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The Debris Disk Fraction for M-dwarfs in Nearby Young Moving Groups

Published online by Cambridge University Press:  27 January 2016

Alex Binks
Alex Binks*
Affiliation:
Keele University email: a.s.binks@keele.ac.uk
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Abstract

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I present the first substantial work to measure the fraction of debris disks for M-dwarfs in nearby moving groups (MGs). Utilising the AllWISE IR catalog, 17 out of 151 MG members are found with an IR photometric excess indicative of disk structure. The M-dwarf debris disk fraction is ≲6 per cent in MGs younger than 40 Myr, and none are found in the groups older than 40 Myr. Simulations show, however, that debris disks around M-dwarfs are not present above a WISEW1-W4 colour of ~2.5, making calculating the absolute disk fractions difficult. The debris disk dissipation timescale appears to be faster than for higher-mass stars, and mechanisms such as enhanced stellar wind drag and/or photoevaporation could account for the more rapid decline of disks observed amongst M-dwarfs.

Keywords

stars: late-typestars: low-massstars: pre-main sequenceprotoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 159 - 162
Copyright
Copyright © International Astronomical Union 2016 

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