The dynamical nature of coronal streamers

By Y. Wang, N. Sheeley, D. Socker, R. A. Howard, N. Rich. 2000

190 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/da54f60be75179e75e038909336040ff5ad6ff99

How researchers see this paper

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In Astronomy and Astrophysics

1. S. Cranmer
2. S. Solanki
3. Roberto Lionello
4. Jon A. Linker
5. Zoran Mikic
6. J. C. Raymond
7. A. van Ballegooijen
8. R. Edgar

In Molecular Biology

1. S. Solanki
2. S. Cranmer
3. J. C. Raymond
4. S. Antiochos
5. Harry Wechsler
6. V. Titov
7. G. Noci
8. M. Schüssler

Citations in the corpus

• A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, background): “In fact, the plasma emanating from the streamer tops, the so-called stalks, is observed to be only ∼ 3◦–6◦ wide, which agrees well with the plasma sheet width in the heliosphere (Bavassano et al. 1997; Wang et al. 2000).”
• Ultraviolet spectroscopy of the extended solar corona (2006, background): “Wang et al. (2000) reviewed three proposed scenarios for the production of the “blobs” seen emerging from the tips of streamers in LASCO images (see Sect.”
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “High-resolution coronagraphic observations of streamers reveal an almost continual release of low-contrast density inhomogeneities (Sheeley et al. 1997; Wang et al. 2000).”
• Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds (2005, background): “Origins ofthe slow solar wind are still in debate; there are mainly two types argued (see Wang et al.2000 for review).”
• Automatic Detection and Tracking of Coronal Mass Ejections in Coronagraph Time Series (2008, background): “These kinds of small features have been reported and studied (e.g., Wang et al., 2000; Bemporad et al., 2005).”
• Slow Solar Wind: Observations and Modeling (2016, unknown): “At 1 AU, SSW2 plasma would be found around the narrow plasma sheet between two solar wind streams, while the SSW1 plasma can have a certain spatial extent away from the plasma sheet (Wang et al. 2000).”
• The solar magnetic field (2006, background): “Density irregularities carried away by the dense, slow wind can be observed in coronagraph image sequences out to about 30 R [536, 611] and by radio scintillation measurements to even larger distances.”