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Far Infrared and Submillimeter Continuum Observations of Solar Flares: Justifications and Prospects for Ground-Based Experiments

Published online by Cambridge University Press:  03 August 2017

P. Kaufmann ,
E. Correia ,
J. E. R. Costa  and
A. M. Zodi
P. Kaufmann
Affiliation:
Centro de Radio-Astronomia e Aplicações Espaciais, CRAAE/EPUSP, C.P. 8174, 05508 - São Paulo, SP, Brazil
E. Correia
Affiliation:
Centro de Radio-Astronomia e Aplicações Espaciais, CRAAE/EPUSP, C.P. 8174, 05508 - São Paulo, SP, Brazil
J. E. R. Costa
Affiliation:
Centro de Radio-Astronomia e Aplicações Espaciais, CRAAE/EPUSP, C.P. 8174, 05508 - São Paulo, SP, Brazil
A. M. Zodi
Affiliation:
Centro de Radio-Astronomia e Aplicações Espaciais, CRAAE/EPUSP, C.P. 8174, 05508 - São Paulo, SP, Brazil

Abstract

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Solar flare observations in the sub-mm spectral bands are essentially non-existent. There is evidence that some solar bursts exhibit a spectral component rising in intensity towards wavelengths shorter than 3 mm, displaying fast sub-second pulses at different repetition rates. On the other hand, the spectral features of white light flares are also unknown in the infra-red range of frequencies. In both wavelength ranges the physics of the emission processes may involve particles accelerated to high energies. The diagnostics of solar flare continuum emission in the IR and sub-mm spectral regions will provide crucial tests on various flare models and bring some clues on the initial primary energy release mechanisms. We propose the construction and operation of a ground-based telescope, operating at two sub-millimeter wavelengths (at about 210 GHz and 405 GHz), with high time resolution (one millisecond), capable of determining the spatial position of burst emission centroids with high definition (a few arcseconds) using the multiple beam technique. Final installation and operation at a high-altitude site in the Argentinian Andes mountains are planned in a joint cooperation with Argentina's Instituto de Astronomia y Fisica del Espacio, IAFE (M. Rovira and associates) and Complejo Astronomico El Leoncito, CASLEO, San Juan (H. Levato and associates); and Switzerland's University of Bern, Institute of Applied Physics, IAP, Bern (A. Magun and associates).

Keywords

infrared: starsSun: flaresSun: radio radiation
Type
Part 1: Infrared Diagnostics of the Solar Atmosphere and Solar Activity
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 93 - 101
Copyright
Copyright © Kluwer 1994 

References

Acton, L.W.: 1964, Nature, 204, 64.Google Scholar
Akabane, K., Nakajima, H., Ohki, K., Moriyama, F., Miyaji, T.: 1973, Solar Phys. 33, 431.CrossRefGoogle Scholar
Alaart, M.A.F., van Nieuwkoop, J., Slottje, C., and Sondaar, L.H.: 1990, Solar Phys., in press.Google Scholar
Benz, A.: 1991, IAU Colloquium 133. Google Scholar
Brown, J.C.: 1976, Phil. Trans. R. Soc. Lond., 281, 473.Google Scholar
Butz, M., Hirth, W., Furst, E., and Harth, W.: 1976, Sond. Kleinheubacher Berichte, 19, 345.Google Scholar
Cliver, E.W., Kahler, S.W., McIntosh, P.: 1983, Astrophys. J. 264, 699.Google Scholar
Cogdell, J.R.: 1972, Solar Phys. 22, 147.CrossRefGoogle Scholar
Correia, E. and Kaufmann, P.: 1987, Solar Phys. 111, 143.Google Scholar
Correia, E., Kaufmann, P., and Magun, A.: 1993, these proceedings.Google Scholar
Costa, J.E.R., Correia, E., Kaufmann, P., Herrmann, R., Magun, A.: 1991, IAU Colloq. 133. Google Scholar
Croom, D.L.: 1970, Solar Phys. 15, 414.CrossRefGoogle Scholar
Droge, F.: 1977, Astron. Astrophys. 57, 285.Google Scholar
de Jager, C., Kuijpers, J., Correia, E., Kaufmann, P.: 1987, Solar Phys. 110, 317.Google Scholar
Filloy, E.M., Arnal, E.M.: 1991, display at 21st IAU General Assembly, Buenos Aires.Google Scholar
Forrest, D.J., Chupp, E.L.: 1983, Nature, 395, 291.Google Scholar
Georges, C.B., Schaal, R.E., Costa, J.E.R., Kaufmann, P., Magun, A.: 1989, IEEE Cat. no. 89TH0260-0, II, 447.Google Scholar
Hachenberg, O., and Wallis, G.: 1961, Zs.f. Astrophys., 52, 42.Google Scholar
Henoux, J.C., Aboudarham, J.: 1991, IAU Colloq. 133. Google Scholar
Herrmann, R.: 1990, , , Switzerland.Google Scholar
Kampfer, N.: 1991, private communication.Google Scholar
Kaufmann, P., Iacomo, P. Jr., Koppe, E.H., Santos, P.M., Schaal, R.E., and Blakey, J.R.: 1975, Solar Phys. 45, 189.CrossRefGoogle Scholar
Kaufmann, P., Piazza, L.R.; Schaal, R.E., Iacomo, P.: 1978, Ann. Geophys., 34, 105.Google Scholar
Kaufmann, P., Strauss, F.M., Opher, R., Laporte, C.: 1980, Astron. Astrophys. 87, 58.Google Scholar
Kaufmann, P., Correia, E., Costa, J.E.R., Dennis, B.R., Hurford, G.J., Brown, J.C.: 1984, Solar Phys. 91, 539.Google Scholar
Kaufmann, P., Correia, E., Costa, J.E.R., Zodi Vaz, A.M., and Dennis, B.R.: 1985, Nature, 313, 380.CrossRefGoogle Scholar
Kaufmann, P., Correia, E., Costa, J.E.R., and Zodi Vaz, A.M.: 1986, Astron. Astrophys. 157, 11.Google Scholar
Kaufmann, P.: 1988, Adv. Space Res., 48, (11)39.CrossRefGoogle Scholar
Kiplinger, A.L., Dennis, B.R., Emslie, A.G., Frost, K.J., and Orwig, L.E.: 1983, Astrophys. J. 265, 199.Google Scholar
Korchak, A.A.: 1971, Solar Phys. 18, 284.Google Scholar
Levato, H.: 1991, private communication.Google Scholar
Loran, J.M., Brown, J.C., Correia, E., and Kaufmann, P.: 1985, Solar Phys. 97, 363.Google Scholar
Machado, M., Schwartz, R., Fishman, G., Meegan, C., Paciesas, W. and Wilson, R.: 1992, Solar Phys. (Submitted).Google Scholar
McClements, K.G., and Brown, J.C.: 1986, Astron. Astrophys. 165, 235.Google Scholar
Magun, A., Fuhrer, M., Grater, M., Herrmann, R., Rolli, E., and Marti, A.: Report No 58, University of Bern, IAP. Google Scholar
Najita, K., and Orrall, F.Q.: 1970, Solar Phys. 15, 176.Google Scholar
Ohki, K., and Hudson, H.S.: 1975, Solar Phys. 43, 405.Google Scholar
Qijin, F., Qin, Z., Gao, Z., Li, Z., Huang, G., Jin, S., Cheng, Y., Huo, C., and Wei, S.: 1991, Proc. Chantilly Flares Workshop, 77.Google Scholar
Ramaty, R. and Petrosian, V.: 1972, Astrophys. J. 178, 241.Google Scholar
Rieger, E.: 1991, IAU Colloquium 133. Google Scholar
Shimabukuro, F.I.: 1970, Solar Phys., 15, 424.Google Scholar
Shimabukuro, F.I.: 1972, Solar Phys., 23, 19.Google Scholar
Shklovsky, J.: 1964, Nature, 202, 275.CrossRefGoogle Scholar
Slottje, C.: 1978, Nature, 275, 520.Google Scholar
Stein, W.A., and Ney, E.P.: 1963, J. Geophys. Res., 68, 65.Google Scholar
Sturrock, P.A., Kaufmann, P., Moore, R.L., and Smith, D.: 1985, Solar Phys., 94, 341.Google Scholar
Takakura, T., Kaufmann, P., Costa, J.E.R., Dagaonkar, K., Ohki, K., and Nitta, N.: 1983, Nature, 302, 317.CrossRefGoogle Scholar
Zirin, H. and Tanaka, K.: 1973, Solar Phys., 32, 173.Google Scholar
Zheleznyakov, V.V.: 1970, Radio Emission of the Sun and Planets, Pergamon Press.Google Scholar