This observation is consistent with the observations obtained with Yohkoh/Soft X-ray Telescope (SXT) that soft X-ray cusp structures only appear after the major impulsive energy release in solar flares.
A set of experiments (Table 2) was conducted to reduce the amount of volatiles in the run charge; nonetheless, they show the appearance of dendritic aggregates of a carbonate phase at 4.0 GPa, 870 °C (Fig. 6e), and, most notably, small pools with lobe and cusp structures (Fig. 6f) at 3.8 4.2 GPa, 900 °C.
Lobe and cusp structures are known to develop during viscous fingering moved by Saffman–Taylor instabilities in liquids of contrasting viscosities (e.g., Perugini and Poli, 2005), and their coexistence with whiskery crystals strongly suggests the occurrence of more than a single liquid on quenching of these experiments.
The syngas flames possess much wrinkled flame front with much smaller fine cusps structure compared to that of CH4/air flames and the main difference is on the convex structure.
In this study, we demonstrated a one-to-one correspondence between the moving cusp auroral structure measured at a wavelength of 630.0 nm and the electron precipitation region responsible for its creation.
Using data from the high-sensitivity all-sky imager at Longyearbyen, Svalbard, and particle data from the DMSP F18 spacecraft, we examined particle precipitation features in the early and final stages of a moving cusp auroral structure.
Since then, this odontogenic anomaly has been given several descriptions, such as, prominent accessory cusp-like structure [ 3], exaggerated cingula [ 4] additional cusp [ 5], cusp-like hyperplasia [ 6], accessory cusp [ 7] and supernumerary cusp [ 8].
The cusp-leading nature of the fingering pattern is revealed, which is opposite to the cusp-trailing structure typical of premixed gas cellular/wrinkled flames.
For example, Tsuneta et al. (1992) discovered the cusp-shaped structure during the solar flare seen in the lower right panel in Fig. 3 a.
