Day 2 of Debris Disk Connection conference.
This time it is about regular debris disks around regular main sequence stars. Thanks to recent infrared observations from JWST and the 1.3 mm ALMA radio interferometry survey, we have unprecedented details about the shapes of debris disks and gas profiles. As for the reason that astronomers study debris disks at different wavelengths, the wavelength of the scattered or emitted light is proportional to the size of the dust grains. So JWST will resolve the warm debris disks that are located closer to the star, and the small cold dust grains that are farther away than the mm grains due to radiation pressure. Anyways, these new, very detailed data are a testbed for a whole bunch of theoretical models. In broad strokes, three processes affect debris disk shapes. One, collisional cascade, in which collisions between planetesimals will shatter the objects into smaller pieces, triggering further collisions between the pieces. Two, Poynting-Robertson drag, which is caused by uneven emission of radiation after absorbing solar radiation due to the dust moving around the sun. Third, larger planetesimals or planets can perturb or stir debris disks due to their gravity. All these factors can affect the shape of the ring, dust size distribution, disk eccentricity (how oval it is), brightness asymmetry, and other asymmetric features. Finally, they have started probing on debris disk populations around M dwarfs, the stars with the lowest possible mass.
Even a bigger deal though, is that now we have a lot more studies and details on gas around debris disks. Something that even two years ago, while we did detect gas such as carbon monoxide (CO) were around disks, we did not have enough papers coming out to detail them. With current observations, we can begin resolving whether the gas is mainly primordial or replenished. Aside from further details on gas and dust compositions, we now know that the gas profile follow dust profile, and that there are gas asymmetry in the disks. They also observed that there is opacity to the radio waves from CO. Furthermore, since they know more about gas around debris disks, they can finally do fluid simulations, and model gas asymmetry and the dampening of dust velocity.
A notable result on debris disk gas that the talks loved to bring up was they detected fluorescence from CO around the star 49 ceti using JWST near infrared spectrograph. The emission even has evenly spaced peaks due to vibrational states of the CO molecule (Worthen et al 2025):
This curve is best explained by having some dust population fluoresce from UV light combined with some dust being hit by infrared.
A fun fact I found out from one of the talks. There is a debris disk picture from the Artemis II moon mission:
The two spike like features from the moon image is from light scattered by dust particles in the inner solar system, called zodiacal dust. The presenter had a slide that declared the picture wins the award for best debris disk observation of the year.














