Abstract
A tiny and low-cost ground-based Fabry-Perot interferometer (FPI) was designed using a filter behind etalon and Galilean telescope system for the thermospheric wind observation with OI 630.0 nm nightglow emissions (~250 km). Based on the instrument, experiments were carried out at Langfang (39.40° N, 116.65° E) site for a rough comparison and Kelan (38.71° N, 111.58° E) site for a detailed validation. Wind results of Langfang experiment are well consistent with measurements of two other FPIs deployed at Xinglong (40.40° N, 117.59° E) and Kelan which are retrieved by the American National Center for Atmospheric Research (A-NCAR). In Kelan experiment, the averaged wind deviation between our FPI and A-NCAR FPI is 11.8 m/s. The averaged deviation of wind measurement error between them is 2.9 m/s. The comparisons suggest good agreement. Then, the analysis of influencing factors was made. The center determination offset has an exponential relation with wind deviation, while the radius calculation offset is linear with wind deviation.
Highlights
The observations of thermosphere neutral winds are used for studying the dynamics and behavior of the thermospheric atmosphere and for developing forecasting capabilities for the space environment
Measurements of two American National Center for Atmospheric Research (A-NCAR) Fabry–Perot interferometer (FPI) deployed at Xinglong and Kelan sites are considered as reference data
Wind measurements of a clear night (24 September 2014) at Langfang site are compared with wind velocities of A-NCAR FPIs
Summary
The observations of thermosphere neutral winds are used for studying the dynamics and behavior of the thermospheric atmosphere and for developing forecasting capabilities for the space environment. Various investigations and improvements have been reported for FPIs, for example, studies featuring long-term measurements (Hernandez and Roble 1995, Biondi et al 1999), use of cooled CCD detectors (Biondi et al 1995, Shiokawa et al 2001, 2003), two-dimensional imaging capability (Rees et al 1984, Niciejewski et al 1994, Nakajima et al 1995, Ishii et al 1997, Conde et al 2001, Sakanoi et al 2009, Kosch et al 2010), and daytime measurement (Gerrard and Meriwether 2011, Wu et al 2012) Most of these instruments are designed using large-aperture etalons and filters. Some FPIs have been reported using small-aperture etalons to lower the costs (Makela et al 2009, 2011; Shiokawa et al 2012)
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