Formation and development of shock waves in the solar corona and the near-Sun interplanetary space

By G. Mann, A. Klassen, H. Aurass, H. Classen. 2003

182 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/09ebbbdc26fff8c8148abc1cfe294cfab1eecaea

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In Astronomy and Astrophysics

Citations in the corpus

Space Weather: The Solar Perspective (2006, background): “For a majority of the slower CMEs this stringent condition is not fulfilled before the CMEs reach a distance of several Rs (Mann 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).”
An Observational Overview of Solar Flares (2011, background): “The existence of a minimum in the Alfvén speed in the middle corona (Mann et al. 2003) allows the CME-driven disturbance to attain a higher Mach number even as its absolute speed may be constant or even decreasing.”
Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption (2004, methodology): “Let us note that using the isothermal (T = 106 K) solar wind model by Parker (1958; see also Mann et al. 2003) instead of Eq.”
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.”
Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, methodology): “Other methods of computing the Alfvén speed profile can be found in Mann et al. (2003) and Warmuth and Mann (2005), but they all lead to qualitatively similar profile with a minimum Alfvén speed around 1.5 Rs and a maximum around 3.5 Rs .”
The Two Sources of Solar Energetic Particles (2012, background): “…to a minimum of ∼200 km s-1 at ∼ 1.5 solar radii (∼100 MHz), rises to a maximum of ~500–700 km s-1 at ∼3 solar radii (∼14 MHz) and decreases thereafter (Mann et al. 1999, 2003; Gopalswamy et al. 2001; Vršnak et al. 2002) On the flanks of the shock, acceleration times are later and altitudes are…”
Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era (2008, background): “It is well known that shocks accelerate electrons and protons efficiently when the Mach number exceeds a critical value, which depends on the plasma beta (see Mann et al., 2003, for a discussion on this topic).”
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.”
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).”
Solar Orbiter (2012, background): “It will measure the acceleration profile of the latter and then track the CMEs through the crucial heights for shock formation (2 – 10 RSun) and provide speed, acceleration, and shock compression ratio measurements.”