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dc.contributor.authorGalván-Madrid, Roberto
dc.contributor.authorLiu, Hauyu Baobab
dc.contributor.authorManara, Carlo Felice
dc.contributor.authorForbrich, Jan
dc.contributor.authorPascucci, Ilaria
dc.contributor.authorCarrasco-González, Carlos
dc.contributor.authorGoddi, Ciriaco
dc.contributor.authorHasegawa, Yasuhiro
dc.contributor.authorTakami, Michihiro
dc.contributor.authorTesti, Leonardo
dc.date.accessioned2017-07-20T16:10:10Z
dc.date.available2017-07-20T16:10:10Z
dc.date.issued2014-10-21
dc.identifier.citationGalván-Madrid , R , Liu , H B , Manara , C F , Forbrich , J , Pascucci , I , Carrasco-González , C , Goddi , C , Hasegawa , Y , Takami , M & Testi , L 2014 , ' Constraints on photoevaporation models from (lack of) radio emission in the Corona Australis protoplanetary disks ' Astronomy & Astrophysics , vol. 570 , L9 . https://doi.org/10.1051/0004-6361/201424630
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 11212747
dc.identifier.otherPURE UUID: aae7c30f-c7a2-47d9-9b1c-9f04f7e94b57
dc.identifier.otherArXiv: http://arxiv.org/abs/1409.7110v1
dc.identifier.otherScopus: 84908402868
dc.identifier.urihttp://hdl.handle.net/2299/19031
dc.descriptionR. Galván-Madrid, et al., “Constraints on photoevaporation models from (lack of) radio emission in the Corona Australis protoplanetary disks”, Astronomy & Astrophysics, Vol. 570, October 2014. This version of record is available online at: https://doi.org/10.1051/0004-6361/201424630 Reproduced with Permission from Astronomy and Astrophysics, © ESO 2014.
dc.description.abstractPhotoevaporation due to high-energy stellar photons is thought to be one of the main drivers of protoplanetary disk dispersal. The fully or partially ionized disk surface is expected to produce free-free continuum emission at centimeter (cm) wavelengths that can be routinely detected with interferometers such as the upgraded Very Large Array (VLA). We use deep (rms noise down to 8 $\mu$Jy beam$^{-1}$ in the field of view center) 3.5 cm maps of the nearby (130 pc) Corona Australis (CrA) star formation (SF) region to constrain disk photoevaporation models. We find that the radio emission from disk sources in CrA is surprisingly faint. Only 3 out of 10 sources within the field of view are detected, with flux densities of order $10^2$ $\mu$Jy. However, a significant fraction of their emission is non-thermal. Typical upper limits for non-detections are $3\sigma\sim 60~\mu$Jy beam$^{-1}$. Assuming analytic expressions for the free-free emission from extreme-UV (EUV) irradiation, we derive stringent upper limits to the ionizing photon luminosity impinging on the disk surface $\Phi_\mathrm{EUV}en
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectastro-ph.GA
dc.subjectastro-ph.EP
dc.subjectastro-ph.SR
dc.titleConstraints on photoevaporation models from (lack of) radio emission in the Corona Australis protoplanetary disksen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201424630
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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