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    <subfield code="a">10.1007/s11214-025-01177-3</subfield>
    <subfield code="2">DOI</subfield>
  </datafield>
  <datafield tag="037" ind1=" " ind2=" ">
    <subfield code="a">SCART-2025-0138</subfield>
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  <datafield tag="100" ind1=" " ind2=" ">
    <subfield code="a">Harra, L.</subfield>
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  <datafield tag="245" ind1=" " ind2=" ">
    <subfield code="a">The Dynamics of the Extreme Ultraviolet Quiet Sun and Coronal Holes in the Solar Orbiter Era</subfield>
  </datafield>
  <datafield tag="260" ind1=" " ind2=" ">
    <subfield code="c">2025</subfield>
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  <datafield tag="520" ind1=" " ind2=" ">
    <subfield code="a">The quiet Sun corona and coronal holes, as seen in the extreme ultraviolet (EUV), host a variety of phenomena that operate over a range of spatial and temporal scales. Dynamic brightenings and jets of at most a few megameters appear to evolve on minute timescales. Coronal structures larger than tens of Mm evolve on much longer, hour timescales. Un- derstanding the characteristics of the quiet Sun corona and coronal holes along with their disparate phenomena will provide important constraints on models that aim to explain how the plasma is heated and how it further expands to form the solar wind. In 2020, the Euro- pean Space Agency (ESA) Solar Orbiter mission was launched. It features a comprehensive remote-sensing package, which includes two instruments observing in the Extreme Ultravi- olet (EUV) and UV spectrometer data: the Extreme Ultraviolet Imager (EUI) that provides high resolution Extreme Ultraviolet (EUV) images at 174 Å (HRIEUV), and the Spectral Imaging of the Coronal Environment (SPICE) spectrometer that enables plasma diagnos- tics, and the Polarimetric and Helioseismic Imager (PHI) that measures the photospheric magnetic field. These data, alongside a fleet of instruments on the Solar Dynamics Observa- tory (SDO), Hinode and the Interface Region Imaging Spectrograph (IRIS), are providing new information on the behaviour and dynamics of the quiet Sun and coronal holes. We will review the latest results and put them in context of describing the physics of coronal heating and solar wind formation.</subfield>
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  <datafield tag="594" ind1=" " ind2=" ">
    <subfield code="a">STCE</subfield>
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  <datafield tag="653" ind1="1" ind2=" ">
    <subfield code="a">Solar Orbiter</subfield>
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  <datafield tag="653" ind1="1" ind2=" ">
    <subfield code="a">Quiet Sun</subfield>
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  <datafield tag="653" ind1="1" ind2=" ">
    <subfield code="a">Extreme Ultraviolet</subfield>
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  <datafield tag="653" ind1="1" ind2=" ">
    <subfield code="a">Coronal heating</subfield>
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  <datafield tag="653" ind1="1" ind2=" ">
    <subfield code="a">Solar Wind</subfield>
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  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="a">Barczynski, K.</subfield>
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  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="a">Auchère, F.</subfield>
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  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="a">Berghmans, D.</subfield>
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  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="a">Chitta, L. P.</subfield>
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  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="a">Parenti, S.</subfield>
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  <datafield tag="700" ind1=" " ind2=" ">
    <subfield code="a">Peter, H.</subfield>
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  <datafield tag="773" ind1=" " ind2=" ">
    <subfield code="p">Space Science Reviews</subfield>
    <subfield code="v">221 </subfield>
    <subfield code="y">2025</subfield>
    <subfield code="c">article number 50</subfield>
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  <datafield tag="856" ind1="0" ind2=" ">
    <subfield code="f">david.berghmans@ksb-orb.be</subfield>
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  <datafield tag="856" ind1="4" ind2="2">
    <subfield code="a">https://link.springer.com/article/10.1007/s11214-025-01177-3?utm_source=rct_congratemailt&amp;utm_medium=email&amp;utm_campaign=oa_20250605&amp;utm_content=10.1007/s11214-025-01177-3</subfield>
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    <subfield code="a">published in</subfield>
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  <datafield tag="980" ind1=" " ind2=" ">
    <subfield code="a">REFERD</subfield>
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