Poster Open Access

Probing the magnetospheric accretion region of the young system DoAr 44 using VLTI/GRAVITY

Bouvier Jerome; Perraut Karine; Alecian Evelyne

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<identifier identifierType="DOI">10.5281/zenodo.4563911</identifier>
<creators>
<creator>
<creatorName>Bouvier Jerome</creatorName>
<affiliation>IPAG</affiliation>
</creator>
<creator>
<creatorName>Perraut Karine</creatorName>
<affiliation>IPAG</affiliation>
</creator>
<creator>
<creatorName>Alecian Evelyne</creatorName>
<affiliation>IPAG</affiliation>
</creator>
</creators>
<titles>
<title>Probing the magnetospheric accretion region of the young system DoAr 44 using VLTI/GRAVITY</title>
</titles>
<publisher>Zenodo</publisher>
<publicationYear>2021</publicationYear>
<subjects>
<subject>Young stars</subject>
</subjects>
<contributors>
<contributor contributorType="Editor">
<contributorName>Wolk, Scott</contributorName>
<givenName>Scott</givenName>
<familyName>Wolk</familyName>
</contributor>
</contributors>
<dates>
<date dateType="Issued">2021-02-26</date>
</dates>
<resourceType resourceTypeGeneral="Text">Poster</resourceType>
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<alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/4563911</alternateIdentifier>
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<relatedIdentifiers>
<relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4563910</relatedIdentifier>
<relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/coolstars20half</relatedIdentifier>
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<rightsList>
<rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
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<descriptions>
<description descriptionType="Abstract">&lt;p&gt;Young stars accrete material from their circumstellar disk through magnetically-controlled funnel flows. This so-called magnetospheric accretion process is central to the properties of young systems and not yet fully deciphered. We report here on an attempt to directly probe the star-disk interaction region a scale of less than 0.1 au in the young system DoAr 44, using with VLTI/GRAVITY in the K-band. We computed interferometric visibilities and phases in the continuum and in the Br$\gamma$ line in order to constrain the extent and geometry of the emitting regions. We resolve the continuum emission of the inner dusty disk and measure a half-flux radius of 0.14 au. We show that Br$\gamma$ emission arises from an even more compact region than the inner disk, with an upper limit of 0.047 au (&amp;sim;5 R$_\star$). Differential phase measurements between the Br$\gamma$ line and the continuum allow us to measure the astrometric displacement of the Br$\gamma$ line-emitting region relative to the continuum on a scale of a few tens of microarcsec, corresponding to a fraction of the stellar radius. Our results can be accounted for by a simple geometric model where the Br$\gamma$ line emission arises from a compact region interior to the inner disk edge, on a scale of a few stellar radii, fully consistent with the concept of magnetospheric accretion process in low-mass young stellar systems.&lt;/p&gt;</description>
</descriptions>
<fundingReferences>
<fundingReference>
<funderName>European Commission</funderName>
<funderIdentifier funderIdentifierType="Crossref Funder ID">10.13039/100010661</funderIdentifier>
<awardNumber awardURI="info:eu-repo/grantAgreement/EC/H2020/742095/">742095</awardNumber>
<awardTitle>Star-Planet-Inner Disk Interactions (SPIDI): unveiling the formation and evolution of inner planetary systems</awardTitle>
</fundingReference>
</fundingReferences>
</resource>

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