Heliophysics Events Knowledgebase Coverage Registry (HCR)
Observation Details
Overview Where Groups: Mode, FOV, # spectra in map Data Links
2007-11-22 16:37:05-17:09:27
HOP46: Irradiance scan (N-S)
Synoptic SOT Irradiance Scans
x,y:-5",335"
Max FOV:60"x162"
Target:Active Region
Nearby Events
6302A Continuum Intensity60"x162"380 spectra
6302A Longitudinal Flux Density60"x162"380 spectra
6302A Transverse Flux Density60"x162"380 spectra
6302A Velocity 6301.5A60"x162"380 spectra
Level 1 Summary
Level 2 Summary
Level 1 Monthly
Level 2 Monthly
SP Cubes 13 MB
SOTSP: HOP46: Irradiance scan (N-S)
2007-11-22T16:37:05 to 2007-11-22T17:09:27
Science Goal: Synoptic SOT Irradiance Scans
Program: Normal map 60 arcsec, Irradiance: DO NOT MODIFY!
Target: Active Region
xcen=-5 ycen=335
Instrument: SOTSP
HOP/JOP: 46
Description: The total solar irradiance varies by about 0.1% over the course of the solar cycle, primarily due to the influence of magnetic structures such as sunspots and faculae on the photospheric spectral irradiance. Short-term irradiance variation (on the scale of days-to- months) is well understood to be due to the balance of sunspots and facular areas as they cross the disk. However on the decadal scale of the solar cycle, questions remain as to why the irradiance variation can lead and/or lag the active region count over the course of the cycle. Explanations ranging from changes in the solar diameter in response to magnetic flux storage in the convection zone to changes in the surface area of the photosphere due to F-mode modulation have been put forward. Seeing-free observations of both granulation and magnetic flux on a large range of scales are now possible with the SOT SP/FG instrument combination.

The total solar irradiance varies by about 0.1% over the course of the solar cycle, primarily due to the influence of magnetic structures such as sunspots and faculae on the photospheric spectral irradiance. Short-term irradiance variation (on the scale of days-to- months) is well understood to be due to the balance of sunspots and facular areas as they cross the disk. However on the decadal scale of the solar cycle, questions remain as to why the irradiance variation can lead and/or lag the active region count over the course of the cycle. Explanations ranging from changes in the solar diameter in response to magnetic flux storage in the convection zone to changes in the surface area of the photosphere due to F-mode modulation have been put forward. Seeing-free observations of both granulation and magnetic flux on a large range of scales are now possible with the SOT SP/FG instrument combination.

Annotations:
Hits: 41
Chief Observer
Observer: Ishikawa
Related Links
Cites: HOP46: Irradiance scan (N-S)     
Timeline: gif use
See also
Datasets
Order AIA Data Cutout
Get All Data
saaIntervals hiIntervals

wavelength: 6302A Continuum Intensity cadence: -1 min fov: 60,162 images: 380 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: -1 min fov: 60,162 images: 380 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: -1 min fov: 60,162 images: 380 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: -1 min fov: 60,162 images: 380 JavaScript Landing Page
Time Series (SP Datacubes)
VOEvent XML Planning Event