Exploring the Dynamics of Debris Disks through Vertical Thickness Analysis: Case Study of HD32297

Debris disks are circumstellar disks made of dust and rocky material that orbit stars. In the Solar System, the Asteroid and Kuiper Belt are debris disks similar to the ones we observe around other stars. Debris disks provide valuable insights into planetary system dynamics that complement findings from planet and protoplanetary disc studies. Our research probes the implications of the vertical profile shape on the characteristics of the debris disk environment, with a specific focus on the intriguing case of HD 32297. 

One key aspect of our research is the differentiation between the influences of planets, flyby stars and large planetesimals on the vertical shape of debris disks. By understanding these distinct influences, we can gain a deeper understanding of the dynamics of these systems.

We present a multi-wavelength analysis of HD 32297's edge-on debris disk, a well-known disk orbiting a young A star. This system exhibits one of the largest infrared excesses observed among main-sequence stars. HD 32297's disk is highly edge-on and very narrow in mm-dust, so it is one of the best disks to examine the vertical structure profile.

Our high-resolution data enable us to measure the disk's vertical thickness for different radii and, therefore, to create a vertical thickness profile along the radial direction. This makes the system an excellent test bed, allowing us to examine various dynamical models for debris disk interactions.