What Is Missing from Our Understanding of Long-Term Solar and Heliospheric Activity?

By C. Schrijver, M. DeRosa, A. Title. 2002

140 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/1fcd1527f9b7b3613eb06e5a89fd430ddd7ea305

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In Astronomy and Astrophysics

1. S. Solanki
2. I. Usoskin
3. Paul Charbonneau
4. N. Krivova
5. Matthias Rempel
6. Y. Wang
7. A. Title
8. T. Wiegelmann

In Molecular Biology

1. Paul Charbonneau
2. S. Solanki
3. I. Usoskin
4. N. Krivova
5. C. Schrijver
6. T. Wiegelmann
7. J. Thalmann
8. Matthias Rempel

Citations in the corpus

• Modeling the Sun’s Magnetic Field and Irradiance since 1713 (2005, background): “When the meridional flow speed was held fixed, we found that the polar fields built up during the more active cycles were too strong to be reversed during the less active ones (a similar problem was encountered by Schrijver et al. 2002).”
• A phenomenological study of the long-term cosmic ray modulation, 850-1958 AD (2004, methodology): “It is shown that there is better agreement between the variations in the (10)Be data, and the changes in the open solar magnetic flux predicted by the Schrijver et al. [2002] and Solanki et al. [2002] models based on historic sunspot numbers.”
• A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results (2006, methodology): “To fully address this, we must study solutions incorporating the evolution of the photospheric magnetic field (Mikić et al. 1999; Schrijver et al. 2002).”
• Acceleration of the solar wind as a result of the reconnection of open magnetic flux with coronal loops (2003, background): “Processes similar to this are invoked to explain the evolution of the polar magnetic field of the Sun [Schrijver et al., 2002] and to explain the apparent ease with which the magnetic fields in CMEs become detached from the Sun and do not result in a buildup of the magnetic field in the heliosphere…”
• Sunspot Group Tilt Angles and the Strength of the Solar Cycle (2010, background): “Schrijver et al. (2002) tested the hypothesis where the polar magnetic field on the Sun is determined by the accumulation of field transported poleward from sunspots at lower latitudesas a consequence of the tilt in the bipoles.”
• Magnetic Flux Transport at the Solar Surface (2014, background): “Schrijver et al. (2002) found that a simple exponential decay of the fieldτd with a decay time of about 10 yr allowed regular reversals of the polar fields given fluc- 20 tuations in the source term similar to those in the historical records.”
• Solar Cycle Prediction Using Precursors and Flux Transport Models (2006, background): “D effects (Schrijver et al. 2002; Baumann et al. 2006).”
• Flux-Transport Dynamos with Lorentz Force Feedback on Differential Rotation and Meridional Flow: Saturation Mechanism and Torsional Oscillations (2006, background): “…observations (it is the essential ingredient in models describing the evolution of the surface magnetic field assimilating real observations (Schrijver et al. 2002; Baumann et al. 2004, 2006; Wang et al. 2005)) this is of secondary concern for the model presented here; it is however of…”
• Long‐range magnetic couplings between solar flares and coronal mass ejections observed by SDO and STEREO (2011, methodology): “SolarSoft PFSS package (described by, e.g., Schrijver et al. [2002] ), which matches the normal component of the surface magnetic field to a potential field that is forced to become radial at 1.5 R� above the solar surface.”
• The magnetic field in the solar atmosphere (2014, background): “As a consequence, the open flux on global scales varies in the course of the solar cycle (its long-term variation was computed by Solanki et al. 2000, 2002; Schrijver et al. 2002; Jiang et al. 2011).”
• Dynamo Models of the Solar Cycle (2005, background): “…that magnetic flux liberated by the decay of tilted bipolar active regions does accumulate in the polar regions, where it triggers polarity reversal of the poloidal component (see Wang and Sheeley Jr, 1991; Schrijver et al., 2002; Wang et al., 2002; Baumann et al., 2004, and references therein).”