scholarly journals Diagnostics of plasma jets in the solar corona

2021 ◽  
Vol 7 (2) ◽  
pp. 3-10
Author(s):  
Sergey Anfinogentov ◽  
Tatyana Kaltman ◽  
Alexey Stupishin ◽  
Valery Nakariakov ◽  
Maria Lukitcheva
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Extreme Ultraviolet ◽  
Three Dimensional ◽  
Statistical Processing ◽  
Coronal Magnetic Field ◽  
Plasma Jets ◽  
Dimensional Structure ◽  
Lower Corona ◽  
Diagnostic Capabilities

The paper discusses the diagnostics of plasma jets in the solar corona with the use of data from modern space- and ground-based telescopes observing the Sun in the extreme ultraviolet (EUV) and micro- wave bands. We examine observational parameters of EUV and radio emission in events associated with plasma jets, depending on the mechanism of formation, initiation conditions, and evolution of the jets. The opportunities provided by the study of plasma jets, which relies on simultaneous observations in different bands, are highlighted. For a number of jets, we have measured their primary parameters; and in this paper we present preliminary results of statistical processing of the data obtained. Microwave observations of several specific events, made by ground-based instruments RATAN-600, SRH, and Nobeyama Radioheliograph, are considered in detail. The diagnostic capabilities of these instruments for studying coronal jets are shown. To analyze the three-dimensional structure of the coronal magnetic field, we have used SDO/HMI data, which allowed for the reconstruction of the field in the lower corona. The information gained is compared with the results of diagnostics of the magnetic field at the base of the corona according to RATAN-600 data. The purpose of the methods developed is to determine the physical mechanisms responsible for the generation, collimation, and dynamics of plasma jets in the solar atmosphere.

scholarly journals Diagnostics of plasma jets in the solar corona

2021 ◽  
Vol 7 (2) ◽  
pp. 3-11
Author(s):  
Sergey Anfinogentov ◽  
Tatyana Kaltman ◽  
Alexey Stupishin ◽  
Valery Nakariakov ◽  
Maria Lukitcheva
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Extreme Ultraviolet ◽  
Three Dimensional ◽  
Statistical Processing ◽  
Coronal Magnetic Field ◽  
Plasma Jets ◽  
Dimensional Structure ◽  
Lower Corona ◽  
Diagnostic Capabilities

The paper discusses the diagnostics of plasma jets in the solar corona with the use of data from modern space- and ground-based telescopes observing the Sun in the extreme ultraviolet (EUV) and micro- wave bands. We examine observational parameters of EUV and radio emission in events associated with plasma jets, depending on the mechanism of formation, initiation conditions, and evolution of the jets. The opportunities provided by the study of plasma jets, which relies on simultaneous observations in different bands, are highlighted. For a number of jets, we have measured their primary parameters; and in this paper we present preliminary results of statistical processing of the data obtained. Microwave observations of several specific events, made by ground-based instruments RATAN-600, SRH, and Nobeyama Radioheliograph, are considered in detail. The diagnostic capabilities of these instruments for studying coronal jets are shown. To analyze the three-dimensional structure of the coronal magnetic field, we have used SDO/HMI data, which allowed for the reconstruction of the field in the lower corona. The information gained is compared with the results of diagnostics of the magnetic field at the base of the corona according to RATAN-600 data. The purpose of the methods developed is to determine the physical mechanisms responsible for the generation, collimation, and dynamics of plasma jets in the solar atmosphere.

scholarly journals Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval

2009 ◽  
Vol 5 (H15) ◽  
pp. 491-493 ◽  
Author(s):  
Pete Riley ◽  
Jon A. Linker ◽  
Zoran Mikic
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Extreme Ultraviolet ◽  
Plasma Temperature ◽  
Transport Processes ◽  
Coronal Heating ◽  
Dimensional Structure ◽  
Plasma Parameters ◽  
Whole Heliosphere Interval ◽  
Inner Heliosphere

AbstractWith the goal of understanding the three-dimensional structure of the solar corona and inner heliosphere during the “Whole Heliosphere Interval” (WHI), we have developed a global MHD solution for Carrington rotation (CR) 2068. Our model, which includes energy transport processes, such as coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and the effects of Alfvén waves, is capable of producing significantly better estimates of the plasma temperature and density in the corona than have been possible in the past. With such a model, we can compute emission in extreme ultraviolet (EUV) and X-ray wavelengths, as well as scattering in polarized white light. Additionally, from our heliospheric solutions, we can deduce magnetic field and plasma parameters along specific spacecraft trajectories. We have made detailed comparisons of both remote solar and in situ observations with the model results, allowing us to: (1) Connect these disparate sets of observations; (2) Infer the global structure of the inner heliosphere; and (3) Provide support for (or against) assumptions in the MHD model, such as the empirically-based coronal heating profiles.

scholarly journals A three-dimensional velocity of an erupting prominence prior to a coronal mass ejection

2021 ◽  
Vol 73 (2) ◽  
pp. 394-404
Author(s):  
Maria V Gutierrez ◽  
Kenichi Otsuji ◽  
Ayumi Asai ◽  
Raul Terrazas ◽  
Mutsumi Ishitsuka ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Extreme Ultraviolet ◽  
Three Dimensional ◽  
Coronal Magnetic Field ◽  
Coronal Loops ◽  
Active Region Noaa ◽  
Loop Expansion ◽  
Mass Ejection ◽  
Multiple Interactions ◽  
Full Disk

Abstract We present a detailed three-dimensional (3D) view of a prominence eruption, coronal loop expansion, and coronal mass ejections (CMEs) associated with an M4.4 flare that occurred on 2011 March 8 in the active region NOAA 11165. Full-disk Hα images of the flare and filament ejection were successfully obtained by the Flare Monitoring Telescope (FMT) following its relocation to Ica University, Peru. Multiwavelength observation around the Hα line enabled us to derive the 3D velocity field of the Hα prominence eruption. Features in extreme ultraviolet were also obtained by the Atmospheric Imager Assembly onboard the Solar Dynamic Observatory and the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory - Ahead satellite. We found that, following collision of the erupted filament with the coronal magnetic field, some coronal loops began to expand, leading to the growth of a clear CME. We also discuss the succeeding activities of CME driven by multiple interactions between the expanding loops and the surrounding coronal magnetic field.

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

Radio Measurements of Coronal Magnetic Fields

1994 ◽  
Vol 144 ◽  
pp. 21-28 ◽  
Author(s):  
G. B. Gelfreikh
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Active Regions ◽  
High Sensitivity ◽  
Coronal Magnetic Field ◽  
Transverse Magnetic ◽  
Radio Sources ◽  
Radio Waves ◽  
Solar Active Regions

AbstractA review of methods of measuring magnetic fields in the solar corona using spectral-polarization observations at microwaves with high spatial resolution is presented. The methods are based on the theory of thermal bremsstrahlung, thermal cyclotron emission, propagation of radio waves in quasi-transverse magnetic field and Faraday rotation of the plane of polarization. The most explicit program of measurements of magnetic fields in the atmosphere of solar active regions has been carried out using radio observations performed on the large reflector radio telescope of the Russian Academy of Sciences — RATAN-600. This proved possible due to good wavelength coverage, multichannel spectrographs observations and high sensitivity to polarization of the instrument. Besides direct measurements of the strength of the magnetic fields in some cases the peculiar parameters of radio sources, such as very steep spectra and high brightness temperatures provide some information on a very complicated local structure of the coronal magnetic field. Of special interest are the results found from combined RATAN-600 and large antennas of aperture synthesis (VLA and WSRT), the latter giving more detailed information on twodimensional structure of radio sources. The bulk of the data obtained allows us to investigate themagnetospheresof the solar active regions as the space in the solar corona where the structures and physical processes are controlled both by the photospheric/underphotospheric currents and surrounding “quiet” corona.

THREE-DIMENSIONAL STRUCTURE AND EVOLUTION OF EXTREME-ULTRAVIOLET BRIGHT POINTS OBSERVED BYSTEREO/SECCHI/EUVI

2012 ◽  
Vol 757 (2) ◽  
pp. 167 ◽  
Author(s):  
Ryun-Young Kwon ◽  
Jongchul Chae ◽  
Joseph M. Davila ◽  
Jie Zhang ◽  
Yong-Jae Moon ◽  
...  
Keyword(s):  
Extreme Ultraviolet ◽  
Three Dimensional ◽  
Dimensional Structure ◽  
Three Dimensional Structure

scholarly journals Eclipse mapping at X-ray wavelengths

1996 ◽  
Vol 176 ◽  
pp. 85-94 ◽  
Author(s):  
J.H.M.M. Schmitt
Keyword(s):  
Solar Corona ◽  
Binary Systems ◽  
Three Dimensional ◽  
Dimensional Structure ◽  
Similar Amount ◽  
Inversion Problem ◽  
X Ray ◽  
Three Dimensional Structure ◽  
Spatially Resolved ◽  
Rotational Modulation

Stellar coronae cannot be spatially resolved, and yet stellar coronae are likely to exhibit a similar amount of structure as the solar corona. Currently, the only way to infer structure from spatially unresolved data is to look for rotational modulation of the X-ray emission or eclipses in the case of binary systems. I will discuss some of the observations obtained and critically review the methods used to infer structure from these data. Particular emphasis will be placed on the ill-conditioned nature of the inversion problem, that makes it next to impossible to infer the possibly three-dimensional structure of stellar coronae.

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