Variability of magnetospheric storms driven by different solar wind perturbations

By K. Huttunen, H. Koskinen, R. Schwenn. 2002

157 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/5e472f0ccdf2ac92f162151fdf44726f4380d9cc

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

1. S. Gibson
2. N. Lugaz
3. Pete Riley
4. R. Schwenn
5. B. Vršnak
6. E. Kilpua
7. Tibor Török
8. W. Manchester IV

In Molecular Biology

1. Tibor Török
2. S. Gibson
3. E. Kilpua
4. S. Cranmer
5. B. Vršnak
6. N. Lugaz
7. V. Bothmer
8. A. Balogh

Citations in the corpus

• Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “Although only a small fraction of the most intense storms appear to come from CIRs alone (Gosling et al. 1991; Huttunen et al. 2002; Zhang et al. 2007), they are responsible for the majority of moderate-strength storms, especially at solar minimum (Verbanac et al. 2011; Echer et al. 2013).”
• Properties and geoeffectiveness of magnetic clouds in the rising, maximum and early declining phases of solar cycle 23 (2005, background): “For the first event the complex magnetic structure probably results from the interaction of multiple fast halo CMEs that were detected by LASCO within a short time interval, Huttunen et al.(2002b); Wang et al.”
• The Physical Processes of CME/ICME Evolution (2017, background): “In such cases, the ICME sheath is typically the primary driver of the storm (see also Huttunen et al. 2002), but cases have been reported where clear ejecta signatures upstream of the Earth and geomagnetic activity have been associated with limb CMEs (e.g., Schwenn et al. 2005; Cid et al. 2012;…”
• Geoeffective Properties of Solar Transients and Stream Interaction Regions (2017, methodology): “, Bothmer and Schwenn 1998; Huttunen et al. 2005; Li et al. 2011). The SN-type (NS-type) MCs dominate from the late declining phase of even (odd) numbered solar cycles to the next rising phase. At solar maximum a mixture of SN- and NS-type clouds are observed because the Sun’s global magnetic field ”