To fit one specific definition of a Peter Pan disk, the source needs to have an infrared "color" of
This low-mass star showed signs of youth, for example a strong infrared excess and active accretion of gaseous material.
It is part of the 45+11−7 Myr old Carina young moving group, older than expected for these characteristics of an M-dwarf.
[3][4] Other stars and brown dwarfs were discovered to be similar to J0808, with signs of youth while being in an older moving group.
[4][2] Together with J0808, these older low-mass accretors in nearby moving groups have been called Peter Pan disks in one scientific paper published in early 2020.
[7][12][13] A detailed study of J0446B with JWST MIRI detected 9 hydrocarbons, two nitrogen-bearing species, two isotopes of CO2, molecular hydrogen and two noble gases.
The researchers of this study concluded that the current X-ray luminosity of Peter Pan disk cannot explain their old age.
[18] Murphy et al. found additional Peter Pan disks in the literature, which were identified as part of the Columba and Tucana-Horologium associations.
[2] The paper also mentions that members of NGC 2547 were previously identified to have 22 μm excess and could be similar to Peter Pan disks.
[2] There are different models to explain the existence of Peter Pan disks, such as disrupted planetesimals[4] or recent collisions of planetary bodies.
[1][2] Peter Pan disks that form multiplanetary systems could force the planets in close-in, resonant orbits.
A longer lifetime for a disk would give more time for a solid core to form, which could initiate runaway core-accretion.