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Exploration of the molecular gas content of young debris disks

Published online by Cambridge University Press:  13 January 2020

A. Moór ,
Á. Kóspál ,
P. Ábrahám  and
N. Pawellek
A. Moór
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Konkoly-Thege Miklós út 15-17, Budapest, Hungary email: [email protected]
Á. Kóspál
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Konkoly-Thege Miklós út 15-17, Budapest, Hungary email: [email protected] Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
P. Ábrahám
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Konkoly-Thege Miklós út 15-17, Budapest, Hungary email: [email protected]
N. Pawellek
Affiliation:
Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Konkoly-Thege Miklós út 15-17, Budapest, Hungary email: [email protected] Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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Abstract

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Thanks especially to the ALMA interferometer, there are several new detections of CO gas in debris disks. Based on our own and archival ALMA observations, we found that the presence of CO gas in dust-rich debris disks around young (10–50 Myr) A-type stars is common. Interestingly, similarly dust-rich debris disks around young F-K type stars exhibit significantly lower gas incidence. The main difference between the two subsamples is related to a special population of gaseous debris disks whose total CO gas quantity is comparable to that of the less massive Herbig Ae disks. The origin of gas in these CO-rich debris systems is not fully clarified yet.

Keywords

(stars:) circumstellar matterradio lines: stars
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. 349 - 350
Copyright
© International Astronomical Union 2020 

References

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