Authors: D. Hovestadt, M. Hilchenbach, A. Bürgi, B. Klecker, P.
Laeverenz, M. Scholer, H. Grnwaldt, W.I. Axford, S. Livi, E. Marsch,
B. Wilken, P. Winterhoff, F.M. Ipavich, P. Bedini, M.A. Coplan, A.B.
Galvin, G. Gloeckler, P. Bochsler, H. Balsiger, J. Fischer, J. Geiss,
R. Kallenbach, P. Wurz, K.-U. Reiche, F. Gliem, D.L. Judge, K.H.
Hsieh, E. Möbius, M.A. Lee, G.G. Managadze, M.I. Verigin, and M.
Neugebauer
Reference: Solar Physics 162, 441-481, 1995.
Abstract:
The CELIAS experiment on SOHO is designed to measure the mass,
ionic charge and energy of the low and high speed solar wind, of
suprathermal ions, and of low energy flare particles. Through analysis of
the elemental and isotopic abundances, the ionic charge state, and the
velocity distributions of ions originating in the solar atmosphere, the
investigation focuses on the plasma processes on various temporal and
spatial scales in the solar chromosphere, transition zone, and
corona.
The CELIAS experiment on SOHO is designed to measure the mass,
ionic charge and energy of the low and high speed solar wind, of
Abstract.1 The CELIAS experiment on SOHO is designed to measure the mass,
ionic charge and energy of the low and high speed solar wind, of
suprathermal ions, and of low energy flare particles. Through analysis of
the elemental and isotopic abundances, the ionic charge state, and the
velocity distributions of ions originating in the solar atmosphere, the
investigation focuses on the plasma processes on various temporal and
Abstract.1 The CELIAS experiment on SOHO is designed to measure the mass,
ionic charge and energy of the low and high speed solar wind, of
suprathermal ions, and of low energy flare particles. Through analysis of
the elemental and isotopic abundances, the ionic charge state, and the
velocity distributions of ions originating in the solar atmosphere, the
investigation focuses on the plasma processes on various temporal and
spatial scales in the solar chromosphere, transition zone, and corona.
CELIAS includes 3 mass- and charge discriminating sensors based on the
time-of-flight technique: CTOF for the elemental, charge and velocity
distribution of the solar wind, MTOF for the elemental and isotopic
composition of the solar wind, and STOF for the mass, charge and energy
distribution of suprathermal ions. The instrument will provide detailed in
situ diagnostics of the solar wind and of accelerated particles, which will
complement the optical and spectroscopic investigations of the solar
atmosphere on SOHO. CELIAS also contains a Solar Extreme Ultraviolet
Monitor, SEM, which continuously measures the EUV flux in a wide band of
17-170 nm, and narrow band around the 30.4 nm He II line.