Poster Open Access

Relation of Observable Stellar Parameters to Mass-Loss Rate of AGB Stars in the LMC

Prager, Henry; Willson, Lee Anne; Marengo, Massimo; Creech-Eakman, Michelle

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  <identifier identifierType="DOI">10.5281/zenodo.4567529</identifier>
      <creatorName>Prager, Henry</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0002-0658-6175</nameIdentifier>
      <affiliation>New Mexico Tech</affiliation>
      <creatorName>Willson, Lee Anne</creatorName>
      <givenName>Lee Anne</givenName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0001-7921-8739</nameIdentifier>
      <affiliation>Iowa State University</affiliation>
      <creatorName>Marengo, Massimo</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0001-9910-9230</nameIdentifier>
      <affiliation>Iowa State University</affiliation>
      <creatorName>Creech-Eakman, Michelle</creatorName>
      <affiliation>New Mexico Tech</affiliation>
    <title>Relation of Observable Stellar Parameters to Mass-Loss Rate of AGB Stars in the LMC</title>
    <subject>Post main sequence cool stars</subject>
    <subject>mass loss</subject>
    <date dateType="Issued">2021-02-26</date>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
    <alternateIdentifier alternateIdentifierType="url"></alternateIdentifier>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4567528</relatedIdentifier>
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    <rights rightsURI="">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
    <description descriptionType="Abstract">&lt;p&gt;Mass loss in Asymptotic Giant Branch (AGB) stars has historically proven difficult to characterize accurately.&lt;br&gt;
This is due to a multitude of factors such as differing composition--including chemistry, metallicity, and differences in carbon and oxygen ratios--and differences in their ongoing motion--particularly, differing pulsation modes.&amp;nbsp;&lt;br&gt;
In mass-loss formulations, the mass-loss rate depends on some combinations of stellar parameters, including but not limited to pulsation period, mass, and luminosity.&lt;/p&gt;

&lt;p&gt;Using a combination of stellar models and archival data, we have been working at improving the relation between these parameters and the mass-loss rate of the stars. We have used the models and data to improve on the period-mass-luminosity and radius-mass-luminosity relations for M and C stars in both the fundamental and overtone pulsation modes. Current work is focused on accounting for any remaining sources of scatter in the relation between $\dot{M}$ and our parameters $P$, $L$, and $M$.&lt;/p&gt;</description>
    <description descriptionType="Other">{"references": ["Riebel et al. (2012). THE MASS-LOSS RETURN FROM EVOLVED STARS TO THE LARGE MAGELLANIC CLOUD. VI. LUMINOSITIES AND MASS-LOSS RATES ON POPULATION SCALES.", "Trabucchi et al. (2018). Modelling long-period variables \u2013 I. A new grid of O-rich and C-rich pulsation models.", "Willson (2000). MASS LOSS FROM COOL STARS: Impact on the Evolution of Stars and Stellar Populations.", "Willson (2009). Big, Cool, and Losing Mass: Dependence of Mass Loss Rates on L, R, M and Z.", "Willson and Marengo (2012). Miras.", "Harris, C.R., Millman, K.J., van der Walt, S.J. et al. (2020). Array programming with NumPy.", "Virtanen et al. (2020). SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python.", "Hunter, J.D. (2007). Matplotlib: A 2D graphics environment."]}</description>
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