Interplanetary acceleration of coronal mass ejections

By Nat Gopalswamy, A. Lara, R. Lepping, M. Kaiser, D. Berdichevsky, O. S. Cyr. 2000

476 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/f116ffdb904cc73adc49a1b134740e21c99f418f

How researchers see this paper

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In Astronomy and Astrophysics

1. Nat Gopalswamy
2. M. Temmer
3. B. Vršnak
4. S. Yashiro
5. N. Lugaz
6. R. Schwenn
7. R. Howard
8. A. Vourlidas

In Molecular Biology

1. Nat Gopalswamy
2. M. Temmer
3. N. Lugaz
4. R. Schwenn
5. B. Vršnak
6. R. Howard
7. J. Davies
8. A. Vourlidas

Citations in the corpus

• Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption (2004, background): “The slopes from Gopalswamy et al. (2000) and Gopalswamy et al. (2001b) are drawn at R = 40 and R = 46, respectively, corresponding to the geometrical mean (see the argumentation in Vršnak 2001a) of the considered distance ranges (0.76 and 1 au, respectively).”
• The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “To first order, this interaction results in a deceleration of fast CMEs and an acceleration of slow CMEs (Gopalswamy et al., 2000; Vršnak, 2001; Cargill, 2004; Liu et al., 2013), changes in the radial expansion rate of the magnetic ejecta (Gulisano et al., 2010; Poomvises, Zhang, and Olmedo, 2010)…”
• Solar and interplanetary sources of major geomagnetic storms during 1996–2002 (2004, background): “66 between the initial speeds of the geoeffective CMEs and the strengths of the resulting geomagnetic storms indicates that the initial speed could be used as one of the parameters for predicting geomagnetic activity [cf. Cane et al., 2000; Gopalswamy et al., 2000].”
• The SOHO/LASCO CME Catalog (2009, background): “This can be quantified as an effective interplanetary acceleration (Gopalswamy et al. 2000; 2001a).”
• Near‐Sun and near‐Earth manifestations of solar eruptions (2001, background): “The last two metric type II bursts (events 43 and 44 in Table 1) had DH type II bursts in the appropriate time window, but they are known to be associated with other eruptions that did not produce metric type II bursts [Gopalswamy et al., 2000b].”
• The Heliospheric Magnetic Field (2013, background): “CMEs move out through the corona and into the heliosphere where fast (slow) CMEs are accelerated (decelerated) towards the ambient solar wind speed (e.g., Gopalswamy et al., 2000; Cargill, 2004).”
• CME interactions with coronal holes and their interplanetary consequences (2009, background): “These suggestions were based on case studies and detailed investigations have not been performed except for the large-scale deflection by the global solar magnetic field [Gopalswamy et al., 2000b; Filippov et al., 2001; Gopalswamy et al., 2003c; Cremades et al., 2006].”
• ON SUN-TO-EARTH PROPAGATION OF CORONAL MASS EJECTIONS (2013, background): “Previous studies suggest that CMEs slower than the ambient solar wind are accelerated, whereas events faster than the solar wind are decelerated (e.g., Lindsay et al. 1999; Sheeley et al. 1999; Gopalswamy et al. 2000).”
• Properties of Interplanetary Coronal Mass Ejections (2007, methodology): “Gopalswamy et al. (2000) quantified this acceleration using SOHO and Wind observations and improved it further using quadrature data from Solwind coronagraph and Pioneer Venus Orbiter (PVO) data (Gopalswamy et al., 2001b).”