dc.contributor.author | Tsap Y. | |
dc.contributor.author | Nagnibeda V. | |
dc.contributor.author | Motorina G. | |
dc.contributor.author | Smirnova V. | |
dc.contributor.author | Ryzhov V. | |
dc.contributor.author | Morgachev A. | |
dc.contributor.author | Kuznetsov S. | |
dc.date.accessioned | 2022-10-27T12:19:28Z | |
dc.date.available | 2022-10-27T12:19:28Z | |
dc.identifier.uri | https://www.utupub.fi/handle/10024/157832 | |
dc.description.abstract | <p>The 5 July 2012 solar flare SOL2012-07-05T11:44 (11:39 – 11:49 UT) with an increasing millimeter spectrum between 93 and 140 GHz is considered. We use space and ground-based observations in X-ray, extreme ultraviolet, microwave, and millimeter wave ranges obtained with the <em>Reuven Ramaty High-Energy Solar Spectroscopic Imager</em>, <em>Solar Dynamics Observatory</em> (SDO), <em>Geostationary Operational Environmental Satellite</em>, <em>Radio Solar Telescope Network</em>, and <em>Bauman Moscow State Technical University millimeter</em> radio telescope RT-7.5. The main parameters of thermal and accelerated electrons were determined through X-ray spectral fitting assuming the homogeneous thermal source and thick-target model. From the data of the <em>Atmospheric Imaging Assembly</em>/SDO and differential-emission-measure calculations it is shown that the thermal coronal plasma gives a negligible contribution to the millimeter flare emission. Model calculations suggest that the observed increase of millimeter spectral flux with frequency is determined by gyrosynchrotron emission of high-energy (≳300 ≳300
keV) electrons in the chromosphere. The consequences of the results are discussed in the light of the flare-energy-release mechanisms.<br /></p> | |
dc.language.iso | en | |
dc.publisher | Springer Netherlands | |
dc.title | Millimeter and X-Ray Emission from the 5 July 2012 Solar Flare | |
dc.identifier.urn | URN:NBN:fi-fe2021042719015 | |
dc.relation.volume | 293 | |
dc.contributor.organization | fi=fysiikan ja tähtitieteen laitos, yhteiset|en=Department of Physics and Astronomy| | |
dc.contributor.organization-code | 2606700 | |
dc.converis.publication-id | 30741852 | |
dc.converis.url | https://research.utu.fi/converis/portal/Publication/30741852 | |
dc.identifier.eissn | 1573-093X | |
dc.identifier.jour-issn | 0038-0938 | |
dc.okm.affiliatedauthor | Smirnova, Victoria | |
dc.okm.discipline | 115 Astronomy and space science | en_GB |
dc.okm.discipline | 115 Avaruustieteet ja tähtitiede | fi_FI |
dc.okm.internationalcopublication | international co-publication | |
dc.okm.internationality | International publication | |
dc.okm.type | Journal article | |
dc.publisher.country | Alankomaat | fi_FI |
dc.publisher.country | Netherlands | en_GB |
dc.publisher.country-code | NL | |
dc.relation.articlenumber | 50 | |
dc.relation.doi | 10.1007/s11207-018-1269-6 | |
dc.relation.ispartofjournal | Solar Physics | |
dc.relation.issue | 3 | |
dc.year.issued | 2018 | |