Measuring Velocities in the Early Stage of an Eruption: Using 'Overlappogram' Data fromHinodeEIS
| Autor: | George A. Doschek, Hirohisa Hara, Magnus M. Woods, Harry P. Warren, J. Leonard Culhane, Louise K. Harra, Sarah A. Matthews |
|---|---|
| Rok vydání: | 2017 |
| Předmět: |
Physics
010504 meteorology & atmospheric sciences Solar flare Spectrometer business.industry Imaging spectrometer Astronomy Astronomy and Astrophysics Field of view 01 natural sciences Solar prominence law.invention Optics Space and Planetary Science law Temporal resolution 0103 physical sciences Plasma parameter business 010303 astronomy & astrophysics 0105 earth and related environmental sciences Flare |
| Zdroj: | The Astrophysical Journal. 842:58 |
| ISSN: | 1538-4357 |
| Popis: | In order to understand the onset phase of a solar eruption, plasma parameter measurements in the early phases are key to constraining models. There are two current instrument types that allow us to make such measurements: narrow-band imagers and spectrometers. In the former case, even narrow-band filters contain multiple emission lines, creating some temperature confusion. With imagers, however, rapid cadences are achievable and the field of view can be large. Velocities of the erupting structures can be measured by feature tracking. In the spectrometer case, slit spectrometers can provide spectrally pure images by "rastering" the slit to build up an image. This method provides limited temporal resolution, but the plasma parameters can be accurately measured, including velocities along the line of sight. Both methods have benefits and are often used in tandem. In this paper we demonstrate for the first time that data from the wide slot on the Hinode EUV Imaging Spectrometer, along with imaging data from AIA, can be used to deconvolve velocity information at the start of an eruption, providing line-of-sight velocities across an extended field of view. Using He ii 256 A slot data at flare onset, we observe broadening or shift(s) of the emission line of up to ±280 km s−1. These are seen at different locations—the redshifted plasma is seen where the hard X-ray source is later seen (energy deposition site). In addition, blueshifted plasma shows the very early onset of the fast rise of the filament. |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|