The Flare of September 18, 1957.

Jefferies, J. T.; Smith, Elske V. P.; Smith, Henry J.

doi:10.1086/146602

Cited by 26 publications

(12 citation statements)

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“…Most of those with unequal emission peak intensities are also red dominated, although a couple of examples whose blue peaks are slightly brighter are found. The profile shapes and shifts are generally consistent with a differentially expanding atmosphere, that is, with outward velocities which are highest in the lower levels of the atmosphere (Canfield and Athay, 1974;Kulander, 1979).…”

Section: S~mentioning

confidence: 68%

“…Ellison (1952) described what he considered to be typical profiles of various classes of events as observed visually through the Edinburgh spectrohelioscope; his results are reproduced here as Figure 1. Several observers have derived profiles from selected points in large (generally Class 3) events (Jefferies et al, 1959;Smith and Smith, 1963;Svestka, 1960Svestka, , 1963Banin, 1965;Tanaka in Brown et al, 1978). However, few of the published profiles have been drawn to show enough photometric accuracy to be useful for comparison with calculations.…”

Section: Introductionmentioning

confidence: 99%

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H? flare spectra

Schoolman¹,

Ganz

1981

Sol Phys

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We have studied over 1000 Ha flare profiles from 24 solar flares of Class 1 or brighter as recorded with Lockheed Solar Observatory's multi-slit spectrograph. We find that the profiles can be classified in terms of whether or not they show central self-reversals, whether'or not they have extended wings, and whether they are asymmetric. The profile groupings were found not to be correlated with the size (class) of the flares, nor do they seem to be well correlated with the kind of chromospheric flare structure from which they are emitted. Although different flare points within the same overall event may show profiles of different types, any given element (bright patch) can usually be described in terms of a single combination of the profile descriptors.

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Section: S~mentioning

confidence: 68%

Section: Introductionmentioning

confidence: 99%

H? flare spectra

Schoolman¹,

Ganz

1981

Sol Phys

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“…5) Jefferies, Smith and Smith (1959) found HelI 4686 in the spectra of disk flares. Although the brightness is not great, high loop densities (at least i012"s) are required.…”

Section: )mentioning

confidence: 96%

The optical flare

Zirin

1983

Sol Phys

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Optical observationd now present considerable information on the flare process. It is always associated with filaments and with simplification of existing magnetic connections, and it arises from the emergence and expansion of new flux.The optical flare divides into impulsive phase, with multiple flashes along the neutral line, and thermal phase, with two-ribbon expansion.The former bears some resemblance to tearing mode phenomena.The appearance of loops in emission requires very high densities in those phenomena.The ratios of the hydrogen lines, the excitation of HeII 4686, and the relation of vertical to horizontal structure all remain to be explained.

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“…1 upper element was 1.15 at 2119 UT. If we use the calibration line from Figure 2 for the wider profile, a reasonable assumption considering the profiles observed by Jefferies et al (1959), we obtain central intensities for D 3 of 122% and 126% for the two brightest. These intensities represent the total brightness of the solar surface at the center of the D 3 line.…”

Section: I(xt) = I C ¡F(k)[r(x)mentioning

confidence: 96%