Vourlidas, A.; Sanchez Andrade-Nuño, B.; Landi, E.; Patsourakos, S.; Teriaca, L.; Schühle, U.; Korendyke, C. M.; Nestoras, I.: The Structure and Dynamics of the Upper Chromosphere and Lower Transition Region as Revealed by the Subarcsecond VAULT Observations. Solar Physics 261, pp. 53 - 75 (2010)
Banerjee, D.; Teriaca, L.; Gupta, G. R.; Imada, S.; Stenborg, G.; Solanki, S. K.: Propagating waves in polar coronal holes as seen by SUMER & EIS. Astronomy and Astrophysics 499, pp. L29 - L32 (2009)
Andretta, V.; Mauas, P. J. D.; Falchi, A.; Teriaca, L.: Helium Line Formation and Abundance during a C-Class Flare. Astrophysical Journal 681, pp. 650 - 663 (2008)
Curdt, W.; Tian, H.; Teriaca, L.; Schühle, U.; Lemaire, P.: The Ly-α profile and center-to-limb variation of the quiet Sun. Astronomy and Astrophysics 492, pp. L9 - L12 (2008)
Mierla, M.; Schwenn, R.; Teriaca, L.; Stenborg, G.; Podlipnik, B.: Analysis of the Fe X and Fe XIV line width in the solar corona using LASCO-C1 spectral data. Astronomy and Astrophysics 480, pp. 509 - 514 (2008)
Teriaca, L.; Curdt, W.; Solanki, S. K.: SUMER observations of the inverse Evershed effect in the transition region above a sunspot. Astronomy and Astrophysics 491, pp. L5 - L8 (2008)
Almeida, J. S.; Teriaca, L.; Suetterlin, P.; Spadaro, D.; Schühle, U.; Rutten, R. J.: Search for photospheric footpoints of quiet Sun transition region loops. Astronomy and Astrophysics 475 (3), pp. 1101 - 1109 (2007)
Mierla, M.; Schwenn, R.; Teriaca, L.; Stenborg, G.; Podlipnik, B.: The dynamics of the minimum solar corona during the period August-October 1996. Advances in Space Research 40, pp. 1049 - 1053 (2007)
Mierla, M.; Schwenn, R.; Teriaca, L.; Stenborg, G.; Podlipnik, B.: LASCO-C1 Spectral Analysis of Flows in the Inner Corona. Romanian Astronomical Journal 1, pp. 167 - 181 (2007)
Mauas, P. J. D.; Andretta, V.; Falchi, A.; Falciani, R.; Teriaca, L.; Cauzzi, G.: Helium line formation and abundance in a solar active region. Astrophysical Journal 619, pp. 604 - 612 (2005)
Mierla, M.; Schwenn, R.; Teriaca, L.; Stenborg, G.; Podlipnik, B.: Dynamics of the Solar Corona Using LASCO-C1 Spectral Data. Romanian Astronomical Journal 1, p. 137 (2005)
Wilhelm, K.; Fludra, A.; Teriaca, L.; Harrison, R. A.; Dwivedi, B. N.; Pike, C. D.: The widths of vacuum-ultraviolet spectral lines in the equatorial solar corona observed with CDS and SUMER. Astronomy and Astrophysics 435, pp. 733 - 741 (2005)
Teriaca, L.; Banerjee, D.; Falchi, A.; Doyle, J. G.; Madjarska, M. S.: Transition region small-scale dynamics as seen by SUMER on SOHO. Astronomy and Astrophysics 427, pp. 1065 - 1074 (2004)
Wilhelm, K.; Dwivedi, B. N.; Teriaca, L.: On the widths of the Mg X lines near 60 nm in the corona. Astronomy and Astrophysics 415, pp. 1133 - 1139 (2004)
The Planetary Plasma Environments group (PPE) has a strong heritage in the exploration of planetary magnetospheres and space plasma interactions throughout the solar system. It has contributed instruments to several past missions that flew-by or orbited Jupiter (Galileo, Cassini, Ulysses). The PPE participates in the JUICE mission by contributing hardware and scientific expertise to the Particle Environment Package (PEP).
First Light for Sunrise III: the first tests with real sunlight were successful. The balloon-borne solar observatory should be ready for launch at the end of May.
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.
Images from ESA’s Solar Orbiter offer the best look yet at a source region of the solar wind - and challenge our view of the continuous particle stream from the Sun.
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.