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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 Open the ORCID record for O. Fehér [Opens in a new window] ,
Á. Kóspál ,
P. Ábrahám ,
M. R. Hogerheijde ,
Ch. Brinch  and
D. Semenov
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
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Abstract

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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.

Keywords

stars: pre–main-sequencemolecular datacircumstellar matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 87 - 90
Copyright
© International Astronomical Union 2020 

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