Millimeter emission structure in the first alma image of the AU Mic debris disk

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DOIResolve DOI: http://doi.org/10.1088/2041-8205/762/2/L21
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TypeArticle
Journal titleThe Astrophysical Journal Letters
ISSN2041-8205
Volume762
Issue2
Article numberL21
AbstractWe present 1.3 mm ALMA Cycle 0 observations of the edge-on debris disk around the nearby, ∼10 Myr old, M-type star AU Mic. These observations obtain 0.″6 (6 AU) resolution and reveal two distinct emission components: (1) the previously known dust belt that extends to a radius of 40 AU and (2) a newly recognized central peak that remains unresolved. The cold dust belt of mass ∼1 MMoon is resolved in the radial direction with a rising emission profile that peaks sharply at the location of the outer edge of the "birth ring" of planetesimals hypothesized to explain the midplane scattered light gradients. No significant asymmetries are discerned in the structure or position of this dust belt. The central peak identified in the ALMA image is ∼6 times brighter than the stellar photosphere, which indicates an additional emission process in the inner regions of the system. Emission from a stellar corona or activity may contribute, but the observations show no signs of temporal variations characteristic of radio-wave flares. We suggest that this central component may be dominated by dust emission from an inner planetesimal belt of mass ∼0.01 MMoon, consistent with a lack of emission shortward of 25 μm and a location ≲3 AU from the star. Future millimeter observations can test this assertion, as an inner dust belt should be readily separated from the central star at higher angular resolution. © 2013. The American Astronomical Society. All rights reserved.
Publication date
LanguageEnglish
AffiliationNational Research Council Canada (NRC-CNRC); National Science Infrastructure
Peer reviewedYes
NPARC number21271783
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Record identifieree0d4c32-8831-41cd-b8ab-ca745d743f07
Record created2014-04-17
Record modified2016-05-09
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