Heliophysics Events Knowledgebase Coverage Registry (HCR)
Observation Details
Overview Where Groups: Mode, FOV, # spectra in map Data Links
2014-10-19 12:06:26-14:59:31
HOP268 (MMF evolution)
Transition region and coronal response to MMFs
x,y:327",-239"
Max FOV:10"x81"
Target:Active Region
Nearby Events
6302A Continuum Intensity10"x81"2122 spectra
6302A Longitudinal Flux Density10"x81"2122 spectra
6302A Transverse Flux Density10"x81"2122 spectra
6302A Velocity 6301.5A10"x81"2122 spectra
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Level 2 Summary
Level 1 Monthly
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SOTSP: HOP268 (MMF evolution)
2014-10-19T12:06:26 to 2014-10-19T14:59:31
Science Goal: Transition region and coronal response to MMFs
Program: Sparse dynamics, 31"x80", step=3, Q75, 1-side, repeat
Target: Active Region
xcen=327 ycen=-239
Instrument: SOTSP
HOP/JOP: 268
Description: This is an investigation of small moving magnetic features (MMFs) that move radially outwards from a sunspot in the moat region. MMFs can have an opposite polarity to the sunspot, and an early IRIS data-set from 2013 October 22 demonstrated that such MMFs can exhibit both transition region and coronal emission as they cancel against stronger plage fields. These MMFs all show signatures in the AIA 1700 channel and the IRIS Mg II and C II lines. A subset show very strong SiIV emission, and a smaller subset show coronal emission in the AIA 171 filter. The MMFs typically have a lifetime of 20-60 minutes, and they move over distances of up to 25 arcsec. This IHOP will obtain coordinated observations between SOT, XRT, EIS and IRIS to identify the magnetic topology and evolution that determines what temperature these MMFs reach. Signatures of the (presumed) magnetic reconnection will be identified through dynamics seen in the IRIS and EIS emission lines.

This is an investigation of small moving magnetic features (MMFs) that move radially outwards from a sunspot in the moat region. MMFs can have an opposite polarity to the sunspot, and an early IRIS data-set from 2013 October 22 demonstrated that such MMFs can exhibit both transition region and coronal emission as they cancel against stronger plage fields. These MMFs all show signatures in the AIA 1700 channel and the IRIS Mg II and C II lines. A subset show very strong SiIV emission, and a smaller subset show coronal emission in the AIA 171 filter. The MMFs typically have a lifetime of 20-60 minutes, and they move over distances of up to 25 arcsec. This IHOP will obtain coordinated observations between SOT, XRT, EIS and IRIS to identify the magnetic topology and evolution that determines what temperature these MMFs reach. Signatures of the (presumed) magnetic reconnection will be identified through dynamics seen in the IRIS and EIS emission lines.

Annotations:
Hits: 31
Chief Observer
DeRosa(RCO)
Related Links
Cites: HOP268 (MMF evolution)     
Timeline: gif use
See also
Datasets
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wavelength: 6302A Continuum Intensity cadence: 0.01 min fov: 10,81 images: 2122 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: 0.01 min fov: 10,81 images: 2122 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: 0.01 min fov: 10,81 images: 2122 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: 0.01 min fov: 10,81 images: 2122 JavaScript Landing Page
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