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dc.contributor.authorPascucci, Ilaria
dc.contributor.authorTesti, L.
dc.contributor.authorHerczeg, Gregory J.
dc.contributor.authorLong, F.
dc.contributor.authorManara, C. F.
dc.contributor.authorHendler, N.
dc.contributor.authorMulders, Gijs D.
dc.contributor.authorKrijt, S.
dc.contributor.authorCiesla, F.
dc.contributor.authorHenning, Th.
dc.contributor.authorMohanty, S.
dc.contributor.authorDrabek-Maunder, E.
dc.contributor.authorApai, D.
dc.contributor.authorSzűcs, L.
dc.contributor.authorSacco, G.
dc.contributor.authorOlofsson, J.
dc.date.accessioned2017-01-25T22:01:12Z
dc.date.available2017-01-25T22:01:12Z
dc.date.issued2016-11-02
dc.identifier.citationA STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION 2016, 831 (2):125 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/0004-637X/831/2/125
dc.identifier.urihttp://hdl.handle.net/10150/622163
dc.description.abstractThe disk mass is among the most important input parameter for every planet formation model to determine the number and masses of the planets that can form. We present an ALMA 887 mu m survey of the disk population around objects from similar to 2 to 0.03 M-circle dot in the nearby similar to 2 Myr old Chamaeleon I star-forming region. We detect thermal dust emission from 66 out of 93 disks, spatially resolve 34 of them, and identify two disks with large dust cavities of about 45 au in radius. Assuming isothermal and optically thin emission, we convert the 887 mu m flux densities into dust disk masses, hereafter M-dust. We find that the M-dust-M* relation is steeper than linear and of the form M-dust proportional to (M*)(1.3-1.9), where the range in the power-law index reflects two extremes of the possible relation between the average dust temperature and stellar luminosity. By reanalyzing all millimeter data available for nearby regions in a self-consistent way, we show that the 1-3 Myr old regions of Taurus, Lupus, and Chamaeleon. I share the same M-dust-M* relation, while the 10 Myr old Upper. Sco association has a steeper relation. Theoretical models of grain growth, drift, and fragmentation reproduce this trend and suggest that disks are in the fragmentation-limited regime. In this regime millimeter grains will be located closer in around lower-mass stars, a prediction that can be tested with deeper and higher spatial resolution ALMA observations.
dc.description.sponsorshipNSF Astronomy & Astrophysics Research Grant [1515392]; National Science Foundation of China [11473005]; Italian Ministero dell'Istruzione, Universita e Ricerca through the grant Progetti Premiali -iALMA [CUP C52I13000140001]; Gothenburg Centre of Advanced Studies in Science and Technology through the program Origins of Habitable Planets; National Aeronautics and Space Administration [NNX15AD94G]; NASA's Science Mission Directorateen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/831/i=2/a=125?key=crossref.c1985cd9e48727176615fdab86de4c8den
dc.rights© 2016. The American Astronomical Society. All rights reserved.en
dc.subjectbrown dwarfsen
dc.subjectprotoplanetary disksen
dc.subjectstars: pre-main sequenceen
dc.subjectsubmillimeter: planetary systemsen
dc.titleA STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATIONen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-19T04:25:26Z
html.description.abstractThe disk mass is among the most important input parameter for every planet formation model to determine the number and masses of the planets that can form. We present an ALMA 887 mu m survey of the disk population around objects from similar to 2 to 0.03 M-circle dot in the nearby similar to 2 Myr old Chamaeleon I star-forming region. We detect thermal dust emission from 66 out of 93 disks, spatially resolve 34 of them, and identify two disks with large dust cavities of about 45 au in radius. Assuming isothermal and optically thin emission, we convert the 887 mu m flux densities into dust disk masses, hereafter M-dust. We find that the M-dust-M* relation is steeper than linear and of the form M-dust proportional to (M*)(1.3-1.9), where the range in the power-law index reflects two extremes of the possible relation between the average dust temperature and stellar luminosity. By reanalyzing all millimeter data available for nearby regions in a self-consistent way, we show that the 1-3 Myr old regions of Taurus, Lupus, and Chamaeleon. I share the same M-dust-M* relation, while the 10 Myr old Upper. Sco association has a steeper relation. Theoretical models of grain growth, drift, and fragmentation reproduce this trend and suggest that disks are in the fragmentation-limited regime. In this regime millimeter grains will be located closer in around lower-mass stars, a prediction that can be tested with deeper and higher spatial resolution ALMA observations.


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