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Signatures of Slow Solar Wind Streams from Active Regions in the Inner Corona

  • PROBA2 – First Two Years of Solar Observation
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Abstract

The identification of solar-wind sources is an important question in solar physics. The existing solar-wind models (e.g., the Wang–Sheeley–Arge model) provide the approximate locations of the solar wind sources based on magnetic field extrapolations. It has been suggested recently that plasma outflows observed at the edges of active regions may be a source of the slow solar wind. To explore this we analyze an isolated active region (AR) adjacent to small coronal hole (CH) in July/August 2009. On 1 August, Hinode/EUV Imaging Spectrometer observations showed two compact outflow regions in the corona. Coronal rays were observed above the active-region coronal hole (ARCH) region on the eastern limb on 31 July by STEREO-A/EUVI and at the western limb on 7 August by CORONAS-Photon/TESIS telescopes. In both cases the coronal rays were co-aligned with open magnetic-field lines given by the potential field source surface model, which expanded into the streamer. The solar-wind parameters measured by STEREO-B, ACE, Wind, and STEREO-A confirmed the identification of the ARCH as a source region of the slow solar wind. The results of the study support the suggestion that coronal rays can represent signatures of outflows from ARs propagating in the inner corona along open field lines into the heliosphere.

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Acknowledgements

The authors are very grateful to Y.-M. Wang for providing and commenting on the WSA map of the derived coronal holes for CR 2086, and to Nariaki Nitta and Andrey Zhukov for useful discussions. Many thanks to the anonymous referee for valuable remarks and advice which helped to significantly improve the article. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, and with NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA (USA), ESA, and NSC (Norway). We are grateful to NASA, ESA, and the TRACE and STEREO teams for their open data policy. SOHO is a project of international cooperation between ESA and NASA. The CORONAS-Photon/TESIS data were provided by the team of the Laboratory of X-ray Astronomy of the Sun of the P.N. Lebedev Physical Institute of the Russian Academy of Sciences. We thank the ACE SWEPAM and SWICS instrument teams and the ACE Science Center for providing the ACE data. The Wind/SWE experiment is a collaborative effort of the Goddard Space Flight Center (GSFC), University of New Hampshire (UNH), and Massachusetts Institute of Technology (MIT). This work was supported by the FP-7 Projects of the European Commission N 218816 SOTERIA, N 284461 eHEROES and the PROBA2 Guest Investigation Grant. SWAP is a project of the Centre Spatial de Liège and the Royal Observatory of Belgium funded by the Belgian Federal Science Policy Office (BELSPO). The work was partially supported by Grant 11-02-01079 of the Russian Foundation for Fundamental Research and Grant OFN-15 of the Russian Academy of Sciences.

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  1. P.N. Lebedev Physical Institute, Leninsky Pr., 53, Moscow, 119991, Russia

    V. Slemzin, A. Urnov, S. Kuzin & F. Goryaev

  2. UCL-Mullard Space Science Laboratory, Holmbury St Mary, Dorking, Surrey, RH5 6NT, UK

    L. Harra

  3. Royal Observatory of Belgium, Ringlaan 3, 1180, Brussels, Belgium

    F. Goryaev & D. Berghmans

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  1. V. Slemzin
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PROBA2 – First Two Years of Solar Observation

Guest Editors: David Berghmans, Anik De Groof, Marie Dominique, and Jean-François Hochedez

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Slemzin, V., Harra, L., Urnov, A. et al. Signatures of Slow Solar Wind Streams from Active Regions in the Inner Corona. Sol Phys 286, 157–184 (2013). https://doi.org/10.1007/s11207-012-0004-y

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