Origin of the 30 THz Emission Detected During the Solar Flare on 2012 March 13 at 17:20 UT
Solar observations in the infrared domain can bring important clues on the response of the low solar atmosphere to primary energy released during flares. At present, the infrared continuum has been detected at 30 THz (10 μm) in only a few flares. SOL2012-03-13, which is one of these flares, has been...
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Springer Netherlands
2015
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| LEADER | 13474caa a22010817a 4500 | ||
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| 001 | PAPER-24635 | ||
| 003 | AR-BaUEN | ||
| 005 | 20230518205631.0 | ||
| 008 | 190411s2015 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-84947495707 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Trottet, G. | |
| 245 | 1 | 0 | |a Origin of the 30 THz Emission Detected During the Solar Flare on 2012 March 13 at 17:20 UT |
| 260 | |b Springer Netherlands |c 2015 | ||
| 270 | 1 | 0 | |m Raulin, J.-P.; CRAAM Universidade Presbiteriana MackenzieBrazil |
| 506 | |2 openaire |e Política editorial | ||
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| 520 | 3 | |a Solar observations in the infrared domain can bring important clues on the response of the low solar atmosphere to primary energy released during flares. At present, the infrared continuum has been detected at 30 THz (10 μm) in only a few flares. SOL2012-03-13, which is one of these flares, has been presented and discussed in Kaufmann et al. (Astrophys. J.768, 134, 2013). No firm conclusions were drawn on the origin of the mid-infrared radiation. In this work we present a detailed multi-frequency analysis of the SOL2012-03-13 event, including observations at radio-millimeter and submillimeter wavelengths, in hard X-rays (HXR), gamma-rays (GR), Hα, and white light. The HXR/GR spectral analysis shows that SOL2012-03-13 is a GR line flare and allows estimating the numbers of and energy contents in electrons, protons, and α particles produced during the flare. The energy spectrum of the electrons producing the HXR/GR continuum is consistent with a broken power-law with an energy break at (Formula presented.). We show that the high-energy part ((Formula presented.)) of this distribution is responsible for the high-frequency radio emission ((Formula presented.)) detected during the flare. By comparing the 30 THz emission expected from semi-empirical and time-independent models of the quiet and flare atmospheres, we find that most ((Formula presented.)) of the observed 30 THz radiation can be attributed to thermal free–free emission of an optically thin source. Using the F2 flare atmospheric model (Machado et al. in Astrophys. J.242, 336, 1980), this thin source is found to be at temperatures T (Formula presented.) and is located well above the minimum temperature region. We argue that the chromospheric heating, which results in 80 % of the 30 THz excess radiation, can be due to energy deposition by nonthermal flare-accelerated electrons, protons, and α particles. The remaining 20 % of the 30 THz excess emission is found to be radiated from an optically thick atmospheric layer at T (Formula presented.), below the temperature minimum region, where direct heating by nonthermal particles is insufficient to account for the observed infrared radiation. © 2015, Springer Science+Business Media Dordrecht. |l eng | |
| 536 | |a Detalles de la financiación: Consejo Nacional de Ciencia y Tecnología, CONACYT, 1045 | ||
| 536 | |a Detalles de la financiación: Fundação de Amparo à Pesquisa do Estado de São Paulo, FAPESP, 2013/24155-3 | ||
| 536 | |a Detalles de la financiación: Fundação de Amparo à Pesquisa do Estado de São Paulo, FAPESP, 2015/13596-4 | ||
| 536 | |a Detalles de la financiación: Conselho Nacional de Desenvolvimento Científico e Tecnológico, CNPq, 312788/2013-4 | ||
| 593 | |a LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, Meudon, 92195, France | ||
| 593 | |a CRAAM Universidade Presbiteriana Mackenzie, São Paulo, Brazil | ||
| 593 | |a School of Physics and Astronomy, SUPA, University of Glasgow, Glasgow, G12 8QQ, United Kingdom | ||
| 593 | |a SCiESMEX, Instituto de Geofisica, Unidad Michoacan, Universidad Nacional Autonoma de Mexico, Morelia, Michoacan CP 58190, Mexico | ||
| 593 | |a IAFE, University of Buenos Aires, Buenos Aires, Argentina | ||
| 593 | |a CCS, University of Campinas, Campinas, Brazil | ||
| 690 | 1 | 0 | |a CHROMOSPHERE, MODELS |
| 690 | 1 | 0 | |a HEATING, CHROMOSPHERIC |
| 690 | 1 | 0 | |a HEATING, IN FLARES |
| 690 | 1 | 0 | |a RADIO BURSTS, MICROWAVE |
| 690 | 1 | 0 | |a X-RAY BURST, SPECTRUM |
| 690 | 1 | 0 | |a X-RAY BURSTS, ASSOCIATION WITH FLARES |
| 700 | 1 | |a Raulin, J.-P. | |
| 700 | 1 | |a Mackinnon, A. | |
| 700 | 1 | |a Giménez de Castro, G. | |
| 700 | 1 | |a Simões, P.J.A. | |
| 700 | 1 | |a Cabezas, D. | |
| 700 | 1 | |a de La Luz, V. | |
| 700 | 1 | |a Luoni, M. | |
| 700 | 1 | |a Kaufmann, P. | |
| 773 | 0 | |d Springer Netherlands, 2015 |g v. 290 |h pp. 2809-2826 |k n. 10 |p Sol. Phys. |x 00380938 |w (AR-BaUEN)CENRE-2238 |t Solar Physics | |
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