Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· arXiv e-print (arXiv:1203.6756)
· References in the article
· Citations to the Article (12) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Signatures of Slow Solar Wind Streams from Active Regions in the Inner Corona
Authors:
Slemzin, V.; Harra, L.; Urnov, A.; Kuzin, S.; Goryaev, F.; Berghmans, D.
Affiliation:
AA(P.N. Lebedev Physical Institute), AB(UCL-Mullard Space Science Laboratory), AC(P.N. Lebedev Physical Institute), AD(P.N. Lebedev Physical Institute), AE(P.N. Lebedev Physical Institute; Royal Observatory of Belgium), AF(Royal Observatory of Belgium)
Publication:
Solar Physics, Volume 286, Issue 1, pp.157-184 (SoPh Homepage)
Publication Date:
08/2013
Origin:
SPRINGER
Keywords:
Sun: corona, Sun: EUV imaging, Active regions, Solar wind: source regions, Differential emission measure
Abstract Copyright:
(c) 2013: Springer Science+Business Media B.V.
DOI:
10.1007/s11207-012-0004-y
Bibliographic Code:
2013SoPh..286..157S

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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints