Abstract
Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.
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References
Billings, D.E.: 1963,Ap. J. 137, 592
Billings, D.E., Lilliequist, C.G.: 1963,Ap. J. 137, 16
Delone, A.B., Makarova, E.A.: 1969,Solar Phys. 9, 116
Dere, K.P., Mason, H.E.: 1993,Solar Phys. 144, 217
Esser, R., Holzer, T.E., Leer, E.: 1987,J. Geophys. Res. 92, 13377
Hassler, D.M., Rottman, G.J., Shoub, E.C., Holzer, T.E.: 1990,Ap. J. Lett. 348, L77
Hassler, D.M., Moran, T.G.: 1994,Ap. J., in preparation
Hollweg, J.V.: 1973,Ap.J. 181, 547
Kim, I.S., Nikolsky, G.M.: 1975,Solar Phys. 43, 351
Kim, I.S.: 1992,Proceedings of the First SOHO Workshop, ESA SP-348, p. 149
Scudder, J.D.: 1992,Ap. J. 398, 319
Shoub, E.C.: 1988,Proc. 6th Int. Solar Wind Conf., NCAR TN-306, p.59
Shignh, J., Bappu, M.K.V., Saxena, A.K.: 1982,J. Astrophys. Astron. 3, 249
Tsubaki, T.: 1975,Solar Phys. 43, 147
Tsubaki, T.: 1977,Solar Phys. 51, 121
Tsuneta, S., L. Acton, M. Bruner, J. Lemen, W. Brown, R. Caravalho, R. Catura, S. Freeland, B. Jurcevich, M. Morrison, Y. Ogawara, T. Hirayama, J. Owens: 1991,Solar Phys. 136, 37
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Hassler, D.M., Moran, T.G. Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole. Space Sci Rev 70, 373–377 (1994). https://doi.org/10.1007/BF00777895
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DOI: https://doi.org/10.1007/BF00777895