Abstract

An instrument is described that poduces monochromatic images differing from normal filtergrams in that the wavelength of the transmission band varies slowly and linearly across the image. The monochromatic bandwidth can be changed to almost any value, and the transmission band can easily be shifted to any part of the visible spectrum. Various applications for solar research are discussed.

© 1973 Optical Society of America

Full Article  |  PDF Article

References

  • View by:
  • |
  • |
  • |

  1. Y. Öhman, Astrophys. J. 111, 362 (1950).
    [CrossRef]
  2. W. E. Behring, J. M. Jackson, S. C. Miller, W. A. Rense, J. Opt. Soc. Am. 44, 229 (1954).
    [CrossRef]
  3. J. O. Stenflo, Solar Phys. 3, 482 (1968).
    [CrossRef]
  4. Y. Öhman, Stockholm Obs. Medd. 175 (1967).
  5. Y. Öhman, in F. Labuhn, R. Lüst (Eds.), New Techniques in Space Astronomy, IAU Symp.41, 313 (1971).
  6. P. Mein, M. Blondel, Solar Phys., in press.
  7. F. H. Seares, Astrophys. J. 38, 99 (1913).
    [CrossRef]
  8. J. O. Stenflo, in R. Howard, Ed., Solar Magnetic Fields, IAU Symp.43, 101 (1971).
    [CrossRef]
  9. J. M. Beckers, Solar Phys. 3, 258 (1968).
    [CrossRef]
  10. G. Pålsgård, J. O. Stenflo, Solar Phys. 11, 155 (1970).
    [CrossRef]

1970 (1)

G. Pålsgård, J. O. Stenflo, Solar Phys. 11, 155 (1970).
[CrossRef]

1968 (2)

J. O. Stenflo, Solar Phys. 3, 482 (1968).
[CrossRef]

J. M. Beckers, Solar Phys. 3, 258 (1968).
[CrossRef]

1967 (1)

Y. Öhman, Stockholm Obs. Medd. 175 (1967).

1954 (1)

1950 (1)

Y. Öhman, Astrophys. J. 111, 362 (1950).
[CrossRef]

1913 (1)

F. H. Seares, Astrophys. J. 38, 99 (1913).
[CrossRef]

Beckers, J. M.

J. M. Beckers, Solar Phys. 3, 258 (1968).
[CrossRef]

Behring, W. E.

Blondel, M.

P. Mein, M. Blondel, Solar Phys., in press.

Jackson, J. M.

Mein, P.

P. Mein, M. Blondel, Solar Phys., in press.

Miller, S. C.

Öhman, Y.

Y. Öhman, Stockholm Obs. Medd. 175 (1967).

Y. Öhman, Astrophys. J. 111, 362 (1950).
[CrossRef]

Y. Öhman, in F. Labuhn, R. Lüst (Eds.), New Techniques in Space Astronomy, IAU Symp.41, 313 (1971).

Pålsgård, G.

G. Pålsgård, J. O. Stenflo, Solar Phys. 11, 155 (1970).
[CrossRef]

Rense, W. A.

Seares, F. H.

F. H. Seares, Astrophys. J. 38, 99 (1913).
[CrossRef]

Stenflo, J. O.

G. Pålsgård, J. O. Stenflo, Solar Phys. 11, 155 (1970).
[CrossRef]

J. O. Stenflo, Solar Phys. 3, 482 (1968).
[CrossRef]

J. O. Stenflo, in R. Howard, Ed., Solar Magnetic Fields, IAU Symp.43, 101 (1971).
[CrossRef]

Astrophys. J. (2)

F. H. Seares, Astrophys. J. 38, 99 (1913).
[CrossRef]

Y. Öhman, Astrophys. J. 111, 362 (1950).
[CrossRef]

J. Opt. Soc. Am. (1)

Solar Phys. (3)

J. M. Beckers, Solar Phys. 3, 258 (1968).
[CrossRef]

G. Pålsgård, J. O. Stenflo, Solar Phys. 11, 155 (1970).
[CrossRef]

J. O. Stenflo, Solar Phys. 3, 482 (1968).
[CrossRef]

Stockholm Obs. Medd. (1)

Y. Öhman, Stockholm Obs. Medd. 175 (1967).

Other (3)

Y. Öhman, in F. Labuhn, R. Lüst (Eds.), New Techniques in Space Astronomy, IAU Symp.41, 313 (1971).

P. Mein, M. Blondel, Solar Phys., in press.

J. O. Stenflo, in R. Howard, Ed., Solar Magnetic Fields, IAU Symp.43, 101 (1971).
[CrossRef]

Cited By

OSA participates in CrossRef's Cited-By Linking service. Citing articles from OSA journals and other participating publishers are listed here.

Alert me when this article is cited.


Figures (3)

Fig. 1
Fig. 1

Chromatograms illustrating the properties of the image (see text). The two exposures show a solar flare of importance Sb in Hα. In the lower image, which was obtained at UT10h12m on 15 June 1972, there is a large filament at the red side of Hα. It can only be seen at that wavelength because of its motion away from us. The Doppler shift is about 1.2 Å. In the top image, obtained 10 min earlier, the filament can hardly be discerned at all. This gives evidence for the sudden descent of the whole- filament toward the solar surface with velocities of the order of 55 km/sec, an event possibly triggered by the flare.

Fig. 2
Fig. 2

Optical scheme of the Capri chromatograph. The position of the optical components is somewhat variable. The numerical values (mm) in the figure represent a typical setup used.

Fig. 3
Fig. 3

Two simultaneous images of an active region, obtained using the polarization optics acting as a beam splitter. The images are purposely displaced in wavelength relative to each other for the study of velocity fields.

Equations (5)

Equations on this page are rendered with MathJax. Learn more.

I = I 0 [ 1 - r λ ( Δ λ - Δ λ v ± Δ λ H ) ] ,
Δ λ v = ( v / c ) λ 0 .
Δ λ H = 4.67 × 10 - 13 g λ 0 2 B ,
Δ λ = ( d / k ) × ( s / f ) cos b ,
d α / d λ = ( k / d cos i ) × ( f / f 0 ) .

Metrics