Proxauf, B.; Gizon, L.; Löptien, B.; Birch, A.; Schou, J.; Bogart, R. S.: On the depth dependence of solar equatorial Rossby waves. XXXth General Assembly of the International Astronomical Union, Vienna, Austria (2018)
Nagashima, K.; Duvall, T.; Birch, A. C.; Gizon, L.: Comparison between time-distance and ring-diagram helioseismology measurements of subsurface convective flows. Annual Meeting of the Astronomische Gesellschaft 2017, Göttingen, Germany (2017)
Ferret, R. Z.; Gizon, L.; Birch, A.; Cameron, R.: New insights on supergranular depth obtained through the resolution of the forward problem in local helioseismology. Astronomische Gesellschaft Meeting, Göttingen, Germany (2017)
Poulier, P.-L.; Gizon, L.; Duvall, T.; Fournier, D.: Multiple scattering of acoustic waves. AG2017 The many Scales of Universe: Galaxies, theirs Suns and their Planets, Göttingen, Germany (2017)
Pourabdian, M.; Fournier, D.; Gizon, L.: Comparison Between Travel-time and Amplitude Measurements Using Deep-focusing Time-distance Helioseismology. AG Meeting 2017, Göttingen, Germany (2017)
Yang, D.; Gizon, L.; Fournier, D.: A Possible Improvement on Helioseismic Holography. the many Scales of the Universe: Galaxies, their Suns, and their Planets - Annual Meeting of the Astronomische Gesellschaft 2017, Göttingen, Germany (2017)
Hanson, C. S.; Leguebe, M.; Fournier, D.; Brich, A. C.; Gizon, L.: Computational Local Helioseismology in the Frequency Domain. Seismology of the Sun and the Distant Stars 2016, Angra do Heroísmo, Portugal (2016)
Löptien, B.; Birch, A. C.; Duvall Jr, T. L.; Gizon, L.; Schou, J.: Measuring active region inflows with local correlation tracking. Seismology of the Sun and the Distant Stars 2016, Angra do Heroísmo, Portugal (2016)
First icy cold, then midnight sun: at the Arctic Circle, the team will prepare the next flight of the balloon-borne solar observatory - and hopes for solar fireworks.
Astronomical teamwork: By combining data from Solar Orbiter and SDO, a group of researchers has unambiguously determined the magnetic field at the solar surface.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.