The Coronal Analysis of SHocks and Waves (CASHeW) framework

Kozarev, Kamen; Davey, A. R.; Kendrick, Alexander; Hammer, Michael F.; Keith, Celeste

doi:10.1051/swsc/2017028

Cited by 13 publications

(16 citation statements)

References 55 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The advantage of our method is that we estimate the density change at all points of the shock model, not only one or several regions. This method has previously been employed in Kozarev et al (Kozarev et al, 2017). We find that the density jump based on the DEM modeling within the AIA field of view is generally quite small, predominantly below 1.2, which is consistent with many previous studies (Kozarev et al, 2015;Vanninathan et al, 2015).…”

Section: Plasma Parameters Along Individual Shock-crossing Magnetic F...supporting

confidence: 90%

“…To characterize the kinematics of CBFs, we applied to the AIA observations the methodology of the Coronal Analysis of SHocks and Waves (CASHeW) framework (Kozarev et al, 2017), updated and implemented in SPREAdFAST. Our framework estimates the CBF kinematics in a similar way to Long et al (Long et al, 2021) and Downs et al (Downs et al, 2021), by following the leading edge of the front on consecutive images.…”

Section: Cbf Kinematics and Geometric Modelingmentioning

confidence: 99%

See 1 more Smart Citation

A Multi-Event Study of Early-Stage SEP Acceleration by CME-Driven Shocks—Sun to 1 AU

Kozarev

Nedal

Miteva

et al. 2022

Front. Astron. Space Sci.

View full text Add to dashboard Cite

The solar corona between below 10 solar radii is an important region for early acceleration and transport of solar energetic particles (SEPs) by coronal mass ejection-driven shock waves. There, these waves propagate into a highly variable dynamic medium with steep gradients and rapidly expanding coronal magnetic fields, which modulates the particle acceleration near the shock/wave surfaces, and the way SEPs spread into the heliosphere. We present a study modeling the acceleration of SEPs in global coronal shock events in the corona, as well as their transport to 1 au, based on telescopic observations coupled with dynamic physical models. As part of the project Solar Particle Radiation Environment Analysis and Forecasting—Acceleration and Scattering Transport (SPREAdFAST), we model the interaction of observed off-limb coronal bright fronts (CBF) with the coronal plasma from synoptic magnetohydrodynamic (MHD) simulations. We then simulate the SEP acceleration in analytical diffusive shock acceleration (DSA) model. The simulated fluxes are used as time-dependent inner boundary conditions for modeling the particle transport to 1 au. Resulting flux time series are compared with 1 au observations for validation. We summarize our findings and present implications for nowcasting SEP acceleration and heliospheric connectivity.

show abstract

Section: Plasma Parameters Along Individual Shock-crossing Magnetic F...supporting

confidence: 90%

Section: Cbf Kinematics and Geometric Modelingmentioning

confidence: 99%

A Multi-Event Study of Early-Stage SEP Acceleration by CME-Driven Shocks—Sun to 1 AU

Kozarev

Nedal

Miteva

et al. 2022

Front. Astron. Space Sci.

View full text Add to dashboard Cite

show abstract

“…Despite these tremendous enhancements in our knowledge gained from stereoscopic observational data, still a major drawback in unraveling the SEP nature is the unknown configuration of the interplanetary magnetic field along which SEPs propagate and internal distribution (Kahler and Vourlidas 2013). Therefore, the acceleration process of SEPs seems not to be spatially limited but happens over a wide range of longitudes including transport before being injected at distant longitudes (e.g., Vlahos et al 2019;Kozarev et al 2017;Malandraki and Crosby 2018).…”

Section: Seps Observed From Multiple Viewpointsmentioning

confidence: 99%

Space weather: the solar perspective

Temmer

2021

Living Rev Sol Phys

164

View full text Add to dashboard Cite

The Sun, as an active star, is the driver of energetic phenomena that structure interplanetary space and affect planetary atmospheres. The effects of Space Weather on Earth and the solar system is of increasing importance as human spaceflight is preparing for lunar and Mars missions. This review is focusing on the solar perspective of the Space Weather relevant phenomena, coronal mass ejections (CMEs), flares, solar energetic particles (SEPs), and solar wind stream interaction regions (SIR). With the advent of the STEREO mission (launched in 2006), literally, new perspectives were provided that enabled for the first time to study coronal structures and the evolution of activity phenomena in three dimensions. New imaging capabilities, covering the entire Sun-Earth distance range, allowed to seamlessly connect CMEs and their interplanetary counterparts measured in-situ (so called ICMEs). This vastly increased our knowledge and understanding of the dynamics of interplanetary space due to solar activity and fostered the development of Space Weather forecasting models. Moreover, we are facing challenging times gathering new data from two extraordinary missions, NASA’s Parker Solar Probe (launched in 2018) and ESA’s Solar Orbiter (launched in 2020), that will in the near future provide more detailed insight into the solar wind evolution and image CMEs from view points never approached before. The current review builds upon the Living Reviews article by Schwenn from 2006, updating on the Space Weather relevant CME-flare-SEP phenomena from the solar perspective, as observed from multiple viewpoints and their concomitant solar surface signatures.

show abstract

“…Better coronal models will improve our computations of shock properties and provide more reliable estimates of the magnetic connectivity between the shock and the energetic particle detectors Rodríguez-Pacheco et al (2019). To this end, the 3D shock triangulation codes (e.g., Kwon et al 2014) readily available in SolarSoft and the Coronal Analysis of SHocks and Waves (CASHeW) framework (Kozarev et al 2017), compatible with SolarSoft routines will be modified to naturally include these new viewpoints. Remote observations from Solar Orbiter will also enable a more accurate geometrical characterization of coronal and interplanetary shocks, so that non-radial propagation and small-scale structure of the fronts may be accounted for.…”

Section: Investigations On the Properties And Origin(s) Of Sepsmentioning

confidence: 99%

Models and data analysis tools for the Solar Orbiter mission

Rouillard

Pinto

Vourlidas

et al. 2020

A&A

View full text Add to dashboard Cite

Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in-situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency (ESA)'s Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our proc...

show abstract

The Coronal Analysis of SHocks and Waves (CASHeW) framework

Cited by 13 publications

References 55 publications

A Multi-Event Study of Early-Stage SEP Acceleration by CME-Driven Shocks—Sun to 1 AU

A Multi-Event Study of Early-Stage SEP Acceleration by CME-Driven Shocks—Sun to 1 AU

Space weather: the solar perspective

Models and data analysis tools for the Solar Orbiter mission

Contact Info

Product

Resources

About