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Infrared Helioseismology: Detection of the chromospheric mode

Published online by Cambridge University Press:  03 August 2017

Drake Deming ,
David A. Glenar ,
Hans Ulrich Käufl  and
Fred Espenak
Drake Deming
Affiliation:
Planetary Systems Branch, Code 693, Goddard Space Flight Center, Greenbelt, MD 20771
David A. Glenar
Affiliation:
Department of Physics, Colgate University, Hamilton, NY 13346
Hans Ulrich Käufl
Affiliation:
Planetary Systems Branch, Code 693, Goddard Space Flight Center, Greenbelt, MD 20771
Fred Espenak
Affiliation:
Planetary Systems Branch, Code 693, Goddard Space Flight Center, Greenbelt, MD 20771

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We have observed solar oscillations using a new instrumental technique in a relatively unexplored region of the solar spectrum. We obtained a 2-day sequence of line profiles, at 30 second intervals, for a pure rotation line of OH at 11.065 μm, using a laser heterodyne spectrometer to view a 2 arc-sec portion of the quiet Sun at disk center. The continuous opacity of the solar atmosphere increases with wavelength longward of 1.6 μm, so 11 μm lines are formed in the upper photosphere, near h = 250 km. In this region the OH rotational transitions have δJ=1 collisional rates which are two orders of magnitude larger than their radiative rates. Hence the OH lines have source functions which are equal to the Planck function, and the high spectral purity provided by the laser heterodyne technique makes their line profiles especially appropriate for investigating the dynamics of the solar atmosphere. We have recently reported (Deming et al. 1986) that oscillations in this OH line show evidence of a resonance due to a cavity in the solar chromosphere.

Type
Chapter 7: Oscillations in the Solar Atmosphere
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 425 - 428
Copyright
Copyright © Reidel 1988 

References

Ando, H. and Osaki, Y. (1977), Publ. Astron. Soc. Japan, 29, 221.Google Scholar
Christensen-Dalsgaard, J. and Frandsen, S. (1983), Solar Phys. 82, 165.Google Scholar
Deming, D., Glenar, D. A., Käufl, H. U., Hill, A. A., and Espenak, F. (1986), Nature 322, 232.Google Scholar
Frazier, E. N. (1968), Ap. J. 152, 557.Google Scholar
Gouttebroze, P. (1986), paper presented at IAU Symposium No. 123, Aarhus, Denmark (these proceedings).Google Scholar
Gurman, J. B. and Liebacher, J. W. (1984), Ap. J. 283, 859.Google Scholar
Libbrecht, K. G., Popp, B. D., Kaufman, J. M. and Penn, M. J. (1986), submitted to Nature. Google Scholar
Lindsey, C., Becklin, E. E., Jefferies, J. T., Orrall, F. Q., Werner, M. W., and Gatley, I. (1983), Ap. J. (Lett.) 264, L25.Google Scholar
Lindsey, C. and Kaminski, C. (1984), Ap. J. (Lett.) 282, L103.Google Scholar
Lites, B. W. and Chipman, E. G. (1979), Ap. J. 231, 570.Google Scholar
Stix, M. (1970), Astr. Ap. 4, 189.Google Scholar
Ulrich, R. K. and Rhodes, E. J. Jr. (1977), Ap. J. 218, 521.Google Scholar