Solar physics in the VUV: the importance of high resolution observations

G. E. Brueckner

doi:10.1364/AO.19.003994

Applied Optics
Vol. 19,
Issue 23,
pp. 3994-4001
(1980)
•https://doi.org/10.1364/AO.19.003994

Solar physics in the VUV: the importance of high resolution observations

G. E. Brueckner

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G. E. Brueckner, "Solar physics in the VUV: the importance of high resolution observations," Appl. Opt. 19, 3994-4001 (1980)

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Abstract

Newly developed space instrumentation has made it possible to explore the sun’s UV spectrum with high spatial, spectral, and temporal resolution. The global existence of a hot corona and the outstreaming solar wind may be caused by rather high energetic events occurring in the quiet sun. These events are extremely localized and cover only a small fraction of the solar disk.

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Designation	Wavelength range (Å)	Wavelength coverage (Å)	Spectral res. or bandwidth (Å)	Field of view	Spatial resolution	Detector	Ref.
U. Hawaii echelle	2700–2900	2700–2900	0.015	12 min of arc	5 sec of arc	Film	1
LASP OSO-8	1200–2000	Single elem.	0.02–0.04	1 res. el.	2 × 20 sec of arc	Photoel.	2
LSPS OSO-8	1016–3982 six channels	Six channels 16–32 Å wide Centered around H Lyman-β, H Lyman-α, Mg iih + k, Ca iih + k	0.020–0.060	1 res. el.	1 sec of arc	Photoel.	3
Saljut	970–1400	970–1400	0.3	8 min of arc	5 sec of arc	Film	4,5
HRTS spectrograph	1175–1710	1175–1710	0.06	16 min of arc	1 sec of arc	Film	6,7
HRTS spectroheliograph	1550–1600	Single elem.	40	16 × 10 min of arc	1 sec of arc	Film	8
Lyman-α coronagraph	1216	±1	0.3	0-3 R. (solar radius)	0.6 × 4 min of arc	Photel.	9
SMM	1150–3600	Four spectral elements	0.02	1 res. el.	2 sec of arc	Photoel.	10

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Applied Optics