Presentation Open Access

How planets affect cool stars

Poppenhaeger, Katja

DataCite XML Export

<?xml version='1.0' encoding='utf-8'?>
<resource xmlns:xsi="" xmlns="" xsi:schemaLocation="">
  <identifier identifierType="DOI">10.5281/zenodo.1460576</identifier>
      <creatorName>Poppenhaeger, Katja</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0003-1231-2194</nameIdentifier>
      <affiliation>Leibniz Institute for Astrophysics Potsdam; Queen's University Belfast</affiliation>
    <title>How planets affect cool stars</title>
    <date dateType="Issued">2018-10-12</date>
  <resourceType resourceTypeGeneral="Text">Presentation</resourceType>
    <alternateIdentifier alternateIdentifierType="url"></alternateIdentifier>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.1460575</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf"></relatedIdentifier>
    <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;All cool stars display magnetic phenomena including flares, spots, and coronal high-energy emission, collectively called magnetic activity. Cool stars also spin down over time by shedding a magnetized wind which couples to the stellar magnetic field; these magnetic effects therefore fade over timescales of gigayears. Cool stars with exoplanets in close orbits may be a fundamental exception from the age-activity-rotation relationships which govern other cool stars. In analogy to close stellar binaries, a planet and its star are thought to interact tidally and magnetically. If the planetary orbit is shorter than the stellar rotation period, angular momentum transfer from the orbit to the stellar spin can take place. This can lead to a spin-up (or inhibited spin-down) of the host stars and a shrinking planetary orbit. In addition to this long-term evolution, planets have also been speculated to trigger stellar flares or other changes in the stellar atmosphere through magnetic interaction or accretion of evaporating exoplanetary material. Observational searches for such enhanced rotation or activity of Hot-Jupiter host stars are not straightforward due to the presence of selection effects and the stochastic nature of stellar activity itself; however, there has been progress over the past years which I will report on. I will also highlight the influence these effects can have on exoplanets themselves.&lt;/p&gt;</description>
    <description descriptionType="Other">{"references": ["Mathis, S. and Remus, F. (2013), DOI 10.1007/978-3-642-30648-8_4", "Lanza, A. and Mathis, S. (2016), arXiv:1606.08623", "Jackson, B. et al. (2009), arXiv:0904.1170", "Penev, K. et al. (2012), arXiv:1205.1803", "Shkolnik, E. (2013), arXiv:1301.6192", "Miller, B. et al. (2015), arXiv:1411.3348", "Hebb, L. et al (2010), arXiv:1001.0403", "Penev, K. et al. (2016), arXiv:1606.00848", "Kashyap, V. (2008), arXiv:0807.1308", "Poppenhaeger, K. and Wolk, S. (2014), arXiv:1404.1073", "Rogers, T. and McElwaine, J. (2017), arXiv:1704.04197", "Yadav, R. and Thorngren, D. (2017), arXiv:1709.05676", "Shkolnik, E. et al. (2005), arXiv:astro-ph/0411655", "Shkolnik, E. et al. (2008), arXiv:0712.0004", "Miller, B. et al. (2012), arXiv:1206.0746", "Pillitteri, I. et al. (2014), arXiv:1406.2620", "Poppenhaeger, K. et al. (2011), arXiv:1010.5632", "Pillitteri, I. et al. (2015), arXiv:1503.05590", "Bourrier, V. et al. (2018), arXiv:1803.10783", "Matsakos, T. et al. (2015), arXiv:1503.03551", "Strugarek, A. et al. (2014), arXiv:1409.5268", "Lanza, A. (2013), arXiv:1307.2341", "Scandariato, G. et al. (2013), arXiv:1301.7748", "Getman, K. et al. (2011), arXiv:1101.4044", "Getman, K. et al. (2016), arXiv:1609.04773", "Maggio, A. et al. (2015), arXiv:1509.00662", "Kulow, J. et al. (2014), arXiv:1403.6834", "Ehrenreich, D. et al. (2015), arXiv:1506.07541", "Poppenhaeger, K. et al. (2013), arXiv:1306.2311", "Murray-Clay, R. et al. (2009), arXiv:0811.0006", "Lecavelier des Etangs, A. et al. (2004), arXiv:astro-ph/0403369", "Lopez, E. and Fortney, J. (2013), arXiv:1305.0269", "Sanz-Forcada, J. et al. (2011), arXiv:1105.0550", "Booth, R. et al. (2017), arXiv:1706.08979"]}</description>
All versions This version
Views 8484
Downloads 5858
Data volume 245.7 MB245.7 MB
Unique views 8383
Unique downloads 5353


Cite as