Sources of the solar wind at solar activity maximum

By M. Neugebauer, P. Liewer, E. Smith, R. Skoug, T. Zurbuchen. 2002

147 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/d1f6bd17995900feb58c70e85cbfa5639636c7a6

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results (2006, background): “These include (1) coronal structure during eclipses (e.g., Smith & Schatten 1970) (2) interplanetary magnetic fields (e.g., Burlaga et al. 1978) (3) wave propagation in the corona (e.g., Uchida et al. 1973) and (4) the photospheric sources of solar wind (e.g., Neugebauer et al. 2002).”
The three‐dimensional solar wind around solar maximum (2003, background): “These flows arise from a mixture of sources including streamers, coronal mass ejections (CMEs), small low latitude coronal holes, and possibly active regions [Neugebauer et al., 2002].”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “There is increasing evidence that much of the slow solar wind is connected somehow to open flux tubes that are rooted in or near active regions (e.g., Neugebauer et al. 2002; Liewer et al. 2004).”
Flows and Nonthermal Velocities in Solar Active Regions Observed with the EUV Imaging Spectrometer on Hinode: A Tracer of Active Region Sources of Heliospheric Magnetic Fields? (2008, background): “Liewer et al. (2004), Schrijver &DeRosa (2003), Luhmann et al. (2002), Neugebauer et al. (2002), and Wang & Sheeley (2002) have found from data and modeling that active regions can contribute substantially to the heliospheric magnetic field and solar wind.”
Global distribution of the solar wind during solar cycle 23: ACE observations (2009, methodology): “We assume as did Neugebauer et al. [2002] that solar wind plasma propagates radially from the source surface to the spacecraft at a constant speed, which we take to be the observed proton speed.”
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, methodology): “The origin of the slow solar wind is still under consideration with observations suggesting coronal streamers [Gosling et al., 1981], coronal hole boundaries [Neugebauer et al., 1998], and active regions [Neugebauer et al., 2002] as potential sources.”
Slow Solar Wind: Observations and Modeling (2016, unknown): “There have been detailed studies of an active region (Neugebauer et al. 2002) that also show how upflows can become outflows even with no associated coronal hole.”