Photospheric and heliospheric magnetic fields

By C. Schrijver, M. DeRosa. 2003

527 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/96357579bb50f96f8b25b6eea0525dc27f4f5254

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In Astronomy and Astrophysics

1. C. Schrijver
2. T. Wiegelmann
3. A. Title
4. M. DeRosa
5. G. Aulanier
6. Pete Riley
7. G. Barnes
8. A. A. Ballegooijen

Citations in the corpus

• 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).”
• The Open Flux Problem (2017, methodology): “…synchronic maps were constructed using the ADAPT model (based on NSO VSM magnetograms) and the LMSAL Evolving SurfaceFlux Assimilation Model (ESFAM; Schrijver & DeRosa 2003, based on SOHO MDI magnetograms) as well as daily updated synoptic maps for GONG, SDO HMI, SOHO MDI, and NSO VSM (referred to…”
• The Heliospheric Magnetic Field (2013, background): “The solar cycle evolution of photospheric magnetic flux has been well characterised by three complete cycles of observation (Schrijver and DeRosa, 2003; Hathaway, 2010).”
• Long‐range magnetic couplings between solar flares and coronal mass ejections observed by SDO and STEREO (2011, methodology): “[16] The full‐sphere magnetic field is being created by direct insertion of the line‐of‐sight magnetic field observed within 60° of disk center into a full‐sphere field that is evolving subject to differential rotation, meridional advection, and random walk dispersal (http://www.lmsal.com/ forecast/”
• Nonlinear Force-Free Modeling of Coronal Magnetic Fields. II. Modeling a Filament Arcade and Simulated Chromospheric and Photospheric Vector Fields (2008, background): “This assumption has proven to be adequate for many quiescent, old active regions and even for the noneruptive global coronal-heliospheric interface (e.g., Wang and Sheeley, 1990; Hoeksema, 1991; Schrijver and 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): “…help address fundamental unsolved problems in active region physics, such as heating in active region loops (e.g., Klimchuk 2006; Warren & Winebarger 2007), and the associations of active regions with the solar wind and heliospheric magnetic flux (e.g., Liewer et al. 2004; Schrijver & DeRosa 2003).”
• RECONNECTION OUTFLOWS AND CURRENT SHEET OBSERVED WITH HINODE/XRT IN THE 2008 APRIL 9 “CARTWHEEL CME” FLARE (2010, methodology): “We use a Potential Field Source Surface (PFSS, Schrijver & DeRosa 2003) model to extrapolate the magnetic field from active region 10989.”
• The Nonpotentiality of Active-Region Coronae and the Dynamics of the Photospheric Magnetic Field (2005, methodology): “…a solar-wind field advection model, the model solar wind conditions near Earth are frequently found to match the observed conditions quite well during quiescent phases (Schatten et al. 1969; Hoeksema 1984; Zhao & Hoeksema 1995; Wang & Sheeley 1992; Neugebauer et al. 1998; Schrijver & DeRosa 2003).”