179 papers
Space physics explores the dynamic environment surrounding our planet and the wider solar system, focusing on how charged particles, magnetic fields, and solar winds interact with celestial bodies. This field helps us understand phenomena like auroras, space weather that can disrupt satellites, and the fundamental behavior of plasma in the vacuum of space. It bridges the gap between astronomy and particle physics, revealing the invisible forces that shape our cosmic neighborhood.
At Gist.Science, we process every new preprint in this category as it appears on arXiv, ensuring you get immediate access to the latest research. For each paper, we provide both a detailed technical summary for experts and a plain-language explanation that makes complex concepts understandable for everyone. Below are the latest space physics papers from arXiv, curated and simplified for your reading.
This study presents the first statistical assessment of using STEREO-A as a sub-L1 monitor for geomagnetic storm forecasting, demonstrating that while longitudinal position significantly influences lead time and intense storms are well-detected, radial separations up to ~0.05 au do not guarantee early warnings and current empirical methodologies tend to predict storm minima later and stronger than observed.
This study systematically compares the ALPS and BO solvers for computing plasma dispersion relations across various particle velocity distributions, finding that while they yield consistent results for many cases, BO becomes unreliable for low-kappa distributions due to fitting limitations, suggesting that a combined approach leveraging the complementary strengths of both solvers offers the most robust framework for investigating non-Maxwellian plasma instabilities.
This paper employs quasi-linear theory to analytically derive a unified ion heating rate that smoothly transitions between stochastic and cyclotron-resonant mechanisms depending on the imbalance of Alfvénic turbulence, while explaining the suppression of heating at small amplitudes due to magnetic moment conservation.
The paper introduces SIREN, a lightweight and interpretable Transformer-based model that outperforms traditional methods in detecting Solar Wind Stream Interaction Regions by leveraging self-attention to identify key physical signatures like proton density and flow deflection, thereby enabling flexible, calibrated probabilities for operational space weather forecasting.
This paper utilizes the GRAPES-3 muon telescope to monitor upper atmospheric temperature and the interplanetary magnetic field by analyzing how solar-induced phenomena, such as solar cycles and transient events, modulate the flux, spectrum, and angular distribution of Galactic Cosmic Rays up to approximately 30 GeV/nuc.
This paper reports ground-based ICEBEAR radar observations of extreme, transient electric field enhancements in the auroral ionosphere, identified as the ionospheric footprints of magnetotail dipolarization-driven shear Alfvén pulses, thereby elucidating the tight coupling between magnetospheric substorms and meter-scale plasma turbulence.
This paper utilizes fully kinetic particle-in-cell simulations and linear theory to demonstrate that parallel-propagating electromagnetic ion cyclotron (EMIC) waves can drive secondary lower-hybrid instabilities in multi-component plasmas, leading to anisotropic heating of cold ions and electrons even at low wave amplitudes.
This study utilizes superposed epoch analysis of over 1600 CMEs from 0.2 to 2.2 au to reveal that CMEs during the solar active phase are faster and magnetically stronger than those in the quiet phase due to intrinsic eruption differences, while also demonstrating that CME magnetic ejecta expand uniformly in toroidal and poloidal dimensions and exhibit increasing magnetic field asymmetry with heliocentric distance.
This study utilizes high-resolution 2.5D MHD simulations with virtual spacecraft to demonstrate that the observed signatures of magnetic clouds in the turbulent solar wind—ranging from stable, rotating magnetic clouds to disordered magnetic obstacles—are determined by the interplay of expansion rates, turbulence intensity, and the specific geometry of the spacecraft encounter relative to the flux rope's initial magnetic configuration.
This paper calculates comprehensive multi-level and multi-term collisional depolarization, polarization-transfer, and population-transfer rates for solar helium I lines resulting from isotropic collisions with neutral hydrogen, providing essential data to improve the modeling of solar spectropolarimetry.