Add to ORKGThe elemental composition of the Sun's hot atmosphere, the corona, shows a distinctive pattern that is different from the underlying surface or photosphere. Elements that are easy to ionize in the chromosphere are enhanced in abundance in the corona compared to their photospheric values. A similar pattern of behavior is often observed in the slow-speed (<500 km s−1) solar wind and in solar-like stellar coronae, while a reversed effect is seen in M dwarfs. Studies of the inverse effect have been hampered in the past because only unresolved (point-source) spectroscopic data were available for these stellar targets. Here we report the discovery of several inverse events observed in situ in the slow solar wind using particle-counting techniques...
While the source of the fast solar wind is known to be coronal holes, the source of the slow solar w...
A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly lo...
The opening of closed magnetic loops via reconnection with open solar flux, so called “interchange r...
International audienceThe elemental composition of the Sun's hot atmosphere, the corona, shows a dis...
We present the first in situ observations of heavy ion dropouts within the slow solar wind, observed...
We analyze the physical origin of plasmas that are ejected from the solar corona. To address this is...
A theory for the origin of the slow solar wind is described. Recent papers have demonstrated that ma...
We present results from a comparison of CME and slow solar wind ejecta detected at the ACE spacecraf...
The elemental composition in the coronae of low-activity solar-like stars appears to be related to f...
Although the origins of slow solar wind are unclear, there is increasing evidence that at least some...
The higher charge states found in slow (<400 km s[superscript −1]) solar wind streams compared to fa...
Coronal elemental abundances, as compared with abundances in the solar wind and solar energetic part...
Observations of the extended corona obtained with the Ultraviolet Coronagraph Spectrometer (UVCS) on...
The solar wind consists of continuous streams of charged particles that escape into the heliosphere ...
Spectroscopic observations of the solar atmosphere reveal regions of the solar corona that are enric...
While the source of the fast solar wind is known to be coronal holes, the source of the slow solar w...
A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly lo...
The opening of closed magnetic loops via reconnection with open solar flux, so called “interchange r...
International audienceThe elemental composition of the Sun's hot atmosphere, the corona, shows a dis...
We present the first in situ observations of heavy ion dropouts within the slow solar wind, observed...
We analyze the physical origin of plasmas that are ejected from the solar corona. To address this is...
A theory for the origin of the slow solar wind is described. Recent papers have demonstrated that ma...
We present results from a comparison of CME and slow solar wind ejecta detected at the ACE spacecraf...
The elemental composition in the coronae of low-activity solar-like stars appears to be related to f...
Although the origins of slow solar wind are unclear, there is increasing evidence that at least some...
The higher charge states found in slow (<400 km s[superscript −1]) solar wind streams compared to fa...
Coronal elemental abundances, as compared with abundances in the solar wind and solar energetic part...
Observations of the extended corona obtained with the Ultraviolet Coronagraph Spectrometer (UVCS) on...
The solar wind consists of continuous streams of charged particles that escape into the heliosphere ...
Spectroscopic observations of the solar atmosphere reveal regions of the solar corona that are enric...
While the source of the fast solar wind is known to be coronal holes, the source of the slow solar w...
A recent paper [Shearer et al., 2014] reported that during solar maximum Ne showed a surprisingly lo...
The opening of closed magnetic loops via reconnection with open solar flux, so called “interchange r...