SOTSP: HOP364 (plumes w/IRIS)
2019-03-01T08:20:05 to 2019-03-01T09:25:15
Science Goal: Observing magnetic field by Hinode(SOT/SP) in plume and non-plume regions seen by IRIS and AIA
Program: HOP 364 Normal Map, 123"x123", 1-side, Q75
Target: Quiet Sun
xcen=200 ycen=-162
Instrument: SOTSP
HOP/JOP: 364
Description:
On-disk solar coronal plumes, best seen in EUV -- AIA 171 A -- form/decay as a result of flux convergence/divergence at their base (Wang et al. 2016
Avallone et al. 2018). It is proposed that flux cancellation, leading to small-scale jets at plume base, is the primary mechanism for plume formation (Raouafi and Stenborg 2014). Avallone et al. (2018) found that plumes are dominantly unipolar in HMI magnetograms, and have similar lifetimes, peak luminosities, base magnetic fluxes in quiet regions and coronal holes. They also found locations of flux convergence forming no plumes in AIA 171, thus suggesting that a critical magnetic field is necessary but not sufficient to form a plume. Moreover, this summer we found hardly any differences between bases of plume and non-plume regions using IRIS MgII and Si IV SJ and spectral data. We propose to repeatedly scan a large FOV of a coronal hole or quiet region by IRIS and SOT/SP, for more than a couple of days, to catch a few plumes, and similarly behaving non-plume areas, and investigate any differences between plume and non-plume regions -- this includes finding out if there is mixed-polarity flux present at plume/non-plume base in SP data.
On-disk solar coronal plumes, best seen in EUV -- AIA 171 A -- form/decay as a result of flux convergence/divergence at their base (Wang et al. 2016
Avallone et al. 2018). It is proposed that flux cancellation, leading to small-scale jets at plume base, is the primary mechanism for plume formation (Raouafi and Stenborg 2014). Avallone et al. (2018) found that plumes are dominantly unipolar in HMI magnetograms, and have similar lifetimes, peak luminosities, base magnetic fluxes in quiet regions and coronal holes. They also found locations of flux convergence forming no plumes in AIA 171, thus suggesting that a critical magnetic field is necessary but not sufficient to form a plume. Moreover, this summer we found hardly any differences between bases of plume and non-plume regions using IRIS MgII and Si IV SJ and spectral data. We propose to repeatedly scan a large FOV of a coronal hole or quiet region by IRIS and SOT/SP, for more than a couple of days, to catch a few plumes, and similarly behaving non-plume areas, and investigate any differences between plume and non-plume regions -- this includes finding out if there is mixed-polarity flux present at plume/non-plume base in SP data.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 121,122 images: 768 JavaScript Landing Page
