Recent discoveries from analysis of measurements made by the Sounding of the Atmosphere
using Broadband Emission Radiometry (SABER) instrument on the Thermosphere-Ionosphere-
Mesosphere Energetics and Dynamics (TIMED) satellite have shown that NO(v) 5.3 um
emission is the primary mechanism of dissipating solar-geomagnetic storm energy in the
thermosphere. Further insight into the ionosphere-thermosphere (IT) storm-time response
emerged from observations and analysis of the SABER 4.3 um channel radiances, which showed
that nighttime 4.3 um emission is dominated by NO+(v) during geomagnetically disturbed
conditions. Analysis of SABER NO+(v) 4.3 um emission led to major advances in the
understanding of E-region ion-neutral chemistry and kinetics, such as the identification of a new
source of auroral 4.3 um emission, which also provides a new context for understanding auroral
infrared emission from O2(a1▵g). Surprisingly, NO+(v) 4.3 um emission is the second largest
contribution to solar-geomagnetic infrared radiative response and provides a non-negligible
contribution to the "natural thermostat" thought to be solely due to NO(v) 5.3 um emission.
Despite these major advances, a fully physics-based understanding of the two largest sources of
storm-time energy dissipation in the IT system from NO(v) and NO+(v) is lacking because of the
limited information content contained in SABER's broadband infrared channel measurements.
On the other hand, detailed information on the chemical-radiative excitation and loss processes
for NO(v), NO+(v), and O2(a1▵g) emission is encoded in the infrared spectrum, of which SABER
only provides an integral constraint. Consequently, a prototype infrared field-wide Michelson
interferometer (FWMI) is currently under development to advance the understanding of IT
storm-time energetics beyond the current state of knowledge. It is anticipated that progress in the
developments of the FWMI technology, along with advancements in a physics-based
understanding of the fundamental chemical-radiative mechanisms responsible for IT infrared
emission, will play an integral role in the future planning of a rocket-borne and satellite-based Eregion
science missions. In this paper, a survey of recent SABER discoveries in IT ion-neutral
coupling will be given, open questions in a physics-based understanding of chemical-radiative
vibration-rotation excitation and loss from important IT infrared emitters will be identified, and
the FWMI instrument requirements necessary to address these open science questions will be
presented.
Auroral infrared emission observed from the TIMED/SABER broadband 4.3 um channel is used
to develop an empirical geomagnetic storm correction to the International Reference Ionosphere
(IRI) E-region electron densities. The observation-based proxy used to develop the storm model
is SABER-derived NO+(v) 4.3 um volume emission rates (VER). A correction factor is defined
as the ratio of storm-time NO+(v) 4.3 um VER to a quiet-time climatological averaged NO+(v)
4.3 um VER, which is linearly fit to available geomagnetic activity indices. The initial version of
the E-region storm model, called STORM-E, is most applicable within the auroral oval region.
The STORM-E predictions of E-region electron densities are compared to incoherent scatter
radar electron density measurements during the Halloween 2003 storm events. Future STORM-E
updates will extend the model outside the auroral oval.
Free space optics (FSO) is attractive for the 'last mile' communication in recent years for many combining advantages of fiber communication and other wireless technologies. FSO can provide high data rate with low power consumption, high immunity to interference, convenient deployment and flexibility. Optical system is an important section in the FSO transceiver terminal. In this paper the design of optical system based on a single Galileo telescope for both transmit and receive is proposed, and a polarization beam splitter is adopted to apart the receiving light from transmitting light. The configuration can avoid interference from the retroreflecting light of the ocular effectively. Some factors that affect the performance of the optical system are analyzed, such as the geometrical spreading loss and the loss increment according to pointing error and telescope maladjustment. Power budget shows that the system can satisfy the need of access for 1km in the light fog, and 2km in the thin fog.
A way to overcome the fading caused by atmosphere is discussed, and the power gain equalization method for the
wireless optical communication system is studied, the results for the system are also given. In the scheme of wide-range power-gain equalization, the power gain of the wireless optical system is controlled automatically in accordance with
visibility change of propagation channel by means of sampling the propagation channel, which has also been shown.
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