FLOWS AT THE EDGE OF AN ACTIVE REGION: OBSERVATION AND INTERPRETATION

@article{Boutry2012FLOWSAT,
  title={FLOWS AT THE EDGE OF AN ACTIVE REGION: OBSERVATION AND INTERPRETATION},
  author={Céline Boutry and {\'E}ric Buchlin and Jean Claude Vial and St'ephane R'egnier},
  journal={The Astrophysical Journal},
  year={2012},
  volume={752},
  pages={13}
}
Upflows observed at the edges of active regions have been proposed as the source of the slow solar wind. In the particular case of Active Region (AR) 10942, where such an upflow has been already observed, we want to evaluate the part of this upflow that actually remains confined in the magnetic loops that connect AR 10942 to AR 10943. Both active regions were visible simultaneously on the solar disk and were observed by STEREO/SECCHI EUVI. Using Hinode/EIS spectra, we determine the Doppler… 
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19 Citations
Background Citations
9
Methods Citations
1

19 Citations

Dynamics in the Transition Region beneath Active Region Upflows Viewed by IRIS
Coronal upflows at the edges of active regions (ARs), which are a possible source of slow solar wind, have been found to connect with dynamics in the transition region. To infer at what scale…
The Formation and Lifetime of Outflows in a Solar Active Region
Active regions are thought to be one contributor to the slow solar wind. Upflows in EUV coronal spectral lines are routinely observed at their boundaries, and provide the most direct way for…
Active region upflows: 1. Multi-instrument observations
Upflows at the edges of active regions (ARs) are studied by spatially and temporally combining multi-instrument observations obtained with EIS/Hinode, AIA and HMI/SDO and IBIS/NSO, to derive their…
Active region upflows. II. Data driven magnetohydrodynamic modelling
Context. Observations of many active regions show a slow systematic outflow/upflow from their edges lasting from hours to days. At present no physical explanation has been proven, while several…
Plasma Upflows Induced by Magnetic Reconnection Above an Eruptive Flux Rope
One of the major discoveries of Hinode’s Extreme-ultraviolet Imaging Spectrometer (EIS) is the presence of upflows at the edges of active regions. As active regions are magnetically connected to the…
Upflows in the Upper Solar Atmosphere
Spectroscopic observations at extreme- and far-ultraviolet wavelengths have revealed systematic upflows in the solar transition region and corona. These upflows are best seen in the network…
Slow Solar Wind: Observations and Modeling
While it is certain that the fast solar wind originates from coronal holes, where and how the slow solar wind (SSW) is formed remains an outstanding question in solar physics even in the post-SOHO…
Magnetic Field Extrapolations into the Corona: Success and Future Improvements
The solar atmosphere being magnetic in nature, the understanding of the structure and evolution of the magnetic field in different regions of the solar atmosphere has been an important task over the…
Chapter 2 Nature and Variability of Plasmas Ejected by the
The Sun not only emits radiation in the whole electromagnetic spectrum but also sends in the interplanetary medium plasmas of different natures (energy, continuous, or episodic flows, etc.) which…
Observations of Reconnection Flows in a Flare on the Solar Disk
Magnetic reconnection is a well-accepted part of the theory of solar eruptive events, though the evidence is still circumstantial. Intrinsic to the reconnection picture of a solar eruptive event,…
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