TY - JOUR
T1 - Image reconstruction with July 11, 1991 eclipse observation
AU - Wang, Haimin
N1 - Funding Information:
ACKNOWLEDGEMENTS I wish to thank Dr. H. Zirin for his encouragement and discussions. I am grateful to the staff at BBS0 for support during the observation. I am also grateful to Michal Peri for reading the manuscript and many helpful comments. The operation of BBS0 and the data reduction was supported by NASA under NAGW-1972 and NASW5-27269 and the NSF under ATM-8816007.
PY - 1994
Y1 - 1994
N2 - White-light observations were carried out during the eclipse of July 11, 1991, at Big Bear Solar Observatory. The images were obtained by the 65 cm reflector with the OSL CCD camera. The lunar limb was always included in the field of view. We derived the one-dimensional point spread function (PSF) of seeing, which includes degradation by the telescope from the smeared lunar limb profile. The width of the PSF is between 0.8 to 1.3 arcsec on that day. Assuming cylindrical symmetry, we obtained the two-dimensional PSF. We then used the seeing function to deconvolve the observed white-light images. The reconstruction method enhances the observed 5% value of rms contrast to 18%; light bridges may be brighter than the normal photosphere; dark penumbra fibrils could be as dark as 50% of normal photosphere while the bright fibrils could reach the brightness of normal photosphere.
AB - White-light observations were carried out during the eclipse of July 11, 1991, at Big Bear Solar Observatory. The images were obtained by the 65 cm reflector with the OSL CCD camera. The lunar limb was always included in the field of view. We derived the one-dimensional point spread function (PSF) of seeing, which includes degradation by the telescope from the smeared lunar limb profile. The width of the PSF is between 0.8 to 1.3 arcsec on that day. Assuming cylindrical symmetry, we obtained the two-dimensional PSF. We then used the seeing function to deconvolve the observed white-light images. The reconstruction method enhances the observed 5% value of rms contrast to 18%; light bridges may be brighter than the normal photosphere; dark penumbra fibrils could be as dark as 50% of normal photosphere while the bright fibrils could reach the brightness of normal photosphere.
KW - Image reconstruction
KW - eclipse observation
UR - http://www.scopus.com/inward/record.url?scp=2742546197&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=2742546197&partnerID=8YFLogxK
U2 - 10.1016/0275-1062(94)90075-2
DO - 10.1016/0275-1062(94)90075-2
M3 - Article
AN - SCOPUS:2742546197
SN - 0275-1062
VL - 18
SP - 97
EP - 103
JO - Chinese Astronomy and Astrophysics
JF - Chinese Astronomy and Astrophysics
IS - 1
ER -