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Episodic accretion in focus: revealing the environment of FU Orionis-type stars

Published online by Cambridge University Press:  13 January 2020

O. Fehér
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, 1121 Budapest, Konkoly Thege Miklós út, 15–17, Hungary Institut de Radioastronomie Millimétrique, 38400, Saint-Martin-d’Hères, 300 Rue de la Piscine, Grenoble, France
Á. Kóspál
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, 1121 Budapest, Konkoly Thege Miklós út, 15–17, Hungary Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
P. Ábrahám
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, 1121 Budapest, Konkoly Thege Miklós út, 15–17, Hungary
M. R. Hogerheijde
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands
Ch. Brinch
Affiliation:
Niels Bohr International Academy, The Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen Ø, Denmark
D. Semenov
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany

Abstract

The earliest phases of star formation are characterised by intense mass accretion from the circumstellar disk to the central star. One group of young stellar objects, the FU Orionis-type stars exhibit accretion rate peaks accompanied by bright eruptions. The occurance of these outbursts might solve the luminosity problem of protostars, play a key role in accumulating the final star mass, and have a significant effect on the parameters of the envelope and the disk. In the framework of the Structured Accretion Disks ERC project, we are conducting a systematic investigation of these sources with millimeter interferometry to examine whether they represent normal young stars in exceptional times or they are unusual objects. Our results show that FU Orionis-type stars can be similar to both Class I and Class II systems and may be in a special evolutionary phase between the two classes with their infall-driven episodic eruptions being the main driving force of the transition.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020 

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