Listed are all scientific papers resulting from an ISSI activity written or co-authored by ISSI Team members, Working Group members, Workshop participants, visitors or staff members.
In situ observations of the solar wind have shown that the electron velocity distribution function (VDF) consists of a quasi-Maxwellian core, comprising most of the electron population, and two sparser components: the halo, which are suprathermal and quasi-isotropic electrons, and an escaping beam population, the strahl.
An instability criterion in the magnetohydrodynamics (MHD) with the open boundary of a magnetic field is proposed in this paper. We use a series of linear force-free extrapolation fields, in which the normal part of the magnetic field is fixed, to obtain the linear fitting coefficient called relative alpha by using the cojoined value of magnetic free energy and magnetic flux at the open boundary (EfΦ2) and the square of relative magnetic helicity ( HR2 ).
Context. Galaxy groups with total masses below ∼1014 M⊙ and up to a few tens of members are the most common galaxy environment, marking the transition between the field and the most massive galaxy clusters. In this framework, identifying and studying groups plays a crucial role in understanding structure formation and galaxy evolution.
Accurate quantification of regional ocean mass changes is crucial for coastal communities to formulate effective management strategies. The regional ocean mass budget comprises the barystatic component driven by terrestrial water and ice mass changes, and ocean mass redistribution resulting from non‐tidal oceanic and atmospheric (Nt‐OcnAtm), the latter being zero in the global mean.
Evapotranspiration (ET) serves as a crucial indicator for understanding both global and regional water cycles and the impacts of climate change. Traditionally, water balance-based ET derived using satellite gravimetry, runoff and precipitation is considered as a benchmark for ET assessment.
Understanding the processes that transform star-forming galaxies into quiescent ones is key to unravelling the role of environment in galaxy evolution.
Aims. Observations and simulations of coronal rain show that as cold and dense plasma falls through the corona, it initially undergoes acceleration by gravity before the downward velocity saturates. Simulations have shown the emergence of an unexpected relation between the terminal velocity of the rain and density ratio that has not been explained. Our aim is to explain this relation. Methods.
Tidal interactions play a key role in the dynamics and evolution of icy worlds. The intense tectonic activity of Europa and the eruption activity on Enceladus are clear examples of the manifestation of tidal deformation and associated dissipation. While tidal heating has long been recognized as a major driver in the activity of these icy worlds, the mechanism controlling how tidal forces deform the different internal layers and produce heat by tidal friction still remains poorly constrained.
Aims. We aim to investigate the energy-resolved pulse profile changes of the accreting X-ray pulsar V 0332+53 focusing in the cyclotron line energy range, using the full set of available NuSTAR observations. Methods. We applied a tailored pipeline to study the energy dependence of the pulse profiles and to build the pulsed fraction spectra (PFS) for the different observations. We also studied the profile changes using cross-correlation and lag spectra.
We examine the statistical properties of extreme solar activity levels through the application of the extreme value theory to the annual sunspot number series reconstructed from 14C data spanning the last millennium. We have used the extreme value theory to study long-term solar variability by applying the peaks-over-threshold technique to an annual sunspot number series reconstructed from 14C data for the last millennium.
