Magnetic fields, bremsstrahlung and synchrotron emission in the flare of 24 October 1969
Magnetic fields, bremsstrahlung and synchrotron emission in impulsive flare of 24 October 1969
Pruss, G.↗
Engineering topics
Zirin, H.
Publications and source records attributed to Zirin, H..
The manifold structure of the chromosphere and corona
Solar chromosphere and corona manifold structure data, using high resolution filter photography
Zirin, H.↗
Observations of stellar chromospheres
Stellar chromosphere detection through H, K and metastable He lines observation, noting importance for solar physics
Zirin, H.↗
On K-line central reversals
Solar atmosphere vertical temperature and density distribution measurements, using spatially averaged H and K resonance line profiles central reversals
Pasachoff, J. M.↗
Magnetic fields, bremsstrahlung and synchrotron emission in the flare of 24 October 1969
Magnetic fields, bremsstrahlung, and synchrotron emission in solar flare of October 24, 1969
Zirin, H.↗
Application of the chromospheric magnetograph to active regions.
It is shown how to determine the magnetic field structure in active regions from the H-alpha morphology. The role of EFR (emerging flux region) as a bipolar region of velocity downflow is also shown. It is pointed out that, since all new magnetic flux emerges in strictly bipolar form, complex spot groups must result from surface interaction, hence most of the solar surface field may be produced on the surface.
Zirin, H.↗
Sunspot motion and flaring in M482
A series of flares was studied in McMath 11482 August 19-22, 1971, with particular reference to the basis for the flares and comparison with dekameter radio data. The flares were produced by rapid (approximately 1000 km/hr) westward motion of a large new p spot. Many flares occur just in front of the spot, and they cease when the motion stops. All flares occuring in front of the spot produce type III bursts, while even strong flares elsewhere in the region produce little or no type III. The time of type III emission agrees perfectly with the start of the H alpha flare. Thus type III bursts are only produced in favorable configurations. Simultaneous K-line movies are compared with H alpha films and show little difference in flare appearance.
Lazareff, B.↗
Active regions. I - The occurrence of solar flares and the development of active regions. II - Mount Wilson 16997- A small spot with big flares
Solar active regions, examining development and occurrence of solar flares
Zirin, H.↗
The chromospheric magnetograph
Chromospheric photoelectric magnetograms with high resolution H alpha pictures for deriving magnetic field directly from filtergrams
Veeder, G. J.↗
Coronagraph observations of the coronal condensation of 4 February 1962
Coronal condensation spectra during 4 February 1962 total eclipse, determining abundances, ionization equilibria, electron densities, etc, from Fe and Ca XV lines analysis
Zirin, H.↗
Identification of the hard X-ray pulse in the flare of September 11-12, 1968
Hard X-ray pulse identification with formation of brilliant kernel /11-12 September 1968/ flare by comparision with optical data
Vorpahl, J.↗
De-occultation X-ray events of 2 December, 1967
Flare rising from behind solar limb deoccultated by simultaneous recording by OSO III X ray detector and photoheliograph
Hudson, H.↗
The coarse structure of the solar atmosphere
Coarse structure of solar atmosphere from observations of quiet sun, discussing contradictions with existing models
Simon, M.↗
Interpretation of XUV spectroheliograms.
Chromospheric structural parameters determined from XUV spectroheliograms, discussing He 2 emission, O 4 and O 5 emission distribution, etc
Zirin, H.↗
The birth of active regions.
Bright regions with loops /BRLS/ in sunspot group development, discussing survey of time lapse movies from 1968
Weart, S. R.↗
Two prominence eruptions and the problem of emission.
Two flare unconnected prominence eruptions on 15, 29 January 1968, discussing emission at arch top
Zirin, H.↗
The solar flares of August 28 and 30, 1966.
Class 3 plus solar proton flare of August 28, 1966 and class 2 solar flare of August 30, 1966, summarizing stages of growth
Lackner, D. R.↗
Abundance analyses from extreme-ultraviolet emission lines.
Solar coronal ion abundance analyses from extreme UV emission lines
Zirin, H.↗