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2019-09-22 23:00:04-00:35:38 +1d
HOP379 Low-Latitude CH-2
Assessing the Solar Open Magnetic Flux from the Surface Up
x,y:454",-177"
Max FOV:89"x162"
Target:Coronal Hole
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6302A Continuum Intensity89"x162"575 spectra
6302A Longitudinal Flux Density89"x162"575 spectra
6302A Transverse Flux Density89"x162"575 spectra
6302A Velocity 6301.5A89"x162"575 spectra
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SOTSP: HOP379 Low-Latitude CH-2
2019-09-22T23:00:04 to 2019-09-23T00:35:38
Science Goal: Assessing the Solar Open Magnetic Flux from the Surface Up
Program: Deep Normal Map, 90"x164", 1-side, Q75
Target: Coronal Hole
xcen=454 ycen=-177
Instrument: SOTSP
HOP/JOP: 379
Description: Main Objective: To characterize the coronal hole (polar or on-disk) photospheric magnetic field properties with the aim to improve the heliospheric open magnetic flux estimate. Scientific Justification: The heliospheric open magnetic flux (OMF) based on moderate-resolution magnetograms was found to be grossly underestimated compared to in situ observation. Possible explanations include systematics in the spectropolarimetry inference. We propose to observe the coronal hole (CH) photospheric field using Hinode/SP (Fe I 630 nm) in coordination with BBSO/GST (Fe 1.56 ?m). The high spatial/spectral resolution data probing two different heights will allow for a systematic investigation of various systematics (e.g., radial field assumption, stray light, noise), and are expected to improve the OMF estimate. This work is an integral component of a recent NSF grant, in which Hinode and NST data are used to train a PhD student in preparation for the imminent DKIST operation.

Main Objective: To characterize the coronal hole (polar or on-disk) photospheric magnetic field properties with the aim to improve the heliospheric open magnetic flux estimate. Scientific Justification: The heliospheric open magnetic flux (OMF) based on moderate-resolution magnetograms was found to be grossly underestimated compared to in situ observation. Possible explanations include systematics in the spectropolarimetry inference. We propose to observe the coronal hole (CH) photospheric field using Hinode/SP (Fe I 630 nm) in coordination with BBSO/GST (Fe 1.56 ?m). The high spatial/spectral resolution data probing two different heights will allow for a systematic investigation of various systematics (e.g., radial field assumption, stray light, noise), and are expected to improve the OMF estimate. This work is an integral component of a recent NSF grant, in which Hinode and NST data are used to train a PhD student in preparation for the imminent DKIST operation.

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Chief Observer
Tiwari and DeRosa (RCO)
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Cites: HOP379 Low-Latitude CH-2     
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wavelength: 6302A Continuum Intensity cadence: -1 min fov: 89,162 images: 575 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: -1 min fov: 89,162 images: 575 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: -1 min fov: 89,162 images: 575 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: -1 min fov: 89,162 images: 575 JavaScript Landing Page
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