On moving shadows and pressure bumps in HD 169142. (arXiv:2007.11565v3 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Bertrang_G/0/1/0/all/0/1">Gesa H.-M. Bertrang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flock_M/0/1/0/all/0/1">Mario Flock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keppler_M/0/1/0/all/0/1">Miriam Keppler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trifonov_T/0/1/0/all/0/1">Trifon Trifonov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penzlin_A/0/1/0/all/0/1">Anna B. T. Penzlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avenhaus_H/0/1/0/all/0/1">Henning Avenhaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Thomas Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montesinos_M/0/1/0/all/0/1">Matias Montesinos</a>
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.
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.
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