February 26, 2021 Poster Open Access

Boudreaux, Thomas M.; Newton, Elisabeth R.; Mondrik, Nicholas; Charbonneau, David; Irwin, Jonathan

MARC21 XML Export

<?xml version='1.0' encoding='UTF-8'?>
<record xmlns="http://www.loc.gov/MARC21/slim">
  <leader>00000nam##2200000uu#4500</leader>
  <datafield tag="999" ind1="C" ind2="5">
    <subfield code="x">Chabrier, G., &amp; Baraffe, I. 1997, A&amp;A, 327, 1039, Astudillo-Defru, N., Delfosse, X., Bonfils, X., et al. 2017, A&amp;A, 600, A13, Wright, N. J., Newton, E. R., Williams, P. K. G., Drake, J. J., &amp; Yadav, R. K. 2018, MNRAS, 479, 2351, Salvatier, J., Wiecki, T. V., &amp; Fonnesbeck, C. 2016, PeerJComputer Science, 2, e55</subfield>
  </datafield>
  <datafield tag="653" ind1=" " ind2=" ">
    <subfield code="a">Cool Stars on the main sequence</subfield>
  </datafield>
  <controlfield tag="005">20210227002714.0</controlfield>
  <controlfield tag="001">4564535</controlfield>
  <datafield tag="711" ind1=" " ind2=" ">
    <subfield code="d">March 2-4, 2021</subfield>
    <subfield code="g">CS20.5</subfield>
    <subfield code="a">The 20.5th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun</subfield>
    <subfield code="c">virtually anywhere</subfield>
  </datafield>
  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="u">Dartmouth College Department of Physics and Astronomy &amp; MIT Kavli Institute</subfield>
    <subfield code="a">Newton, Elisabeth R.</subfield>
  </datafield>
  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="u">Harvard University, Department of Physics &amp; Center for Astrophysics | Harvard &amp; Smithsonian</subfield>
    <subfield code="a">Mondrik, Nicholas</subfield>
  </datafield>
  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="u">Harvard University, Department of Physics &amp; Center for Astrophysics | Harvard &amp; Smithsonian</subfield>
    <subfield code="a">Charbonneau, David</subfield>
  </datafield>
  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="u">Center for Astrophysics | Harvard &amp; Smithsonian</subfield>
    <subfield code="a">Irwin, Jonathan</subfield>
  </datafield>
  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="4">edt</subfield>
    <subfield code="a">Wolk, Scott</subfield>
  </datafield>
  <datafield tag="856" ind1="4" ind2=" ">
    <subfield code="s">533715</subfield>
    <subfield code="z">md5:76160a7ea749bcfc2ce06e5058c2e2e4</subfield>
    <subfield code="u">https://zenodo.org/record/4564535/files/Poster.pdf</subfield>
  </datafield>
  <datafield tag="542" ind1=" " ind2=" ">
    <subfield code="l">open</subfield>
  </datafield>
  <datafield tag="856" ind1="4" ind2=" ">
    <subfield code="y">Conference website</subfield>
    <subfield code="u">http://coolstars20.cfa.harvard.edu/cs20half/</subfield>
  </datafield>
  <datafield tag="260" ind1=" " ind2=" ">
    <subfield code="c">2021-02-26</subfield>
  </datafield>
  <datafield tag="909" ind1="C" ind2="O">
    <subfield code="p">openaire</subfield>
    <subfield code="p">user-coolstars20half</subfield>
    <subfield code="o">oai:zenodo.org:4564535</subfield>
  </datafield>
  <datafield tag="100" ind1=" " ind2=" ">
    <subfield code="u">Dartmouth College, Department of Physics and Astronomy</subfield>
    <subfield code="a">Boudreaux, Thomas M.</subfield>
  </datafield>
  <datafield tag="245" ind1=" " ind2=" ">
    <subfield code="a">The Ca II H&amp;K Rotation-Activity Relation in 50 Mid-to-Late Type M-Dwarfs</subfield>
  </datafield>
  <datafield tag="980" ind1=" " ind2=" ">
    <subfield code="a">user-coolstars20half</subfield>
  </datafield>
  <datafield tag="540" ind1=" " ind2=" ">
    <subfield code="u">https://creativecommons.org/licenses/by/4.0/legalcode</subfield>
    <subfield code="a">Creative Commons Attribution 4.0 International</subfield>
  </datafield>
  <datafield tag="650" ind1="1" ind2="7">
    <subfield code="a">cc-by</subfield>
    <subfield code="2">opendefinition.org</subfield>
  </datafield>
  <datafield tag="520" ind1=" " ind2=" ">
    <subfield code="a">&lt;p&gt;In the canonical formulation of stellar magnetic dynamo theory, the tachocline in partially convective stars serves to arrange small scale randomly oriented fields, which are generated by stochastic movement of plasma, into a large scale coherent field. Mid-to-late M-dwarfs show more magnetic activity than classical magnetic dymano theory predicts. This leads to the open question: what mechanism generates and maintains these fields in fully convective stars? Mid-to-late M-dwarfs show tight correlations between rotation rates and magnetic activity, consistent with elements of classical dynamo theory. We use data from Magellan Inamori Kyocera Echelle (MIKE) Spectrograph to measure&amp;nbsp;R&amp;#39;HK&amp;nbsp;values for 50 spectroscopically identified M-dwarfs selected from the MEarth survey. These stars span spectral classes from M5.0 to M3.5 and have rotation periods ranging from hours to months. Here, we present the rotation&amp;ndash;activity relationship as traced through these data. We find power law and saturated regimes consistent to within one sigma of previously published results, and find the saturated value to be mass-dependent.&lt;/p&gt;</subfield>
  </datafield>
  <datafield tag="773" ind1=" " ind2=" ">
    <subfield code="n">doi</subfield>
    <subfield code="i">isVersionOf</subfield>
    <subfield code="a">10.5281/zenodo.4564534</subfield>
  </datafield>
  <datafield tag="024" ind1=" " ind2=" ">
    <subfield code="a">10.5281/zenodo.4564535</subfield>
    <subfield code="2">doi</subfield>
  </datafield>
  <datafield tag="980" ind1=" " ind2=" ">
    <subfield code="a">poster</subfield>
  </datafield>
</record>