Abstract
The solar X-ray emission spectrum between 1 and 55 Å has been studied for one solar event, using the two X-ray experiments on-board of the ESRO 2 satellite. Although this event fits the description of the class of X-ray events described as gradual rise and fall events there is evidence to show that it is caused by the superposition of a number of events, of which the largest one was correlated with the appearance of an active loop-like prominence on the East limb of the Sun. By assuming the radiation processes in the source region to be thermal, temperatures and emission measures against time for the source region have been derived using the most recent models for free-free continuum and line emission due to thermal plasmas.
The temperatures derived have been used to calculate cooling rates due to radiation losses. It is shown from data in the 2.2–3.0 Å band that the cooling rate of the excited corona associated with the prominence is compatible with an electron density of 1 × 1011 cm−3 if a single injection of particles is considered to occur in the corona. From data in the 5.8–8.8 Å band one finds a value of 2 × 1010 cm−3.
An estimate of the total injected energy is made.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Acton, L. W.: 1968, Astrophys. J. 152, 305.
Brinkman, A. C. and Imhof, J. P.: 1970, ELDO/ESRO Scient. Techn. Rev. 2, 85.
Bruzek, A.: 1964, Astrophys. J. 140, 746.
Culhane, J. L., Herring, J., Sanford, P. W., O'Shea, G., and Phillips, R. D.: 1966, J. Sci. Instr. 43, 908.
Culhane, J. L., Sanford, P. W., Willmore, A. P., Blades, J., and Nettleship, R.: 1967, I.E.E.E. Trans. Nucl. Sci. NS-14, 38.
Culhane, J. L., Sanford, P. W., Shaw, M. L., Phillips, K. J. H., Willmore, A. P., Bowen, P. J., Pounds, K. A., and Smith, D. G.: 1969, Monthly Notices Roy. Astron. Soc. 145, 435.
Culhane, J. L., and Phillips, K. J. H.: 1970, Solar Phys. 11, 117.
Culhane, J. L., Vesecky, J. F., and Phillips, K. J. H.: 1970, Solar Phys. 15, 394.
Hudson, S. H., Petersen, E. L., and Schwartz, A. D.: 1969, Astrophys. J. 157, 389.
Jefferies, J. T. and Orrall, F. Q.: 1965, Astrophys. J. 141, 505.
Jordan, C.: 1969, Monthly Notices Roy. Astron. Soc. 142, 501.
Karzas, W. J. and Latter, R.: 1961, Astrophys. J. Suppl. 6, 167.
Kleczek, J.: 1964, in W. N. Hess (ed.), AAS-NASA Symposium on the Physics of Solar Flares, NASA SP-50.
Korchak, A. A.: 1971, Solar Phys. 18, 284.
Kundu, M. R.: 1965, Solar Radio Astronomy, Interscience Publishers, New York.
Landini, M. and Monsignori Fossi, B. C.: 1970, Astron. Astrophys. 6, 468.
Mewe, R.: 1972, Solar Phys. to be published.
Olson, C. A. and Lykoudis, P. S.: 1967, Astrophys. J. 150, 303.
Phillips, K. J. H., Culhane, J. L., and Sanford, P. W.: 1970, XIII COSPAR Plenary Meeting and Symposium, Leningrad.
Solar Geophysical Data: 1968, U.S. Department of Commerce, Environmental Science Services Administration.
Tandberg-Hanssen, E.: 1971, Colloquium on Physics of Prominences, Anacapri, 1971.
Teske, R. G.: 1971a, Solar Phys. 17, 76.
Teske, R. G.: 1971b, Solar Phys. 17, 181.
Unsöld, A.: 1955, Physik der Sternatmosphären, p. 234 (zweite Auflage).
Zirin, H.: 1963, Astrophys. J. 140, 1216.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Brinkman, A.C., Shaw, M.L. The 1–55 Å X-ray emission from an active limb prominence. Sol Phys 23, 120–133 (1972). https://doi.org/10.1007/BF00153895
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00153895