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

One of the early hypotheses about the origin of FUOR outbursts explains themby the fall of gas clumps from the remnants of protostellar clouds ontoprotoplanetary disks surrounding young stars (Hartmann and Kenyon 1985). Tocalculate the consequences of such an event we make 3D hydrodynamic simulationsby SPH method. It is shown that the fall of the clump on the disk in thevicinity of the star actually causes a burst of the star's accretion activity,resembling in its characteristics the flares of known FUORs. In the region ofincidence, an inhomogeneous gas ring is formed, which is inclined relative tothe outer disk. During several revolutions around the star, this ring combineswith the inner disk and forms a tilted disk. In the process of evolution, theinner disk expands, and its inclination relative to the outer disk decreases.After 100 revolutions, the angle of inclination is a few degrees. This resultis of interest in connection with the discovery in recent years ofprotoplanetary disks, the inner region of which is inclined relative to theouter one. Such structures are usually associated with the existence in thevicinity of a star of a massive body (planet or brown dwarf), whose orbit isinclined relative to the plane of the disk. The results of our modelingindicate the possibility of an alternative explanation for this phenomenon.

3-D SPH simulations of the FUOR flares in the clumpy accretion model