Origin of sunspots
Sunspots, seen as cool regions on the surface of the Sun, are a thermal phenomenon. Sunspots are always associated with bipolar magnetic loops that break through the solar surface.
Solar↗
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On the Origin of Sunspots
It is proposed tha sunspots (and other flux emergence phenomena) originate due ot the presence of fluctuating magnetic fields complementing the regular, mean field in the convection zone. The mean field predicted by dynamo theories is too weak itself to emerge at the surface of the Sun.
sunspots flux emergence solar magnetic fields Sun ↗
The Structure of Sunspot Umbras. I. Observations
High resolution photography of sunspot umbras with stratoscope i telescope
PHOTOGRAPHY↗
Methods for determining the three components of the magnetic field in the sunspots
Determining three components of magnetic field in sunspots
MAGNETIC FIELD↗
A morphological property of sunspot groups responsible for flares attended by emissions in meter waves <une propriete morphologique des groupes de taches solaires responsables des eruptions accompagnees d'emissions en ondes metriques<
Morphological property of sunspot groups related to flares involving radio emission
MORPHOLOGY↗
Measurements of the magnitude and direction of the magnetic field in the region of sunspots <izmereniya velichiny i napravleniya magnitnogo polya v oblasti solnechnykh pyaten<
Magnitude and direction of magnetic field in sunspot region
SUNSPOT↗
The structure of sunspot umbras. i - observations.
Structure of sunspot umbras, studied from photographs obtained from stratoscope i flights
UMBRA↗
On the magneto-hydrostatic theory of sunspots.
Sunspot models used to derive relations between coolness of spot and its magnetic field strength and between magnetic field strength and ratio of mixing length to pressure scale height
SUNSPOT↗
Sunspots - theory.
Sunspot analysis at Princeton University considering energy balance, magnetic field configuration, turbulent velocities in umbras and fine structure
MAGNETOHYDRODYNAMIC WAVE↗
Ionospheric electron content at temperate latitudes during the declining phase of the sunspot cycle
Ionospheric electron density during declining phase of sunspot cycle by Faraday effect observations
IONOSPHERIC ELECTRON DENSITY↗
Ionospheric electron content at temperate latitudes during the declining phase of the sunspot cycle.
Ionospheric electron content at temperature latitudes during declining phase of sunspot cycle determined by observation of Faraday effect
F LAYER↗
Spectrophotometry of the sunspot observed on June 19, 1959
Physical parameters for sunspot, and graphic method of determining excitation temperature from growth curve
GROWTH↗
Sunspot cycle and seasonal variations in the position and intensity of the equatorial electrojet in the Indian region.
Seasonal variations in position and intensity of equatorial electrojet and correlation of latter with sunspot number
STATISTICAL CORRELATION↗
Alfven waves in sunspots.
Model of nonradiative energy transport in sunspots, in which Alfven waves generated in convectively unstable layer propagate upward into overlying stable layer
SUNSPOT↗
Electron concentration profiles during sunspot maximum and minimum.
Ionosphere electron concentration profiles during sunspot maximum and minimum, using DOVAP in 1958 and rocket-borne two frequency propagation in 1964
Lootens, H. T.↗
A study of the green TiO band in the sunspot spectrum.
Sunspot spectra green TiO equivalent line widths measured on high dispersion spectrogram, obtaining rotational temperature
Makita, M.↗
The structure of a sunspot. III.
Sunspot structure model explaining features of Wilson effect, using intensity profiles from microphotometer tracings across photographs during passage across disk
Cannon, C. J.↗
The distribution of irregularities in the Antarctic ionosphere. I - Mean seasonal maps at sunspot minimum.
Irregularity distribution mapping of sunspot minimums in Antarctic ionosphere from satellite transit scaling
Stuart, G. F.↗