Multiwave Siberian Radioheliograph

Altyntsev, A. T.; Lesovoi, Sergey; Глоба, Мария; Gubin, Aleksey; Kochanov, A. A.; Grechnev, V. V.; Ivanov, E.; Кобец, Вероника; Meshalkina, N. S.; Muratov, Anatoliy; Prosovetsky, D. V.; Myshyakov, I. I.; Uralov, A. M.; Fedotova, Anastasiya

doi:10.12737/stp-62202003

Cited by 31 publications

(10 citation statements)

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…SRH consists of three T-shaped antenna arrays (Fig. 1) operating in the frequency ranges [3][4][5][6][6][7][8][9][10][11][12][12][13][14][15][16][17][18][19][20][21][22][23][24]). Arrays 3-6 are oriented in the east-west-north direction, and arrays 6-12 and 12-24 are oriented in the east-west-south direction.…”

Section: Srh Descriptionmentioning

confidence: 99%

Microwave imaging spectroscopy of the solar corona

Lesovoi¹,

Глоба²,

Gubin³

et al. 2022

Proceedings of the Multifaceted Universe: Theory and Observations - 2022 — PoS(MUTO2022)

Self Cite

View full text Add to dashboard Cite

The study of the solar corona plays a key role in understanding solar activity. Microwave imaging spectroscopy -measuring microwave spectra at every point on the solar disk (or image) -is the most promising method for studying the lower corona and the chromosphere-corona transition region. Solar microwave emission originates in the low corona and in the upper chromosphere and is produced both by thermal and non-thermal electrons. The main types of emission are bremsstrahlung, gyroresonance and gyrosynchrotron emission. The quiet Sun emission is dominated by the bremsstrahlung while the active region emission is due to the gyroresonance mechanism. The gyrosynchrotron emission is generated by non-thermal electrons during solar flares. Microwave emission spectra allow us to estimate the temperature and density of the plasma in active regions. Microwave spectroscopy of the solar corona is perhaps the only method for measuring the coronal magnetic field both for the quiet Sun and for transient events. The Siberian Radioheliograph (SRH), a new generation solar radio telescope, is described, and the first observations of solar activity in the broadband frequency range 3-24 GHz are presented. The estimation of the magnetic field scale length is presented. The scale length was estimated by using the SRH data -spectra of an active region emission in the frequency range 3-12 GHz.

show abstract

Section: Srh Descriptionmentioning

confidence: 99%

Microwave imaging spectroscopy of the solar corona

Lesovoi¹,

Глоба²,

Gubin³

et al. 2022

Proceedings of the Multifaceted Universe: Theory and Observations - 2022 — PoS(MUTO2022)

Self Cite

View full text Add to dashboard Cite

show abstract

“…WSRT observed NLSs at 5 GHz; VLA, at 4.9, 8.4, and 15 GHz; SSRT, at 5.7 GHz; RATAN-600, at several frequencies; NoRH, at 17 GHz and in one case even at 34 GHz. Results of these studies have been discussed in several papers [Kundu, Velusamy, 1980;Kundu et al, 1981;Strong et al, 1984;Gelfreikh, 1985;Akhmedov et al, 1986;Chiuderi Drago et al, 1987;Borovik et al, 1989;Vatrushin, Korzhavin, 1989;Sych et al, 1993;Uralov et al, 1996Uralov et al, , 1998Uralov et al, , 2000Uralov et al, , 2006aUralov et al, , 2006bUralov et al, , 2007Uralov et al, , 2008Lee et al, 1997;Rudenko et al, 2007;Bogod et al, 2012;Yasnov, 2014;Abramov-Maximov et al, 2015;Kuznetsov et al, 2016;Bakunina et al, 2017;Zaitsev, 2019].…”

Section: Introductionmentioning

confidence: 99%

Microwave indicator of potential geoeffectiveness and magnetic flux-rope structure of a solar active region

Kudriavtseva

Myshyakov

Uralov

et al. 2021

Solar-Terrestrial Physics

Self Cite

View full text Add to dashboard Cite

We analyze the presence of a microwave neutral-line-associated source (NLS) in a super-active region NOAA 12673, which produced a number of geo-effective events in September 2017. To estimate the NLS position, we use data from the Siberian Radioheliograph in a range 4–8 GHz and from the Nobeyama Radioheliograph at 17 GHz. Calculation of the coronal magnetic field in a non-linear force-free approximation has revealed an extended structure consisting of interconnected magnetic flux ropes, located practically along the entire length of the main polarity separation line of the photospheric magnetic field. NLS is projected into the region of the strongest horizontal magnetic field, where the main energy of this structure is concentrated. During each X-class flare, the active region lost magnetic helicity and became a CME source.

show abstract

“…These data come from space missions, e.g., Helioseismic and Magnetic Imager (HMI;Scherrer et al 2012) on board the Solar Dynamic Observatory (SDO; Pesnell et al 2012), as well as ground-based high-resolution optical and infrared (IR) instruments such as Goode Solar Telescope (GST; Cao et al 2010;Goode & Cao 2012) and Daniel K. Inouye Solar Telescope (DKIST; Rimmele et al 2010;Tritschler et al 2016). Fundamental enhancements of theory and modeling are demanded in order to fully exploit new microwave and millimeter-wave imaging spectropolarimetry data from the Expanded Owens Valley Solar Array (EOVSA; Nita et al 2016;Gary et al 2018), the Siberian Radio Heliograph (SRH; Lesovoi et al 2017;Altyntsev et al 2020), and the Atacama Large Millimeter/submillimeter Array (ALMA), in addition to more traditional radio, X-ray, and EUV data, e.g., from the Nobeyama Radioheliograph (Nakajima et al 1994), Submillimeter Solar Telescope (Kaufmann et al 2001), RHESSI (Lin et al 2003), the Atmospheric Imaging Assembly (AIA; Lemen et al 2012) on board SDO, or the Spectrometer/Telescope for Imaging X-rays (STIX; Krucker et al 2020). Dynamic solar phenomena that constitute solar activity either occur in or are sensitive to the physical conditions in the solar corona.…”

Section: Introductionmentioning

confidence: 99%

Data-constrained Solar Modeling with GX Simulator

Nita

Fleishman

Kuznetsov

et al. 2023

ApJS

View full text Add to dashboard Cite

To facilitate the study of solar flares and active regions, we have created a modeling framework, the freely distributed GX Simulator IDL package, that combines 3D magnetic and plasma structures with thermal and nonthermal models of the chromosphere, transition region, and corona. Its object-based modular architecture, which runs on Windows, Mac, and Unix/Linux platforms, offers the ability to either import 3D density and temperature distribution models, or to assign numerically defined coronal or chromospheric temperatures and densities, or their distributions, to each individual voxel. GX Simulator can apply parametric heating models involving average properties of the magnetic field lines crossing a given voxel, as well as compute and investigate the spatial and spectral properties of radio, (sub)millimeter, EUV, and X-ray emissions calculated from the model, and quantitatively compare them with observations. The package includes a fully automatic model production pipeline that, based on minimal users input, downloads the required SDO/HMI vector magnetic field data, performs potential or nonlinear force-free field extrapolations, populates the magnetic field skeleton with parameterized heated plasma coronal models that assume either steady-state or impulsive plasma heating, and generates non-LTE density and temperature distribution models of the chromosphere that are constrained by photospheric measurements. The standardized models produced by this pipeline may be further customized through specialized IDL scripts, or a set of interactive tools provided by the graphical user interface. Here, we describe the GX Simulator framework and its applications.

show abstract

Multiwave Siberian Radioheliograph

Cited by 31 publications

References 52 publications

Microwave imaging spectroscopy of the solar corona

Microwave imaging spectroscopy of the solar corona

Microwave indicator of potential geoeffectiveness and magnetic flux-rope structure of a solar active region

Data-constrained Solar Modeling with GX Simulator

Contact Info

Product

Resources

About