Poster Open Access

# Understanding stars close to the gap

Wei-Chun Jao; Todd Henry; Elliott Horch; Eliot Vrijmoet; Gemini Speckle Team

### DataCite XML Export

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<identifier identifierType="DOI">10.5281/zenodo.4560526</identifier>
<creators>
<creator>
<creatorName>Wei-Chun Jao</creatorName>
<nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0003-0193-2187</nameIdentifier>
<affiliation>Georgia State University</affiliation>
</creator>
<creator>
<creatorName>Todd Henry</creatorName>
<affiliation>Georgia State University</affiliation>
</creator>
<creator>
<creatorName>Elliott Horch</creatorName>
<affiliation>Southern Connecticut State University</affiliation>
</creator>
<creator>
<creatorName>Eliot Vrijmoet</creatorName>
<affiliation>Georgia State University</affiliation>
</creator>
<creator>
<creatorName>Gemini Speckle Team</creatorName>
</creator>
</creators>
<titles>
<title>Understanding stars close to the gap</title>
</titles>
<publisher>Zenodo</publisher>
<publicationYear>2021</publicationYear>
<subjects>
<subject>Cool Stars On The Main Sequence</subject>
<subject>speckle</subject>
<subject>Gaia</subject>
<subject>TESS</subject>
<subject>Low Mass Stars</subject>
</subjects>
<dates>
<date dateType="Issued">2021-02-24</date>
</dates>
<resourceType resourceTypeGeneral="Text">Poster</resourceType>
<alternateIdentifiers>
<alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/4560526</alternateIdentifier>
</alternateIdentifiers>
<relatedIdentifiers>
<relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4560525</relatedIdentifier>
<relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/coolstars20half</relatedIdentifier>
</relatedIdentifiers>
<version>1</version>
<rightsList>
<rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
</rightsList>
<descriptions>
<description descriptionType="Abstract">&lt;p&gt;Theoretical models show the main sequence gap is a result of the mixing of 3He during the merger of envelope and core convection zones. Unlike stars the either side of the gap, stars in a narrow mass range will go through instability phases, where their dynamos could switch between the &amp;alpha;&amp;Omega; dynamo like the Sun and &amp;Omega;2 dynamo like late M dwarfs. At the same time, they show radial pulsation and their fluxes fluctuate, which resemble the pulsations observed in evolved stars like red giants and asymptotic giant branch stars. Consequently, they are a unique type of dwarf like no other on the main sequence. In this work, we would like to know 1) will the unstable interior structures result in observable characteristics such as flaring and spots, and 2) what is the mass range for these stars observationally? Here we present our preliminary results: 1) stars in the gap have higher percentage rate of activities than their adjacent regions, and 2) high resolution speckle results yield promising close binaries to&amp;nbsp; yield dynamical masses in the future.&lt;/p&gt;</description>
</descriptions>
</resource>

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