English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Context. The study of protoplanetary disks is fundamental to understand theirevolution and interaction with the surrounding environment, and to constrainplanet formation mechanisms.  Aims. We aim at characterising the young binary system HD 34700 A, whichshows a wealth of structures.  Methods. Taking advantage of the high-contrast imaging instruments SPHERE atthe VLT, LMIRCam at the LBT, and of ALMA observations, we analyse this systemat multiple wavelengths. We study the rings and spiral arms morphology and thescattering properties of the dust. We discuss the possible causes of all theobserved features.  Results. We detect for the first time, in the H${\alpha}$ band, a ringextending from $\sim$65 au to ${\sim}$120 au, inside the ring already knownfrom recent studies. These two have different physical and geometricalproperties. Based on the scattering properties, the outer ring may consist ofgrains of typical size $a_{out} > 4 {\mu}m$, while the inner ring of smallergrains ($a_{in} <= 0.4 {\mu m}$). Two extended logarithmic spiral arms stemfrom opposite sides of the disk. The outer ring appears as a spiral arm itself,with a variable radial distance from the centre and extended substructures.ALMA data confirm the presence of a millimetric dust substructure centred justoutside the outer ring, and detect misaligned gas rotation patterns for HD34700 A and B.  Conclusions. The complexity of HD 34700 A, revealed by the variety ofobserved features, suggests the existence of one or more disk-shaping physicalmechanisms. Possible scenarios, compatible with our findings, involve thepresence inside the disk of a yet undetected planet of several Jupiter massesand the system interaction with the surroundings by means of gas cloudletcapture or flybys. Further observations with JWST/MIRI or ALMA (gas kinematics)could shed more light on these.

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring