HD 152384: A 5 Myr old debris disk system showing a gaseous ring of refractory elements at the dust sublimation radius

@misc{ancker2026152384,
  title = {{HD 152384: A 5 Myr old debris disk system showing a gaseous ring of refractory elements at the dust sublimation radius}},
  author = {Mario van den Ancker and Daniela Iglesias and Olja Panić and Monika Petr-Gotzens and Miguel Vioque},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.20059},
  eprint = {2610.20059},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.20059},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - HD 152384: A 5 Myr old debris disk system showing a gaseous ring of refractory elements at the dust sublimation radius
AU  - Mario van den Ancker
AU  - Daniela Iglesias
AU  - Olja Panić
AU  - Monika Petr-Gotzens
AU  - Miguel Vioque
PY  - 2026
DA  - 2026/10/14
PB  - arXiv
DO  - 10.48550/arxiv.2610.20059
UR  - https://arxiv.org/abs/2610.20059
AB  - Context: Circumstellar gas around young stars provides key insights into planet formation and disk evolution. HD 152384, a young (5 Myr) A0 V star in Sco-Cen, shows hybrid-disk traits: a modest infrared excess from small dust grains and atomic emission lines dominated by refractory elements, but its disk structure and origin remain unclear. Aims: We characterise the kinematics and excitation of the circumstellar gas around HD 152384 and constrain the physical properties of its emitting region. Methods: We use new high-resolution optical and near-infrared VLT/UVES and VLT/CRIRES spectra to re-examine the circumstellar environment of HD 152384, previously suggested to host a broad, gas-rich disk. Results: The observations reveal 74 narrow, double-peaked emission lines of Fe, Mg, Si, and Ca, with similar profiles and a 103 km/s peak separation. Keplerian modelling places the gas in a geometrically thin ring at 0.09-0.12 au, close to the dust sublimation radius (0.10-0.14 au for a sublimation temperature of about 1500 K). The Fe I emission is optically thick, whereas the optically thin Mg I lines imply 2.2 x 10^22 kg (3.6 x 10^-3 Earth masses) of magnesium gas in the ring. Conclusions: The dust and gas properties are consistent with a secondary origin involving collisions of rocky planetesimals. We propose that small collision-produced dust grains spiral inward and sublimate near the dust sublimation radius, accumulating atomic gas there. HD 152384 thus represents a young analogue of gas-bearing debris disks such as Beta Pictoris and gaseous debris disks around metal-polluted white dwarfs, offering a new window on the early violent processing of rocky planetesimals.
ER  -