Near‐Sun and near‐Earth manifestations of solar eruptions

By Nat Gopalswamy, A. Lara, M. Kaiser, J. Bougeret. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era (2008, background): “This is in addition to the radial variation discussed by Mann et al. (1999), Gopalswamy et al. (2001a), and Mann et al. (2003).”
Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, methodology): “Gopalswamy et al. (2005c) obtained an empirical relation between the shock travel time (T in h) to 1 AU and the near-Sun CME speed (V in km/s) using an average interplanetary acceleration (Gopalswamy et al. 2001a).”
Visibility of coronal mass ejections as a function of flare location and intensity (2005, unknown): “In the meanwhile, Gopalswamy et al. [2001] reported that 11 out of 34 metric type II bursts from source longitudes <60� were not associated with LASCO CMEs, indicating approximately a third of CMEs originating from the disk center were invisible to LASCO.”
CME interactions with coronal holes and their interplanetary consequences (2009, background): “…observations of CMEs and their IP counterparts over the past decade have revealed that these shocks are also CME driven but the driver does not arrive at the observer because of the observer’s location with respect to the nose of the CME [see, e.g. Gopalswamy et al., 2001a; Gopalswamy, 2006a].”
MAGNETIC PROPERTIES OF SOLAR ACTIVE REGIONS THAT GOVERN LARGE SOLAR FLARES AND ERUPTIONS (2016, unknown): “Such values can be consistent with the Alfvén speed inferred observationally for the solar corona (e.g., Gopalswamy et al. 2001), though not the core of an AR, indicating that the above estimation is fairly plausible.”
A Global Picture of CMEs in the Inner Heliosphere (2004, background): “Some CMEs have voids with no prominence in them (Gopalswamy et al. 2001d).”
Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions (2005, background): “Since the conditions for the formation of shocks at metric wavelengths are less stringent [ Gopalswamy et al., 2001a ], metric type II bursts are more abundant than the DH type II bursts.”
A statistical study on the geoeffectiveness of Earth‐directed coronal mass ejections from March 1997 to December 2000 (2002, methodology): “It should be noted that the transit time used here was not the same as the other transit times which have been used in different authors’ works [e.g., Gopalswamy et al., 2000, 2001a; Cane et al., 2000].”
A multiwavelength study of solar flare waves II. Perturbation characteristics and physical interpretation (2004, background): “Since vA and vms decrease with height at low heights above an AR (Gopalswamy et al. 2001; Mann et al. 2003), a fast disturbance will reach the critical Mach number at a lower height and therefore type II bursts will be observed at higher frequencies.”
Properties of Interplanetary Coronal Mass Ejections (2007, methodology): “They found similar results (92–93% association) for an expanded data set (Gopalswamy et al., 2001a).”
Type II radio bursts and energetic solar eruptions (2003, background): “This may be due to the fact that the Alfven speed in the low corona is typically small, so CMEs with slightly above average energies can become super-Alfvenic to produce m type II bursts [see, e.g., Gopalswamy et al., 2001a ]: once the CME speed exceeds the local Alfvenic speed, am etric type II bu”
A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “Typical coronal magnetic fields (Gopalswamy et al. 2001; Mann et al. 2003) and plasma densities (Mann et al. 1999) yield values (Ellison & Ramaty 1985) in the range of 1.3 to 1.7 for a shock speed of 1750 km s 1 at altitudes of 2Y10 R from Sun center.”
Solar and interplanetary sources of major geomagnetic storms during 1996–2002 (2004, background): “[15] A number of attempts have been made in recent years to predict the arrival time of CMEs at the Earth, for example, by Cane et al. [2000] and Gopalswamy et al. [2000, 2001a, 2001b] .”
Coronal Shocks and Solar Energetic Proton Events (2004, background): “…types of coronal shocks, one primarily observed only in the metric range (identified by the above authors with flare blast waves) and the other characteristically observed in the DH range (generally interpreted in terms of CME-driven shocks [Gopalswamy et al. 2000, 2001b; Lara et al. 2003]).”
SOLAR RELEASE TIMES OF ENERGETIC PARTICLES IN GROUND-LEVEL EVENTS (2009, background): “The Alfvén speed (and fast-mode speed) decreases rapidly with radial distance to a minimum of ∼ 200 km s−1 at ∼ 1.5 RS (∼ 100 MHz), and rises to a maximum of ∼ 500–700 km s−1 at ∼ 3 RS (∼ 14 MHz) and decreases thereafter (Mann et al. 1999, 2003; Gopalswamy et al. 2001; Vršnak et al. 2002).”
Band-splitting of coronal and interplanetary type II bursts - III. Physical conditions in the upper corona and interplanetary space (2004, methodology): “The behaviour of the magnetosonic speed in the ARcorona that is described in the last item was anticipated by Gopalswamy et al. (2001a) and Mann et al. (2003).”
The Physical Processes of CME/ICME Evolution (2017, methodology): “The cessation distance of ICME rapid deceleration (about 50 and 85 R for the 7 March 2012 and 12 December 2008 CMEs, respectively) is much shorter than the average cessation distance of 0.76 AU (163 R ) inferred indirectly by Gopalswamy et al. (2001b).”