2020/07/22 by Gesa H.-M. Bertrang, Gesa H. -M. Bertrang, Mario Flock +17 · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Brightness #Computer science #Context (archaeology) #Debris disk #Earth and Planetary Astrophysics (astro-ph.EP) #Exoplanet #FOS: Physical sciences #Geology #Physics #Planet #Planetary system #RADIUS #Shadow (psychology) #Solar System #Solar and Stellar Astrophysics (astro-ph.SR) #Stars #Stellar, planetary, and galactic studies #Surface brightness #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.2007.11565
published in arXiv (Cornell University) (Cornell University) · Submitted to ApJ, in rev
openalex publication_date 2020/07/22 · arxiv created 2021/04/29 · arxiv updated 2021/04/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The search for young planets had its first breakthrough with the detection of the accreting planet PDS70b. In this study, we aim to broaden our understanding towards the formation of multi-planet systems such as HR8799 or the Solar System. Our previous study on HD169142, one of the closest Herbig stars, points towards a shadow-casting protoplanetary candidate. Here, we present follow-up observations to test our previously proposed hypothesis. We set our new data into context with previous observations to follow structural changes in the disk over the course of 6 years. We find spatially resolved systematic changes in the position of the previously described surface brightness dip in the inner ring. We further find changes in the brightness structure in azimuthal direction along the ring. And finally, a comparison of our SPHERE data with recent ALMA observations reveals a wavelength dependent radial profile of the bright ring. The time-scale on which the changes in the ring's surface brightness occur suggest that they are caused by a shadow cast by a 1-10Mj planet surrounded by dust, an orbit comparable to those of the giant planets in our own Solar System. Additionally, we find the first indications for temperature-induced instabilities in the ring. And finally, we trace a pressure maxima, for the first time spatially resolved, with a width of 4.5au. The density distribution of the ring at mm wavelengths around the pressure maxima could further indicate effects from snow lines or even the dynamics and feedback of the larger grains.