Prominence-corona transition region plasma diagnostics from SOHO observations
New results concerning prominence observations and in particular the prominence-corona transition region (PCTR) are presented. In order to cover a temperature range from 2 × 104 to 7 × 105 K, several emission lines in many different ionization states were observed with SUMER and CDS on board SOHO. E...
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| Formato: | Capítulo de libro |
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2004
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| LEADER | 08325caa a22007577a 4500 | ||
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| 001 | PAPER-21154 | ||
| 003 | AR-BaUEN | ||
| 005 | 20241212100042.0 | ||
| 008 | 190411s2004 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-15444368354 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Cirigliano, Daniela Paola | |
| 245 | 1 | 0 | |a Prominence-corona transition region plasma diagnostics from SOHO observations |
| 260 | |c 2004 | ||
| 270 | 1 | 0 | |m Cirigliano, D.; Institut d'Astrophysique Spatiale, Batiment 121, Campus Universitaire Paris-Sud, 91405 Orsay Cedex, France |
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| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a New results concerning prominence observations and in particular the prominence-corona transition region (PCTR) are presented. In order to cover a temperature range from 2 × 104 to 7 × 105 K, several emission lines in many different ionization states were observed with SUMER and CDS on board SOHO. EM and DEM were measured through the whole PCTR. We compared the prominence DEM with the DEM from other solar structures (active region, coronal hole and the chromosphere-corona transition region (CCTR)). We notice a displacement of the prominence DEM minimum towards lower temperatures with respect to the minimum of the other structures. Electron density and pressure diagnostics have been made from the observed C III lines. Local electron density and pressure for T ∼ 7 × 104 K are respectively log Ne = 9.30-0.34+0.30 and 0.0405-0.014+0.012. Extrapolations over the entire PCTR temperature range are in good agreement with previous SOHO results (Madjarska et al., 1999). We also provide values of electron density and pressure in two different regions of the prominence (center and edge). The Doppler velocity in the PCTR shows a trend to increase with temperature (at least up to 30 km s -1 at T ∼ 7 × 104 K), an indication of important mass flows. A simple morphological model is proposed from density and motion diagnostics. If the prominence is taken as a magnetic flux tube, one can derive an opening of the field lines with increasing temperature. If the prominence is represented as a collection of threads, their number increases with temperature from 20 to 800. Derived filling factors can reach values as low as 10 -3 for a layer thickness of the order of 5000 km. The variation of non-thermal velocities is determined for the first time, in the temperature range from 2 × 104 to 7 × 105 K. The quite clear similarity with the CCTR non-thermal velocities would indicate that heating mechanisms in the PCTR could be the same as in the CCTR (wave propagation, turbulence MHD). © 2004 Kluwer Academic Publishers. |l eng | |
| 536 | |a Detalles de la financiación: Centre National d’Etudes Spatiales, CNES | ||
| 536 | |a Detalles de la financiación: National Aeronautics and Space Administration | ||
| 536 | |a Detalles de la financiación: Ministère de l'Enseignement supérieur, de la Recherche et de l'Innovation, MESRI | ||
| 536 | |a Detalles de la financiación: European Space Agency | ||
| 536 | |a Detalles de la financiación: SOHO is a ESA/NASA mission. French teams are supported by CNES and CNRS. The SUMER project is financially supported by DARA, CNES, NASA, and the ESA PRODEX program (Swiss contribution). We thank the CDS team for the support of the ION-PROM program and the MEDOC team at IAS where the observations and data reduction have been done. We appreciate the corrections and suggestions of the referee Dr. T. Kucera who helped to substantially improve the paper. Daniela Cirigliano acknowledges the support of the Ministère de la Recherche et la Technologie and the ECOS program. | ||
| 593 | |a Institut d'Astrophysique Spatiale, Batiment 121, Campus Universitaire Paris-Sud, 91405 Orsay Cedex, France | ||
| 593 | |a Inst. Astronomia Y Fis. del Espacio, C.C. 67, Suc 28, (1428) Ciudad de Buenos Aires, Argentina | ||
| 700 | 1 | |a Vial, J.-C. | |
| 700 | 1 | |a Rovira, M. | |
| 773 | 0 | |d 2004 |g v. 223 |h pp. 95-118 |k n. 1-2 |p Sol. Phys. |x 00380938 |w (AR-BaUEN)CENRE-2238 |t Solar Physics | |
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