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Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations. / Stupishin, A. G.; Kaltman, T. I.; Bogod, V. M.; Yasnov, L. V.

в: Solar Physics, Том 293, № 1, 13, 01.2018.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Stupishin, AG, Kaltman, TI, Bogod, VM & Yasnov, LV 2018, 'Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations', Solar Physics, Том. 293, № 1, 13. https://doi.org/10.1007/s11207-017-1228-7

APA

Stupishin, A. G., Kaltman, T. I., Bogod, V. M., & Yasnov, L. V. (2018). Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations. Solar Physics, 293(1), [13]. https://doi.org/10.1007/s11207-017-1228-7

Vancouver

Stupishin AG, Kaltman TI, Bogod VM, Yasnov LV. Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations. Solar Physics. 2018 Янв.;293(1). 13. https://doi.org/10.1007/s11207-017-1228-7

Author

Stupishin, A. G. ; Kaltman, T. I. ; Bogod, V. M. ; Yasnov, L. V. / Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations. в: Solar Physics. 2018 ; Том 293, № 1.

BibTeX

@article{517350ecb28f43a78b572b320583d69c,
title = "Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations",
abstract = "Models of the upper transition region of sunspots have been derived based on the observed radio spectrum between 3 and 18 GHz from Radio Astronomical Telescope of the Academy of Sciences 600 (RATAN-600) observations. Our objective is to match the spectrum to show that, within the limits of the one-dimensional observations and modeling, we have obtained a reasonable description of the upper transition-region structure of sunspots. We have developed a diagnostic method, based on iterative correction of the temperature-height profile in the transition region and lower corona, and applied it to three selected active regions with unipolar gyroresonance sources. Good agreement is achieved between observed and modeled microwave spectra using one-dimensional, time-independent models in hydrostatic equilibrium characterized by a given temperature as a function of height. We found that above sunspots the upper height of a transition region is located at 2-2.3 Mm, and the temperature of the low corona is about 1.5-2.5 MK.",
keywords = "Sunspot, Atmosphere model, Microwave observations, Gyroresonance emission, Magnetic field extrapolations, Radiative transfer equation, Polarization, SLOWLY CHANGING COMPONENT, MAGNETIC-FIELD, ACTIVE REGIONS, PHYSICAL CONDITIONS, TRANSITION REGION, RADIO TELESCOPE, EMISSION, COMPUTATION, RESOLUTION, SPECTRUM",
author = "Stupishin, {A. G.} and Kaltman, {T. I.} and Bogod, {V. M.} and Yasnov, {L. V.}",
year = "2018",
month = jan,
doi = "10.1007/s11207-017-1228-7",
language = "English",
volume = "293",
journal = "Solar Physics",
issn = "0038-0938",
publisher = "Springer Nature",
number = "1",

}

RIS

TY - JOUR

T1 - Modeling of Solar Atmosphere Parameters Above Sunspots Using RATAN-600 Microwave Observations

AU - Stupishin, A. G.

AU - Kaltman, T. I.

AU - Bogod, V. M.

AU - Yasnov, L. V.

PY - 2018/1

Y1 - 2018/1

N2 - Models of the upper transition region of sunspots have been derived based on the observed radio spectrum between 3 and 18 GHz from Radio Astronomical Telescope of the Academy of Sciences 600 (RATAN-600) observations. Our objective is to match the spectrum to show that, within the limits of the one-dimensional observations and modeling, we have obtained a reasonable description of the upper transition-region structure of sunspots. We have developed a diagnostic method, based on iterative correction of the temperature-height profile in the transition region and lower corona, and applied it to three selected active regions with unipolar gyroresonance sources. Good agreement is achieved between observed and modeled microwave spectra using one-dimensional, time-independent models in hydrostatic equilibrium characterized by a given temperature as a function of height. We found that above sunspots the upper height of a transition region is located at 2-2.3 Mm, and the temperature of the low corona is about 1.5-2.5 MK.

AB - Models of the upper transition region of sunspots have been derived based on the observed radio spectrum between 3 and 18 GHz from Radio Astronomical Telescope of the Academy of Sciences 600 (RATAN-600) observations. Our objective is to match the spectrum to show that, within the limits of the one-dimensional observations and modeling, we have obtained a reasonable description of the upper transition-region structure of sunspots. We have developed a diagnostic method, based on iterative correction of the temperature-height profile in the transition region and lower corona, and applied it to three selected active regions with unipolar gyroresonance sources. Good agreement is achieved between observed and modeled microwave spectra using one-dimensional, time-independent models in hydrostatic equilibrium characterized by a given temperature as a function of height. We found that above sunspots the upper height of a transition region is located at 2-2.3 Mm, and the temperature of the low corona is about 1.5-2.5 MK.

KW - Sunspot

KW - Atmosphere model

KW - Microwave observations

KW - Gyroresonance emission

KW - Magnetic field extrapolations

KW - Radiative transfer equation

KW - Polarization

KW - SLOWLY CHANGING COMPONENT

KW - MAGNETIC-FIELD

KW - ACTIVE REGIONS

KW - PHYSICAL CONDITIONS

KW - TRANSITION REGION

KW - RADIO TELESCOPE

KW - EMISSION

KW - COMPUTATION

KW - RESOLUTION

KW - SPECTRUM

UR - http://www.scopus.com/inward/record.url?scp=85040329178&partnerID=8YFLogxK

U2 - 10.1007/s11207-017-1228-7

DO - 10.1007/s11207-017-1228-7

M3 - Article

VL - 293

JO - Solar Physics

JF - Solar Physics

SN - 0038-0938

IS - 1

M1 - 13

ER -

ID: 36346509