The fitting of a modeled disk with the
Spectral Energy Distribution of J0808 indicates a disk temperature of about 263
K (-10
°C or 14
°F). The follow-up study found that a single disk had a poor match with the 22 μm data. The researchers found a better match with a "warm" outer disk with a temperature of about 240 K (-33 °C or -28 °F) and a "hot" inner disk with a temperature of about 1100 K (827 °C or 1520 °F). The warm outer disk is located around 0.115
au and the hot inner disk is located around 0.0056 au. The hot inner disk is likely the source of accreted material. The temperature of the inner disk is comparable to temperatures where
amorphous silicates
anneal into
crystalline form. The inner disk also lies near the
Roche limit of the red dwarf and therefore the inner disk could be the result of disrupted
planetesimals. The warm outer disk could be similar to dust belts seen around B- to K-type stars, which have temperatures around 190 K and which likely represent small dust grains of
sublimating ice from icy
planetesimals.
ALMA detected a third component with a temperature of 20 K (-253 °C or -424 °F). Using this temperature the researchers were able to estimate the dust mass to 0.057±0.006 . This is higher than the disk mass around ~20
Myr old
AU Microscopii and the ~50 Myr old
GJ 182, but smaller than the ~10 Myr old
TWA 7. The disk has a radius smaller than 16
au. The missing CO detection is explained with two possible scenarios: Either dust grains are released in a collisional cascade induced by the collisions of km-sized planetesimals or a recent collision of planetary bodies generated a large amount of small dust grains. A light curve from
CTIO shows variations, which could be disk material blocking light from the star. The
TESS light curve shows aperiodic dipping on timescales of 0.5–2 days. == Peter Pan disks ==