These datasets consist of full-disk, daily photographs of the sun taken at the H-alpha wavelength. Collection includes a variety of H-alpha photographic datasets contributed by a number of national and private solar observatories located worldwide. Solar observations in hydrogen-alpha (656.3 nm) reveal the structure and dynamics of chromospheric features including prominences, filaments, plague, filaments and the chromospheric network.

In 1967 Boulder became one of the SPAN observatories when it received its Razdow Telescope. The telescope would be used to observe solar flares and related solar phenomena. Using a Hydrogen - alpha filter that blocks most of the light, an observer could look through an eyepiece at the Sun, and a 35 - mm camera could take constant film footage of the Sun. This dataset shows many of the 35mm images that were taken by forecasters at the Space Environment Lab (SEL) now known as SWPC.

A solar magnetogram is a pictorial representation of the spatial variations in strength of the solar magnetic field. Magnetograms are often produced by exploiting the Zeeman effect (or, in some cases, the Hanle effect), which George Ellery Hale employed in the first demonstration that sunspots were magnetic in origin, in 1908. Solar magnetograms are produced by suitably instrumented telescopes referred to as magnetographs.

A solar magnetogram is a pictorial representation of the spatial variations in strength of the solar magnetic field. Magnetograms are often produced by exploiting the Zeeman effect (or, in some cases, the Hanle effect), which George Ellery Hale employed in the first demonstration that sunspots were magnetic in origin, in 1908. Solar magnetograms are produced by suitably instrumented telescopes referred to as magnetographs.

A solar magnetogram is a pictorial representation of the spatial variations in strength of the solar magnetic field. Magnetograms are often produced by exploiting the Zeeman effect (or, in some cases, the Hanle effect), which George Ellery Hale employed in the first demonstration that sunspots were magnetic in origin, in 1908. Solar magnetograms are produced by suitably instrumented telescopes referred to as magnetographs.

Full sun drawings are a form of synoptic analysis drawings, also known as Neutral line (NL) drawings which provide a comprehensive daily view of the sun for relevant solar feature of interest. To a somewhat limited extent depending on the provider the discerned features include neutral lines, coronal hole boundaries, active regions, plage, filaments and prominences. Also included are specific details about the coronal hole polarity, active region numbers, flare probabilities for each region and the proton event probabilities for each region.

Full sun drawings are a form of synoptic analysis drawings, also known as Neutral line (NL) drawings which provide a comprehensive daily view of the sun for relevant solar feature of interest. To a somewhat limited extent depending on the provider the discerned features include neutral lines, coronal hole boundaries, active regions, plage, filaments and prominences. Also included are specific details about the coronal hole polarity, active region numbers, flare probabilities for each region and the proton event probabilities for each region.

The decision to publish this volume of Solar Activity Maps (d2) in the Annuals of the International Geophyical Year was taken during the Fifth Meeting of the Special Commitee of Annual Geophysical International (CSAGI) held in Moscow, 30 July - 9 August 1958. The D-I series of I.G.Y. solar maps is a set of sketches, one for each day, of the following solar phnomena: sunspots, Bares, calcium plages, surges, and active prominences.

Solar synoptic maps usually refer to assembled composites recorded over a full solar rotation of about 27 days. Synoptic maps can be derived from single wavelength images or from multi-wavelength images highlighting solar features of interest (see above). Images for this dataset were provided by numerous solar observatories. The Boulder H-alpha (6563 A) synoptic maps, or charts, were first developed by McIntosh as an outgrowth of efforts to infer solar magnetic fields.

Solar synoptic maps usually refer to assembled composites recorded over a full solar rotation of about 27 days. Synoptic maps can be derived from single wavelength images or from multi-wavelength images highlighting solar features of interest (see above). Images for this dataset were provided by numerous solar observatories. The Boulder H-alpha (6563 A) synoptic maps, or charts, were first developed by McIntosh as an outgrowth of efforts to infer solar magnetic fields.