lead to hazes, such as seen in Titan or it could influence the mean molecular weight and thermal structure of such atmospheres. Because carbon is in the gas-phase, the solids should have relative little carbon. If carbon is lost in the gas-phase and terrestrial planets are assembled from solids at a late stage, these rocky planets would be carbon-poor.^[2]