Solar cycle changes in coronal holes and space weather cycles

By Jan Luhmann, Y. Li, Charles N. Arge, P. Gazis, R. Ulrich. 2002

141 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/01b18a8d510640381bd8a36687909bf34cf2b91b

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In Astronomy and Astrophysics

Citations in the corpus

Energetic Particles and Corotating Interaction Regions in the Solar Wind (2004, background): “, Richardson, Cane, and Cliver, 2002), but these typically emerge from small, lower latitude, coronal holes (e.g., Bravo, Stewart, and Blanco-Cano, 1998; Luhmann et al., 2002; Neugebauer et al., 2002; Wang, Sheeley, and Andrews, 2002; Wang and Sheeley, 2003).”
Geomagnetic activity indicates large amplitude for sunspot cycle 24 (2006, background): “Additional drivers of geomagnetic activity include interplanetary shocks from high-speed solar wind streams associated with coronal holes that are out of phase with the sunspot cycle [cf. Luhmann et al., 2002 ].”
Coronal Holes, Jets, and the Origin of 3He-rich Particle Events (2006, background): “…structures generally coincide with coronal holes, which are observed as an absence of emission in soft X-ray and EUVimages and as light areas in He i k10830 spectroheliograms (see, e.g., Levine et al. 1977; Wang et al. 1996; Neugebauer et al. 1998; Luhmann et al. 2002; Schrijver & DeRosa 2003).”
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.”
A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results (2006, methodology): “However, it is the basic model developed almost 40 years ago that remains the most widely used (e.g., Luhmann et al. 2002), and hence it is this model that we focus our comparison on here.”
THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID (2010, methodology): “Here we use the potential field source surface (PFSS) model (Luhmann et al. 2002; Zhao et al. 2006; Hu et al. 2008) to determine the expansion factor fS and θb and choose the source surface at 2.5 RS.”
Properties of Interplanetary Coronal Mass Ejections at One AU During 1995 – 2004 (2006, background): “…noted in Cane, Richardson, and St. Cyr (2000) and Cane and Richardson (2003), probably associated with an increase of co-rotating highspeed streams from low-latitude coronal holes and the restructuring of the nearecliptic solar wind in 1999 (e.g., Luhmann et al., 2002; Cane and Richardson, 2003).”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “Figure 8 shows how PFSS models can also be useful tools for mapping the origins of solar wind streams (see also Luhmann et al. 2002; Liewer et al. 2004; Fazakerley et al. 2016).”