SOTSP: HOP 451 (AR 13323)
2023-06-07T10:47:05 to 2023-06-07T11:30:30
Science Goal: Plasma composition evolution in active region leading and following polarities
Program: Fast map, 220"x123", Q65, 1-side CCD
Target: Active Region
xcen=135 ycen=-199
Instrument: SOTSP
HOP/JOP: 451
Description:
Main Objective: Tracking the coronal composition (using Hinode EIS) and plasma temperature at chromospheric heights (using IRIS) in the leading and following polarities of an active region over a few days. Scientific Justification: Plasma composition (quantified using the FIP bias parameter) was found to be correlated to photospheric magnetic flux density (Baker et al., 2015
Mihailescu et al., 2022). Mihailescu et al. (2022) suggest that changes in magnetic flux density influence the plasma temperature at chromospheric heights which in turn influences the amount of ionized low FIP elements at those heights. This then has a direct impact on the FIP bias we measure in the corona. The proposed IHOP observations aim to test this idea by tracking an active region over a few days and simultaneously measuring its photospheric magnetic field (using SDO HMI), plasma temperature at chromospheric height (using IRIS) and coronal plasma composition (using Hinode EIS). Active region leading polarities tend to have more concentrated magnetic field than their following counterparts - we request tracking both polarities to cover a wider range of magnetic flux values.
Main Objective: Tracking the coronal composition (using Hinode EIS) and plasma temperature at chromospheric heights (using IRIS) in the leading and following polarities of an active region over a few days. Scientific Justification: Plasma composition (quantified using the FIP bias parameter) was found to be correlated to photospheric magnetic flux density (Baker et al., 2015
Mihailescu et al., 2022). Mihailescu et al. (2022) suggest that changes in magnetic flux density influence the plasma temperature at chromospheric heights which in turn influences the amount of ionized low FIP elements at those heights. This then has a direct impact on the FIP bias we measure in the corona. The proposed IHOP observations aim to test this idea by tracking an active region over a few days and simultaneously measuring its photospheric magnetic field (using SDO HMI), plasma temperature at chromospheric height (using IRIS) and coronal plasma composition (using Hinode EIS). Active region leading polarities tend to have more concentrated magnetic field than their following counterparts - we request tracking both polarities to cover a wider range of magnetic flux values.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 218,122 images: 687 JavaScript Landing Page
