Band-splitting of coronal and interplanetary type II bursts - II. Coronal magnetic field and Alfvén velocity
By B. Vršnak, Jasmina Magdalenic, H. Aurass, G. Mann. 2002
174 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/d5dc9ea59027684fb4fb3182d0ff516f26f4df46
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In Astronomy and Astrophysics
Citations in the corpus
- A multiwavelength study of solar flare waves II. Perturbation characteristics and physical interpretation (2004, methodology): “7) is enhanced due to an increase of collisional processes (see Vršnak et al. 2002a).”
- The Two Sources of Solar Energetic Particles (2012, background): “These “early” events usually also have associated f st CMEs and shock waves (e.g. Gopalswamy et al. 2012) which must accelerate just as efficiently here as they do in the “late” events.”
- OBSERVATIONS AND INTERPRETATION OF A LOW CORONAL SHOCK WAVE OBSERVED IN THE EUV BY THE SDO/AIA (2011, methodology): “(3) As described in Vršnak et al. (2002), the band-split frequencies in type II emission map the electron densities behind and ahead of the shock front.”
- Numerical simulations of fast and slow coronal mass ejections (2007, background): “…impulsive to slow gradual ones, it also reproduces the observed association of impulsive profiles with highly concentrated flux in the source (active regions, highn) and of gradual profiles with the gradual field decrease over a large height range in the quiet Sun (n ∼ 3/2, Vršnak et al. 2002).”
- SOLAR RELEASE TIMES OF ENERGETIC PARTICLES IN GROUND-LEVEL EVENTS (2009, background): “More recently, Gopalswamy et al. (2005) studied the CME height at the time of SPR for the GLE events of cycle 23, assuming a fixed path length of 1.2 AU for the particles.”
- Coronal Shocks and Solar Energetic Proton Events (2004, background): “…between DH type IIs and SEP events is suggested by the work of Mann et al. (1999), Gopalswamy et al. (2001a), Gopalswamy & Kaiser (2002), and Vršnak et al. (2002), who determined that the Alfvén speed in the corona typically has a peak value of 3 R , corresponding to the 14 MHz plasma…”
- Band-splitting of coronal and interplanetary type II bursts - III. Physical conditions in the upper corona and interplanetary space (2004, methodology): “4 we show the outcome only for θ = 90◦ (shock normal perpendicular to the magnetic field) since it was shown in Paper II that the choice of θ does not influence the results significantly (see also Vršnak et al. 2002a): for typical bandsplits BDW = 0.2–0.3 (Fig.”
- Hot Jupiters and Hot Spots: The Short- and Long-Term Chromospheric Activity on Stars with Giant Planets (2004, background): “For p = 2 (Vrsnak et al. 2002 for the case of our Sun, and Weber & Davis 1967 for the case of open fields), q = 2, a = 0.045 AU, R∗ = 1.3 R⊙, Rp = 1.1 RJ , Prot = 9 d, B∗ = 200 G, and Bp = 10 G, the energy flux 7Since the sound speed is much less than the Alfvén speed in the extended coronal…”