s model, while the final sphere diameter is a linear function of the initial core radius. Different sinusoidal perturbation parameters were considered, showing significant impact in the characteristics of formed spherical features. The theoretical results were in close agreement with previous experimental observations expected to assist in the unde...
s model, while the final sphere diameter is a linear function of the initial core radius. Different sinusoidal perturbation parameters were considered, showing significant impact in the characteristics of formed spherical features. The theoretical results were in close agreement with previous experimental observations expected to assist in the unde...
dinger equations that have been derived in water wave dynamics are integrable, our investigation contributes to the understanding of new effects due to wave coupling, at least for model equations that, even if not integrable, are close enough to the model considered here. For instance, our findings lead to investigate rogue waves generated by insta...
dinger equations that have been derived in water wave dynamics are integrable, our investigation contributes to the understanding of new effects due to wave coupling, at least for model equations that, even if not integrable, are close enough to the model considered here. For instance, our findings lead to investigate rogue waves generated by insta...
The gyro-resonant cosmic-ray (CR) streaming instability is believed to play a crucial role in CR transport, leading to the growth of Alfvén waves at small scales that scatter CRs, and impacts the interaction of CRs with the interstellar medium (ISM) on large scales. However, extreme scale separation (λ ≪ pc), low CR number density (n CR/n ISM ∼ 10−...
The origin of large-scale and coherent magnetic fields in astrophysical discs is an important and long-standing problem. It is common to appeal to a turbulent dynamo sustained by the magnetorotational instability (MRI) to supply the large-scale field. But research over the last decade, in particular, has demonstrated that various non-ideal magnetoh...
The origin of large-scale and coherent magnetic fields in astrophysical discs is an important and long-standing problem. It is common to appeal to a turbulent dynamo sustained by the magnetorotational instability (MRI) to supply the large-scale field. But research over the last decade, in particular, has demonstrated that various non-ideal magnetoh...
The origin of large-scale and coherent magnetic fields in astrophysical discs is an important and long-standing problem. It is common to appeal to a turbulent dynamo sustained by the magnetorotational instability (MRI) to supply the large-scale field. But research over the last decade, in particular, has demonstrated that various non-ideal magnetoh...
The origin of large-scale and coherent magnetic fields in astrophysical discs is an important and long-standing problem. It is common to appeal to a turbulent dynamo sustained by the magnetorotational instability (MRI) to supply the large-scale field. But research over the last decade, in particular, has demonstrated that various non-ideal magnetoh...
The origin of large-scale and coherent magnetic fields in astrophysical discs is an important and long-standing problem. It is common to appeal to a turbulent dynamo sustained by the magnetorotational instability (MRI) to supply the large-scale field. But research over the last decade, in particular, has demonstrated that various non-ideal magnetoh...
