Journal article Open Access

The Pre-Main-Sequence Eclipsing Binary TY Coronae Australis: Precise Stellar Dimensions and Tests of Evolutionary Models

Casey, Brian W.; Mathieu, Robert D.; Vaz, Luiz Paulo R.; Andersen, Johannes; Suntzeff, and Nicholas B.

DataCite XML Export

<?xml version='1.0' encoding='utf-8'?>
<resource xmlns:xsi="" xmlns="" xsi:schemaLocation="">
  <identifier identifierType="URL"></identifier>
      <creatorName>Casey, Brian W.</creatorName>
      <givenName>Brian W.</givenName>
      <creatorName>Mathieu, Robert D.</creatorName>
      <givenName>Robert D.</givenName>
      <creatorName>Vaz, Luiz Paulo R.</creatorName>
      <givenName>Luiz Paulo R.</givenName>
      <creatorName>Andersen, Johannes</creatorName>
      <creatorName>Suntzeff, and Nicholas B.</creatorName>
      <givenName>and Nicholas B.</givenName>
    <title>The Pre-Main-Sequence Eclipsing Binary TY Coronae Australis: Precise Stellar Dimensions and Tests of Evolutionary Models</title>
    <date dateType="Issued">2007-12-18</date>
  <resourceType resourceTypeGeneral="Text">Journal article</resourceType>
    <alternateIdentifier alternateIdentifierType="url"></alternateIdentifier>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsIdenticalTo">10.1086/300270</relatedIdentifier>
    <rights rightsURI="">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
    <description descriptionType="Abstract">We analyze new photometric data for the Herbig Be eclipsing binary TY CrA, which securely reveal the secondary eclipse, ~0.03 mag deep in y. From the light-curve solution and our previous spectroscopic data, absolute dimensions of the primary and secondary stars are derived. The masses are found to be M1 = 3.16 ± 0.02 M☉ and M2 = 1.64 ± 0.01 M☉, the radii are R1 = 1.80 ± 0.10 R☉ and R2 = 2.08 ± 0.14 R☉, the luminosities are L1 = 67 ± 12 L☉ and L2 = 2.4 ± 0.8 L☉, and the effective temperatures are T1 = 12,000 ± 500 K and T2 = 4900 ± 400 K. Here the uncertainties represent high-confidence limits, not standard deviations. The secondary star is a pre–main-sequence star located at the base of the Hayashi tracks. As such, it is the least evolved star with a dynamically measured mass. Given higher effective temperatures for the primary (e.g., 12,500 K), the solar-composition 1.64 M☉ evolutionary tracks of Swenson et al., Claret, and D'Antona &amp;amp; Mazzitelli are all consistent with the properties of the TY CrA secondary and suggest an age of order 3 Myr. The radius and projected rotational velocity of the secondary star are consistent with synchronous rotation. The primary star is located near the zero-age main sequence, which, for solar compositions, is consistent with an age of 3 Myr. However, the primary star is not well represented by any of the 3.16 M☉ evolutionary models, which predict somewhat higher effective temperatures than observed.</description>
Views 55
Downloads 22
Data volume 19.1 MB
Unique views 55
Unique downloads 22


Cite as