Abstract

Observations at the 7 March 1970 eclipse were carried out for the purpose of measuring an expected difference in color between the radially and tangentially polarized components of the corona. The basic instrument was an array of Wollaston prisms and filters in association with a telescope and camera. Excellent photographs were obtained and are now being analyzed. It is expected that the color difference can be used in determination of the three-dimensional configuration of coronal features.

© 1970 Optical Society of America

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References

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  1. D. E. Billings, A Guide to the Solar Corona (Academic, New York, 1966), p. 152/There is an error on p. 151 of this reference. Equation (25) should read: (25)Ir=I0Neπσ(16-10u)/24.This changes Eqs. (26), (27), and (29). It requires that the last sentence of the paragraph following Eq. (27) read: “This is the same as the value found from Eq. (26) for u = 0.” Finally, in the first sentence in the paragraph following Eq. (29) we should have: ρr = 1.21ρ0.
  2. See Ref. 1, p. 150.
  3. C. W. Allen, Astrophysical Quantities (Athlone Press, London, 1963), p. 171.
  4. M. Minnaert, Z. Astrophys. 1, 209 (1930).

1930

M. Minnaert, Z. Astrophys. 1, 209 (1930).

Allen, C. W.

C. W. Allen, Astrophysical Quantities (Athlone Press, London, 1963), p. 171.

Billings, D. E.

D. E. Billings, A Guide to the Solar Corona (Academic, New York, 1966), p. 152/There is an error on p. 151 of this reference. Equation (25) should read: (25)Ir=I0Neπσ(16-10u)/24.This changes Eqs. (26), (27), and (29). It requires that the last sentence of the paragraph following Eq. (27) read: “This is the same as the value found from Eq. (26) for u = 0.” Finally, in the first sentence in the paragraph following Eq. (29) we should have: ρr = 1.21ρ0.

Minnaert, M.

M. Minnaert, Z. Astrophys. 1, 209 (1930).

Z. Astrophys.

M. Minnaert, Z. Astrophys. 1, 209 (1930).

Other

D. E. Billings, A Guide to the Solar Corona (Academic, New York, 1966), p. 152/There is an error on p. 151 of this reference. Equation (25) should read: (25)Ir=I0Neπσ(16-10u)/24.This changes Eqs. (26), (27), and (29). It requires that the last sentence of the paragraph following Eq. (27) read: “This is the same as the value found from Eq. (26) for u = 0.” Finally, in the first sentence in the paragraph following Eq. (29) we should have: ρr = 1.21ρ0.

See Ref. 1, p. 150.

C. W. Allen, Astrophysical Quantities (Athlone Press, London, 1963), p. 171.

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Figures (6)

Fig. 1
Fig. 1

A plot of ρ as defined in Eq. (1) for various azimuths from the plane of the sky of the light scattering coronal material. The various curves are for various heights of the line of sight above the limb.

Fig. 2
Fig. 2

Langley Research Center 9-in. (23-cm) cassegrainian telescope with Bronica camera attached. Photo courtesy of NASA.

Fig. 3
Fig. 3

A photograph of the Wollaston prism fused quartz optical assembly.

Fig. 4
Fig. 4

A diagram showing the function of the Wollaston prisms and their positions in relation to the colored filters. Fused quartz pieces are designated by Q, Wollaston prisms by W. The heavy line is the boundary between blue and red filters. The view is looking into the camera.

Fig. 5
Fig. 5

Four successive photographs of the corona through the optical system described herein. The orientation of the system is the mirror image of Fig. 4.

Fig. 6
Fig. 6

The primary calibrating device. The cut-away portion reveals the turnable scattering plate. The entire assembly is built of balsa wood, black paper, and styrofoam, weighs only a few pounds, and can be rotated into any position without flexing. However, since it is over 2 m tall and 1 m long, it is difficult to handle in even a small breeze.

Equations (5)

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ρ = I r 1 / I r 2 I t 1 / I t 2 ,
ρ = [ ( 1 - u 1 ) ( C - A ) + u 1 ( D - B ) ( 1 - u 2 ) ( C - A ) + u 2 ( D - B ) ] / [ ( 1 - u 1 ) C + u 1 D ( 1 - u 2 ) C + u 2 D ] .
I sc = f I Ω cos θ π = 1.9 × 10 - 5 I f cos θ ,
ρ = ( I r 1 I t 1 ) ( I t 2 I r 2 ) .
Ir=I0Neπσ(16-10u)/24.

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