SOTSP: AR Obs. + EUNIS Backup
2021-05-18T20:34:05 to 2021-05-18T21:21:30
Science Goal: Coordinated Observations Between the EUNIS-2018 Sounding Rocket and EIS
Program: Fast map, 230"x164", Q65, 1-side CCD
Target: Active Region
xcen=-852 ycen=298
Instrument: SOTSP
HOP/JOP: 130
Description:
Main Objective: We propose to coordinate the EUNIS sounding rocket with EIS, IRIS, EOVSA, and IBIS during the flight scheduled for 6 November 2018. Scientific Justification: EUNIS contains two co-aligned multilayer telescope/spectrographs that cover spectral ranges 9.0-11.0 nm and 52.5-63.5 nm with 2-arcsec slits that extend over 11 arcmin (nearly a full solar radius). Our primary science objectives are to investigate pervasive, faint emission in lines of Fe XVIII and Fe XIX that would provide compelling evidence for the nanoflare model of solar coronal heating, and explore the relatively uncharted 9.0-11.0 nm wavelength range. This will be achieved with a sequence of fast EUNIS rasters in which the slit pointings will scan back and forth continuously within a maximum displacement of about 2 arcmin from the initial pointing. An additional EUNIS objective is to cross calibrate with EIS. This will be achieved indirectly for both EIS wavebands (17.0-20.5 nm and 25.0-29.0 nm) by comparing density- and temperature-insensitive line intensity ratios with theoretical values derived from CHIANTI. The key to the "indirect" cross calibration is that each line pair will include one member from EIS and one member from EUNIS.
Main Objective: We propose to coordinate the EUNIS sounding rocket with EIS, IRIS, EOVSA, and IBIS during the flight scheduled for 6 November 2018. Scientific Justification: EUNIS contains two co-aligned multilayer telescope/spectrographs that cover spectral ranges 9.0-11.0 nm and 52.5-63.5 nm with 2-arcsec slits that extend over 11 arcmin (nearly a full solar radius). Our primary science objectives are to investigate pervasive, faint emission in lines of Fe XVIII and Fe XIX that would provide compelling evidence for the nanoflare model of solar coronal heating, and explore the relatively uncharted 9.0-11.0 nm wavelength range. This will be achieved with a sequence of fast EUNIS rasters in which the slit pointings will scan back and forth continuously within a maximum displacement of about 2 arcmin from the initial pointing. An additional EUNIS objective is to cross calibrate with EIS. This will be achieved indirectly for both EIS wavebands (17.0-20.5 nm and 25.0-29.0 nm) by comparing density- and temperature-insensitive line intensity ratios with theoretical values derived from CHIANTI. The key to the "indirect" cross calibration is that each line pair will include one member from EIS and one member from EUNIS.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 235,162 images: 746 JavaScript Landing Page
