In/out pairs and the detachment of coronal streamers. Coronal inflows during the interval 1996-2014. Observational characteristics of coronal mass ejections without low-coronal signatures. Statistical study of coronal mass ejections with and without distinct low coronal signatures. No trace left behind: STEREO observation of a coronal mass ejection without low coronal signatures. An analytical model for reconnection outflow jets including thermal conduction. The effect of reconnection on the structure of the Sun’s open–closed flux boundary. Fading coronal structure and the onset of turbulence in the young solar wind. The solar origin of small interplanetary transients. Examining periodic solar-wind density structures observed in the SECCHI Heliospheric Imagers. Measurements of flow speeds in the corona between 2 and 30 R ☉. SDO/AIA response to coronal hole, quiet Sun, active region, and flare plasma. Inbound waves in the solar corona: a direct indicator of Alfvén surface location. The Solar Corona 2nd edn (Cambridge Univ. Coronal holes and the high-speed solar wind. Physics and Chemistry in Space 5: Coronal Expansion and Solar Wind (ed. Dynamics of the interplanetary gas and magnetic fields. Latitudinal dependence of outflow velocities from O VI Doppler dimming observations during the Whole Sun Month. The Large Angle Spectroscopic Coronagraph (LASCO).
#Sun corona vs center temperature series
Design and on-orbit calibration of the solar ultraviolet imager (SUVI) on the GOES-R series weather satellite. Observations of an eruptive solar flare in the extended EUV solar corona. Coronal imaging with the Solar UltraViolet Imager. Exceptional extended field-of-view observations by PROBA2/SWAP on 2017 April 1 and 3. P., Mierla, M., Podladchikova, O., D’Huys, E. Study of extreme-ultraviolet emission and properties of a coronal streamer from PROBA2/SWAP, Hinode/EIS and Mauna Loa Mk4 observations. SWAP observations of the long-term, large-scale evolution of the extreme-ultraviolet solar corona. B., De Groof, A., Shearer, P., Berghmans, D. Solar coronal structure and stray light in TRACE. Transition Region and Coronal Explorer and Soft X-Ray Telescope active region loop observations: comparisons with static solutions of the hydrodynamic equations. A case for resonant scattering in the quiet solar corona in extreme-ultraviolet lines with high oscillator strengths. Can an unobserved concentration of magnetic flux above the poles of the Sun resolve the open flux problem?. The effect of solar wind expansion and nonequilibrium ionization on the broadening of coronal emission lines. On the magnetic correspondence between the photosphere and the heliosphere. Masson, S., McCauley, P., Golub, L., Reeves, K. The effect of proton temperature anisotropy on the solar minimum corona and wind. Predicting the COSIE-C signal from the outer corona up to 3 solar radii. Contextual predictions for the Parker Solar Probe. The highly structured outer solar corona.
Highly structured slow solar wind emerging from an equatorial coronal hole. Probing the energetic particle environment near the Sun. Alfvénic velocity spikes and rotational flows in the near-Sun solar wind. Near-Sun observations of an F-corona decrease and K-corona fine structure. The properties of the solar corona and its connection to the solar wind. These new data uniquely demonstrate how extreme ultraviolet observations of the middle corona provide strong new constraints on models seeking to unify the corona and heliosphere.
#Sun corona vs center temperature full
This study reveals the full kinematic profile of the initiation of several coronal mass ejections, filling a crucial observational gap that has hindered understanding of the origins of solar eruptions. These data emphasize that low-coronal phenomena can be strongly influenced by inflows from above, not only by photospheric motion, a factor largely overlooked in current models of coronal evolution. Our observations highlight that solar wind structures in the heliosphere originate from complex dynamics manifesting in the middle corona that do not occur at lower heights. Our analysis shows that the dominant emission mechanism here is resonant scattering rather than collisional excitation, consistent with recent model predictions. New observations from the Solar Ultraviolet Imager of a Geostationary Operational Environmental Satellite in August and September 2018 provide the first comprehensive look at this region’s characteristics and long-term evolution in extreme ultraviolet. Nonetheless, it remains poorly understood due to the difficulty of observing this faint region (1.5–3 R ☉). The ‘middle corona’ is a critical transition between the highly disparate physical regimes of the lower and outer solar coronae.
0 kommentar(er)
