Konus-Wind and Helicon-Coronas-F observations of solar flares

Pal'Shin, V.; Charikov, Yu. E.; Aptekar, R.; Golenetskii, S.; Kokomov, A.; Svinkin, D.; Sokolova, Z. Ya.; Ulanov, M.; Frederiks, D.; Tsvetkova, A. E.

doi:10.1134/s0016793214070093

Cited by 26 publications

(25 citation statements)

References 11 publications

(10 reference statements)

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“…HXR data for this event are obtained with RHESSI and Konus-Wind, and the microwave data with OVSA. RHESSI and OVSA have complementary spatial, temporal, and spectral/energy resolution, while Konus-Wind is located in the interplanetary medium, and has a highly stable background (Palʼshin et al 2014), which is helpful in eliminating complications that can arise with RHESSI's highly variable background. For example, Figure 1(d) shows that the high-energy RHESSI channels are strongly contaminated by the particle contribution from the radiation belt passage during the first peak around 17:45UT, while the Konus-Wind light curves are free from such interference.…”

Section: Observationsmentioning

confidence: 99%

Validation of the Coronal Thick Target Source Model

Fleishman

Nita

et al. 2016

ApJ

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We present detailed 3D modeling of a dense, coronal thick-target X-ray flare using the GX Simulator tool, photospheric magnetic measurements, and microwave imaging and spectroscopy data. The developed model offers a remarkable agreement between the synthesized and observed spectra and images in both X-ray and microwave domains, which validates the entire model. The flaring loop parameters are chosen to reproduce the emission measure, temperature, and the nonthermal electron distribution at low energies derived from the X-ray spectral fit, while the remaining parameters, unconstrained by the X-ray data, are selected such as to match the microwave images and total power spectra. The modeling suggests that the accelerated electrons are trapped in the coronal part of the flaring loop, but away from where the magnetic field is minimal, and, thus, demonstrates that the data are clearly inconsistent with electron magnetic trapping in the weak diffusion regime mediated by the Coulomb collisions. Thus, the modeling supports the interpretation of the coronal thick-target sources as sites of electron acceleration in flares and supplies us with a realistic 3D model with physical parameters of the acceleration region and flaring loop.

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Section: Observationsmentioning

confidence: 99%

Validation of the Coronal Thick Target Source Model

Fleishman

Nita

et al. 2016

ApJ

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“…Figures 2 and 3 present an overview of data available for this solar flare from RHESSI (Lin et al 2002), Fermi-GBM (Meegan et al 2009), Konus-Wind 7 (Pal'shin et al 2014), NoRP (Nakajima et al 1985), NoRH (Nakajima et al 1994), and Solar Dynamics Observatory (SDO; Pesnell et al 2012). Specifically, we concentrate on the first flare episode bounded by two vertical dotted lines in Figure 2, primarily because RHESSI missed the main flare, but also because the radio emission is dominated by a single source during this period, but grows more complex during the later period when the flux levels are exceptionally large, which would complicate the analysis.…”

Section: Gx Simulator Overviewmentioning

confidence: 99%

Three-Dimensional Radio and X-Ray Modeling and Data Analysis Software: Revealing Flare Complexity

Nita

Fleishman

Kuznetsov

et al. 2015

ApJ

106

104

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Many problems in solar physics require analysis of imaging data obtained in multiple wavelength domains with differing spatial resolution in a framework supplied by advanced three-dimensional (3D) physical models. To facilitate this goal, we have undertaken a major enhancement of our IDL-based simulation tools developed earlier for modeling microwave and X-ray emission. The enhanced software architecture allows the user to (1) import photospheric magnetic field maps and perform magnetic field extrapolations to generate 3D magnetic field models; (2) investigate the magnetic topology by interactively creating field lines and associated flux tubes; (3) populate the flux tubes with user-defined nonuniform thermal plasma and anisotropic, nonuniform, nonthermal electron distributions; (4) investigate the spatial and spectral properties of radio and X-ray emission calculated from the model; and (5) compare the model-derived images and spectra with observational data. The package integrates shared-object libraries containing fast gyrosynchrotron emission codes, IDL-based soft and hard X-ray codes, and potential and linear force-free field extrapolation routines. The package accepts user-defined radiation and magnetic field extrapolation plug-ins. We use this tool to analyze a relatively simple single-loop flare and use the model to constrain the magnetic 3D structure and spatial distribution of the fast electrons inside this loop. We iteratively compute multi-frequency microwave and multi-energy X-ray images from realistic magnetic flux tubes obtained from pre-flare extrapolations, and compare them with imaging data obtained by SDO, NoRH, and RHESSI. We use this event to illustrate the tool's use for the general interpretation of solar flares to address disparate problems in solar physics.

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“…During its more than 25-year-long history, the KONUS instrument onboard Wind has accumulated an unique volume of solar flare observations in the hard X-ray and gamma ray range. Data on solar flares recorded by KONUS in the triggered mode are published online (http://www.ioffe.ru/LEA/kwsun/) from 1994 to the present along with their GOES classification (Pal'shin et al, 2014). This database (see Table C1 WILSON ET AL.…”

Section: Solar Flaresmentioning

confidence: 99%

A Quarter Century of Wind Spacecraft Discoveries

Wilson

Brosius

Gopalswamy

et al. 2020

Preprint

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This document may differ from the final, published version of the research and has been made available online in accordance with publisher policies. To read and/or cite from the published version of the research, please visit the publisher's website (a subscription may be required.) The Wind MissionNASA launched the Wind spacecraft on November 1, 1994. Wind and Polar (Harten & Clark, 1995) were part of the stand-alone Global Geospace Science (GGS) Program (Acuña et al., 1995), a subset of the International Solar Terrestrial Physics (ISTP) Program (Whipple & Lancaster, 1995). The ISTP Program included the additional missions Geotail (Nishida, 1994), the SOlar and Heliospheric Observatory or SoHO (Domingo et al., 1995), and Cluster (Escoubet et al., 1997). The objective of the ISTP program was to study the origin of solar variability and activity, the transport of manifestations of that activity to the Earth via plasma processes, and the cause-and-effect relationships between that time varying energy transport and the near-earth environment.

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Konus-Wind and Helicon-Coronas-F observations of solar flares

Abstract: Results of solar flare observations obtained in the Konus-Wind experiment from

Cited by 26 publications

References 11 publications

Validation of the Coronal Thick Target Source Model

Validation of the Coronal Thick Target Source Model

Three-Dimensional Radio and X-Ray Modeling and Data Analysis Software: Revealing Flare Complexity

A Quarter Century of Wind Spacecraft Discoveries

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