55 research outputs found
Solar Energetic Particles in the Inner Heliosphere: Status and Open Questions
Solar energetic particle (SEP) events are related to both solar flares and coronal mass ejections (CMEs) and they present energy spectra that span from a few keV up to several GeV. A wealth of observations from widely distributed spacecraft have revealed that SEPs fill very broad regions of the heliosphere, often all around the Sun. High energy SEPs can sometimes be energetic enough to penetrate all the way down to the surface of the Earth and thus be recorded on the ground as ground level enhancements (GLEs). The conditions of the radiation environment are currently unpredictable due to an as-yet incomplete understanding of solar eruptions and their corresponding relation to SEP events. This is because the complex nature and the interplay of the injection, acceleration and transport processes undergone by the SEPs in the solar corona and the interplanetary space prevent us from establishing an accurate understanding (based on observations and modelling). In this work, we review the current status of knowledge on SEPs, focusing on GLEs and multi-spacecraft events. We extensively discuss the forecasting and nowcasting efforts of SEPs, dividing these into three categories. Finally, we report on the current open questions and the possible direction of future research efforts. This article is part of the theme issue Solar eruptions and their space weather impact
On the variability of the slow solar wind: New insights from the modelling and PSP-WISPR observations
We analyse the signature and origin of transient structures embedded in the
slow solar wind, and observed by the Wide-Field Imager for Parker Solar Probe
(WISPR) during its first 10 passages close to the Sun. WISPR provides a new
in-depth vision on these structures, which have long been speculated to be a
remnant of the pinch-off magnetic reconnection occurring at the tip of helmet
streamers. We pursue the previous modelling works of Reville (2020b, 2022) that
simulate the dynamic release of quasi-periodic density structures into the slow
wind through a tearing-induced magnetic reconnection at the tip of helmet
streamers. Synthetic WISPR white-light (WL) images are produced using a newly
developed advanced forward modelling algorithm, that includes an adaptive grid
refinement to resolve the smallest transient structures in the simulations. We
analyse the aspect and properties of the simulated WL signatures in several
case studies, typical of solar minimum and near-maximum configurations.
Quasi-periodic density structures associated with small-scale magnetic flux
ropes are formed by tearing-induced magnetic reconnection at the heliospheric
current sheet and within 3-7Rs. Their appearance in WL images is greatly
affected by the shape of the streamer belt and the presence of
pseudo-streamers. The simulations show periodicities on the ~90-180min, ~7-10hr
and ~25-50hr timescales, which are compatible with WISPR and past observations.
This work shows strong evidence for a tearing-induced magnetic reconnection
contributing to the long-observed high variability of the slow solar wind.Comment: 23 pages, 14 figures, to appear in Astronomy & Astrophysics,
associated movies available at https://doi.org/10.5281/zenodo.813559
Parametric study of the kinematic evolution of coronal mass ejection shock waves and their relation to flaring activity
Coronal and interplanetary shock waves produced by coronal mass ejections
(CMEs) are major drivers of space-weather phenomena, inducing major changes in
the heliospheric radiation environment and directly perturbing the near-Earth
environment, including its magnetosphere. A better understanding of how these
shock waves evolve from the corona to the interplanetary medium can therefore
contribute to improving nowcasting and forecasting of space weather. Early
warnings from these shock waves can come from radio measurements as well as
coronagraphic observations that can be exploited to characterise the dynamical
evolution of these structures. Our aim is to analyse the geometrical and
kinematic properties of 32 CME shock waves derived from multi-point white-light
and ultraviolet imagery taken by the Solar Dynamics Observatory (SDO), Solar
and Heliospheric Observatory (SoHO), and Solar-Terrestrial Relations
Observatory (STEREO) to improve our understanding of how shock waves evolve in
3D during the eruption of a CME. We use our catalogue to search for relations
between the shock wave's kinematic properties and the flaring activity
associated with the underlying genesis of the CME piston. Past studies have
shown that shock waves observed from multiple vantage points can be aptly
reproduced geometrically by simple ellipsoids. The catalogue of reconstructed
shock waves provides the time-dependent evolution of these ellipsoidal
parameters. From these parameters, we deduced the lateral and radial expansion
speeds of the shocks evolving over time. We compared these kinematic properties
with those obtained from a single viewpoint by SoHO in order to evaluate
projection effects. Finally, we examined the relationships between the shock
wave and the associated flare when the latter was observed on the disc by
considering the measurements of soft and hard X-rays.Comment: 11 pages, 12 figures, accepted for publication in A&
On the Role of Coronal Shocks for Accelerating Solar Energetic Electrons
We study the role of coronal mass ejection (CME) driven shocks in the acceleration of solar energetic electrons. Using observations by the two STEREO spacecraft, we correlate electron peak intensities of solar energetic particle events measured in situ with various parameters of the associated coronal shocks. These shock parameters were derived by combining 3D shock reconstructions with global modeling of the corona. This modeling technique provides also shock properties in the specific shock regions that are magnetically connected to the two STEREO spacecraft. We find significant correlations between the peak intensities and the Mach number of the shock with correlation coefficients of about 0.7, which are similar for electrons at similar to 1 MeV and protons at >60 MeV. Lower-energy electrons with <100 keV show a smaller correlation coefficient of 0.47. The causal relationship between electron intensities and the shock properties is supported by the vanishing correlations when peak intensities at STEREO A are related with the Alfvenic Mach number at the magnetic footpoint of STEREO B and vice versa, which yields correlation coefficients of 0.03 and -0.13 for similar to 1 MeV and <100 keV electron peak intensities, respectively. We conclude that the high-energy electrons are accelerated mainly by the shock, while the low-energy electrons are likely produced by a mixture of flare and shock-related acceleration processes
The Solar Origin of Particle Events Measured by Parker Solar Probe
During the second solar encounter phase of Parker Solar Probe (PSP), two small solar energetic particle (SEP) events were observed by the Integrated Science Investigation of the Sun, on 2019 April 2 and 4. At the time, PSP was approaching its second perihelion at a distance of ~24.8 million kilometers from the solar center, it was in near-radial alignment with STEREO-A and in quadrature with Earth. During the two SEP events multiple narrow ejections and a streamer-blowout coronal mass ejection (SBO-CME) originated from a solar region situated eastward of PSP. We analyze remote-sensing observations of the solar corona, and model the different eruptions and how PSP was connected magnetically to the solar atmosphere to determine the possible origin of the two SEP events. We find that the SEP event on April 2 was associated with the two homologous ejections from active region 12738 that included two surges and EUV waves occurring in quick succession. The EUV waves appear to merge and were fast enough to form a shock in the low corona. We show that the April 4 SEP event originates in the SBO-CME. Our modeling work suggests that formation of a weak shock is likely for this CME
PyThea: An open-source software package to perform 3D reconstruction of coronal mass ejections and shock waves
PyThea is a newly developed open-source Python software package that provides tools to reconstruct coronal mass ejections (CMEs) and shocks waves in three dimensions, using multi-spacecraft remote-sensing observations. In this article, we introduce PyThea to the scientific community and provide an overview of the main functionality of the core software package and the web application. This package has been fully built in Python, with extensive use of libraries available within this language ecosystem. PyThea package provides a web application that can be used to reconstruct CMEs and shock waves. The application automatically retrieves and processes remote-sensing observations, and visualizes the imaging data that can be used for the analysis. Thanks to PyThea, the three-dimensional reconstruction of CMEs and shock waves is an easy task, with final products ready for publication. The package provides three widely used geometrical models for the reconstruction of CMEs and shocks, namely, the graduated cylindrical shell (GCS) and an ellipsoid/spheroid model. It also provides tools to process the final fittings and calculate the kinematics. The final fitting products can also be exported and reused at any time. The source code of PyThea package can be found in GitHub and Zenodo under the GNU General Public License v3.0. In this article, we present details for PyThea‘s python package structure and its core functionality, and we show how this can be used to perform three-dimensional reconstruction of coronal mass ejections and shock waves.</p
Modelling two Energetic Storm Particle Events Observed by Solar Orbiter Using the Combined EUHFORIA and iPATH Models
By coupling the EUropean Heliospheric FORcasting Information Asset (EUHFORIA)
and the improved Particle Acceleration and Transport in the Heliosphere (iPATH)
model, two energetic storm particle (ESP) events, originating from the same
active region (AR 13088) and observed by Solar Orbiter (SolO) on August 31 2022
and September 05 2022, are modelled. While both events originated from the same
active region, they exhibited notable differences, including: 1) the August ESP
event lasted for 7 hours, while the September event persisted for 16 hours; 2)
The time intensity profiles for the September event showed a clear cross-over
upstream of the shock where the intensity of higher energy protons exceeds
those of lower energy protons, leading to positive (``reverse'') spectral
indices prior to the shock passage. For both events, our simulations replicate
the observed duration of the shock sheath, depending on the deceleration
history of the CME. Imposing different choices of escaping length scale, which
is related to the decay of upstream turbulence, the modelled time intensity
profiles prior to the shock arrival also agree with observations. In
particular, the cross-over of this time profile in the September event is well
reproduced. We show that a ``reverse'' upstream spectrum is the result of the
interplay between two length scales. One characterizes the decay of upstream
shock accelerated particles, which are controlled by the energy-dependent
diffusion coefficient, and the other characterizes the decay of upstream
turbulence power, which is related to the process of how streaming protons
upstream of the shock excite Alfv\'{e}n waves. Simulations taking into account
real-time background solar wind, the dynamics of the CME propagation, and
upstream turbulence at the shock front are necessary to thoroughly understand
the ESP phase of large SEP events.Comment: Accepted by A&A. 16 pages, 11 figure
HelioCast: heliospheric forecasting based on white-light observations of the solar corona. I. Solar minimum conditions
We present a new 3D MHD heliospheric model for space-weather forecasting
driven by boundary conditions defined from white-light observations of the
solar corona. The model is based on the MHD code PLUTO, constrained by an
empirical derivation of the solar wind background properties at 0.1au. This
empirical method uses white-light observations to estimate the position of the
heliospheric current sheet. The boundary conditions necessary to run HelioCast
are then defined from pre-defined relations between the necessary MHD
properties (speed, density and temperature) and the distance to the current
sheet. We assess the accuracy of the model over six Carrington rotations during
the first semester of 2018. Using point-by-point metrics and event based
analysis, we evaluate the performances of our model varying the angular width
of the slow solar wind layer surrounding the heliospheric current sheet. We
also compare our empirical technique with two well tested models of the corona:
Multi-VP and WindPredict-AW. We find that our method is well suited to
reproduce high speed streams, and does -- for well chosen parameters -- better
than full MHD models. The model shows, nonetheless, limitations that could
worsen for rising and maximum solar activity.Comment: Accepted for publication in the Journal of Space Weather and Space
Climate. 23 pages, 12 figures. The model runs live at
http://heliocast.irap.omp.eu
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