example

<p class="block">
          <span class="image right">
            <img src="images/eso1325a.jpg" alt="ALMA (ESO/NAOJ/NRAO)/Nienke van der Marel">
            <small class="text-muted">Credit: ESO/L. Calçada</small>
          </span> Recent surveys have shown an overwhelming diversity of extrasolar planetary
          systems, prompting the question of how did they form, and whether some may end up looking
          like our own and being able to sustain
          life. Hints to answer such fundamental questions may be hidden in the many trends that
          are slowly emerging from the data. An example are the deserts and peaks in the
          distribution of giant exoplanets, with clear implications for habitability
          of systems, given the role played by giants on the delivery of volatiles to terrestrial
          planets (e.g., Quintana & Lissauer 2014). The environment in which planets form plays a
          major role in understanding both the variety of exoplanets
          and the emerging trends. Planets are born out of the dust and gas left over whenever a
          new star forms: the protoplanetary disk. The initial conditions for planet formation are
          thus determined by the protoplanetary disks, which evolve
          and disperse as they give birth to planets.
        </p>
        <p class="block">
          <span class="image left">
            <img src="images/eso1325d.jpg" alt="ALMA (ESO/NAOJ/NRAO)/Nienke van der Marel">
            <small class="text-muted">ALMA (ESO/NAOJ/NRAO)/Nienke van der Marel</small>
          </span>TDs are only now really becoming spatially resolvable thanks to facilities like
          ALMA and VLT - SPHERE, making their study a timely and urgent task. Only understanding
          the disk evolution and the planet-disk
          interactions allow the large body of existing and planned observations to be exploited to
          answer more complex questions like the formation of planetary systems capable to host
          life. This requires a focussed effort from several communities
          to devise a multi-pronged strategy to approach to tackle the problem. Specifically,
          multiwavelength observations of disks at different stages of evolution together with
          exoplanet and disk statistics should be used to constrain a concerted
          theoretical modelling effort including the hydrodynamics of the dust and gas component of
          disks, with and without planets, joint to chemical and radiative transfer calculations,
          particularly of the surface layers and winds of disks
          in (or just before) the transition phase. This is the motivation for the Research Unit.
        </p>
        <p>
          <a class="btn btn-sm btn-primary" target="_blank" href="https://github.com/RU-TD/2018-2nd_full_meeting/raw/master/Project-A1-Sanchis.pdf">[Internal]
            Full Meeting Project Slides</a>
        </p>