Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares
Hard X-ray emission is generally interpreted as bremsstrahlung of 10-100 keV electron beams. This requires a high number of electrons to explain the intense X-ray flux observed. An interesting suggestion was made recently that 100 keV proton beams bombarding the atmosphere would create a hot thermal...
| Publicado: |
1990
|
|---|---|
| Materias: | |
| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00670049_v73_n2_p303_Henoux http://hdl.handle.net/20.500.12110/paper_00670049_v73_n2_p303_Henoux |
| Aporte de: |
| id |
paper:paper_00670049_v73_n2_p303_Henoux |
|---|---|
| record_format |
dspace |
| spelling |
paper:paper_00670049_v73_n2_p303_Henoux2023-06-08T15:06:17Z Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares Particle acceleration Polarization Sun: flares Sun: particle emission Sun: X-rays Hard X-ray emission is generally interpreted as bremsstrahlung of 10-100 keV electron beams. This requires a high number of electrons to explain the intense X-ray flux observed. An interesting suggestion was made recently that 100 keV proton beams bombarding the atmosphere would create a hot thermal plasma at the origin of the observed X-ray emission. Such low-energy protons have never been detected. We propose to use impact linear polarization of chromospheric lines as a diagnostic of 100 keV protons. Recent observations of Ha linear polarization in solar flares are presented. A polarization degree as high as 2.5% is observed in some Hα -bright patches. The electric vector is radial. This polarization is interpreted as impact polarization by low-energy protons. From existing observations we cannot discriminate between local and nonlocal origins of the detected population of energetic particles. However, we show that nonlocal proton acceleration leading to chromospheric bombardment is a likely explanation of the observed polarization. Whatever the initial distribution, transport effects in the chromosphere generate an anisotropic velocity distribution for protons. The required initial minimum energy and energy flux above this energy in the corona are found to be respectively 200 keV and 3 × 108 ergs cm-2 s-1 for a 107 K corona of mass 3×10-4 g cm-2. These results are valid as long as a possible scattering by waves is not strong enough for increasing the particle path in the corona. 1990 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00670049_v73_n2_p303_Henoux http://hdl.handle.net/20.500.12110/paper_00670049_v73_n2_p303_Henoux |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Particle acceleration Polarization Sun: flares Sun: particle emission Sun: X-rays |
| spellingShingle |
Particle acceleration Polarization Sun: flares Sun: particle emission Sun: X-rays Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares |
| topic_facet |
Particle acceleration Polarization Sun: flares Sun: particle emission Sun: X-rays |
| description |
Hard X-ray emission is generally interpreted as bremsstrahlung of 10-100 keV electron beams. This requires a high number of electrons to explain the intense X-ray flux observed. An interesting suggestion was made recently that 100 keV proton beams bombarding the atmosphere would create a hot thermal plasma at the origin of the observed X-ray emission. Such low-energy protons have never been detected. We propose to use impact linear polarization of chromospheric lines as a diagnostic of 100 keV protons. Recent observations of Ha linear polarization in solar flares are presented. A polarization degree as high as 2.5% is observed in some Hα -bright patches. The electric vector is radial. This polarization is interpreted as impact polarization by low-energy protons. From existing observations we cannot discriminate between local and nonlocal origins of the detected population of energetic particles. However, we show that nonlocal proton acceleration leading to chromospheric bombardment is a likely explanation of the observed polarization. Whatever the initial distribution, transport effects in the chromosphere generate an anisotropic velocity distribution for protons. The required initial minimum energy and energy flux above this energy in the corona are found to be respectively 200 keV and 3 × 108 ergs cm-2 s-1 for a 107 K corona of mass 3×10-4 g cm-2. These results are valid as long as a possible scattering by waves is not strong enough for increasing the particle path in the corona. |
| title |
Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares |
| title_short |
Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares |
| title_full |
Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares |
| title_fullStr |
Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares |
| title_full_unstemmed |
Impact line linear polarization as a diagnostic of 100 keV proton acceleration in solar flares |
| title_sort |
impact line linear polarization as a diagnostic of 100 kev proton acceleration in solar flares |
| publishDate |
1990 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00670049_v73_n2_p303_Henoux http://hdl.handle.net/20.500.12110/paper_00670049_v73_n2_p303_Henoux |
| _version_ |
1768541601255129088 |