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Free keywords:
stars: individual: HD 193571
planet-disk interactions
planets and
satellites: detection
infrared: planetary systems
instrumentation:
high angular resolution
techniques: high angular resolution
Astrophysics - Earth and Planetary Astrophysics
Astrophysics - Solar
and Stellar Astrophysics
Abstract:
Context. The interaction between low-mass companions and the debris discs they reside in is still not fully understood. A debris disc can evolve due to self-stirring, a process in which planetesimals can excite their neighbours to the point of destructive collisions. In addition, the presence of a companion could further stir the disc (companion- stirring). Additional information is necessary to understand this fundamental step in the formation and evolution of a planetary system, and at the moment of writing only a handful of systems are known where a companion and a debris disc have both been detected and studied at the same time.
Aims: Our primary goal is to augment the sample of these systems and to understand the relative importance between self- stirring and companion-stirring.
Methods: In the course of the VLT/NaCo Imaging Survey for Planets around Young stars (ISPY), we observed HD 193571, an A0 debris disc hosting star at a distance of 68 pc with an age between ̃60 and 170 Myr. We obtained two sets of observations in L' band and a third epoch in H band using the GPI instrument at Gemini-South.
Results: A companion was detected in all three epochs at a projected separation of ̃11 au (̃0.17″), and co- motion was confirmed through proper motion analysis. Given the inferred disc size of 120 au, the companion appears to reside within the gap between the host star and the disc. Comparison between the L' and H band magnitude and evolutionary tracks suggests a mass of ̃0.31 - 0.39 M☉.
Conclusions: We discovered a previously unknown M-dwarf companion around HD 193571, making it the third low-mass stellar object discovered within a debris disc. A comparison to self- and companion-stirring models suggests that the companion is likely responsible for the stirring of the disc. The reduced images are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/A77">http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/A77</A>ESO program IDs 097.C-0206 and 1101.C-0092.
