D. J. Strickland

Computational Physics (United States)

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R. R. Meier

George Mason University

L. J. Paxton

Johns Hopkins University Applied Physics Laboratory

J. S. Evans

Computational Physics (United States)

A. B. Christensen

Kolding Hospital

Donald E. Anderson

Johns Hopkins University Applied Physics Laboratory

D. Morrison

Johnson University

G. Crowley

Atmospheric and Space Technology Research Associates (United States)

R. E. Daniell

Institute for Magnetospheric Physics

Ching‐I. Meng

Johns Hopkins University Applied Physics Laboratory

J. D. Craven

University of Alaska Fairbanks

Cooperative Institutions

Johns Hopkins University

Johns Hopkins University Applied Physics Laboratory

University of Colorado Boulder

Laboratory for Atmospheric and Space Physics

Computational Physics (United States)

Goddard Space Flight Center

United States Naval Research Laboratory

NSF National Center for Atmospheric Research

The Aerospace Corporation

University of Colorado System

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{GUVI} Observations of Night Time Ionospheric Morphology

AGU Spring Meeting Abstracts (2002)

Charles Swenson A. B. Christensen R. J. Walterscheid L. J. Paxton Cheng Meng

Morphology

Source

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Citations (0)

The use of far ultraviolet remote sensing to monitor space weather

Advances in Space Research (2003)

L. J. Paxton D. Morrison D. J. Strickland M. G. McHarg Yongliang Zhang

Space Weather

Extreme ultraviolet

Ultraviolet

10.1016/s0273-1177(02)00886-4

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Citations (33)

Solar EUV irradiance variability derived from terrestrial far ultraviolet dayglow observations

Geophysical Research Letters (2004)

D. J. Strickland J. Lean R. R. Meier A. B. Christensen L. J. Paxton

Remotely sensed ultraviolet emissions from the Earth's upper atmosphere are shown to mirror fluctuations in solar EUV irradiance during July 2002, including the overall increase and decrease as the Sun rotated, and episodic increases associated with multiple solar flares. The TIMED/GUVI dayglow observations are used to derive a new quantity, Q EUV GUVI , which is a measure of integrated solar EUV electromagnetic energy shortward of 45 nm. Both the absolute Q EUV GUVI values and their modulation by solar rotation agree well with the corresponding solar EUV energy estimated by the NRLEUV irradiance variability model. The Q EUV GUVI values do not support recent suggestions that the solar EUV irradiances estimated by the model of Hinteregger et al. be increased by a factor of four, nor even a factor of two.

Extreme Ultraviolet Lithography

Extreme ultraviolet

Solar rotation

10.1029/2003gl018415

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Citations (45)

Low latitude ionosphere measurements by the Global-scale Observations of the Limb and Disk (GOLD) mission [poster]

AGUFM (2008)

R. Eastes D. N. Anderson W. E. McClintock A. Aksnes L. Andersson

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Atmospheric Ultraviolet Radiance Integrated Code (AURIC): theory, software architecture, inputs, and selected results

Journal of Quantitative Spectroscopy and Radiative Transfer (1999)

D. J. Strickland J. Bishop J. S. Evans T. Majeed P. Mike Shen

Airglow

Rocket (weapon)

MODTRAN

Ultraviolet

10.1016/s0022-4073(98)00098-3

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Citations (204)

<title>Simulation of spaceborne optical sensor data: I. Modeling capabilities with examples</title>

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (1996)

J. Bishop John A. Persing D. J. Strickland J. S. Evans R. J. Cox

Numerous instruments for UV-visible optical measurements of terrestrial backgrounds have recently flown or are scheduled for launch in the near future. In order to maximize the scientific return from such flight opportunities, simulations of data acquired by imaging and spectrographic imaging instruments spanning wide wavelength ranges are required to support experiment planning and post-launch data analysis/fusion activities. We are currently developing comprehensive capabilities for modeling these types of remote sensing data suitable for a number of mission-support applications, with specific focus on data acquired by the UVISI instruments on the Midcourse Space Experiment satellite. These capabilities are described in this presentation. The core modeling capabilities reside in a suite of well-tested first principles and empirical modeling codes for atmospheric radiances arising from a variety of physical processes (e.g., photoelectron impact excitation, Rayleigh and aerosol scattering, solar resonance and resonant fluorescence scattering, chemistry). Image generation and LOS spectral radiance evaluation techniques permitting continual change in observer location and viewing geometry without incurring large computational burdens have been set up to ingest the radiance modeling results to create high fidelity synthetic satellite data. Illustrative examples are presented.

10.1117/12.257194

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Precipitating electron interaction with the atmosphere: 2. The dayside cusp region

Journal of Geophysical Research Atmospheres (1985)

S. S. Prasad D. J. Strickland Yam T. Chiu

Interaction of precipitating low‐energy magnetosheath electrons with the atmosphere in the dayside cusp region has been studied. Both pitch angle and energy distributions of the fluxes as well as excitation functions for selected N 2 and O UV emission were obtained by numerically solving the multiangle equations of electron transport. The angular dependence of the elastic scattering was treated more precisely—in contrast to its treatment in previous studies via limiting approximations involving either sharply forward peaked or isotropic shapes. Pitch angle distributions with broad peaks around 90° were encountered, albeit in a very narrow energy, band, in the upper atmosphere above the collision‐dominated lower atmosphere where isotropic pitch angle distributions predominate. Pitch angle distributions in the upper atmosphere at energies below this narrow band are approximately mirror images of the distributions at higher energy in the sense that the high and low values of the two distributions are located in diametrically opposite pitch angle directions. In our energy regime, it is difficult to accurately infer the spectral characteristics of the incident flux from the spectral characteristics of the flux measured at 350–250 km because the densities at even these altitudes are sufficient to substantially alter the spectral characteristics of low‐energy incident electrons. In contrast, the incident flux in the keV region travel through this altitude region almost unaffected. For low precipitating fluxes on the order of (1–2) × 10 8 el cm −2 s −1 , photoelectrons may constitute a significant fraction of the measured flux for solar zenith angles as large as 100°. Influence of the photoelectrons decreases if either the precipitating flux increases or the solar zenith angle increases. There is some possibility that atmospheric emissions may be used for remote measurements of incident soft energy flux, because the ratios of molecular to atomic emission line intensities in the low‐energy region are quite different from those in the high‐energy region.

Pitch angle

Zenith

Energy flux

Electron precipitation

10.1029/ja090ia11p11025

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Citations (6)

Analysis of nitrogen and oxygen far ultraviolet auroral emissions

Journal of Geophysical Research Atmospheres (1982)

R. R. Meier Robert R. Conway P. D. Feldman D. J. Strickland E. P. Gentieu

A far ultraviolet rocket observation of an auroral arc has been analyzed by using laboratory measured emission cross sections and self‐consistent models of the atmospheric composition and energetic electron flux. We find that the observed arc was produced by a precipitating electron flux of 5–8 erg cm −2 s −1 energy content and 1.75‐ to 2.5‐keV characteristic energy. The N 2 Lyman‐Birge‐Hopfield spectral synthesis shows that the vibrational populations for the observed emissions are in agreement with laboratory electron impact spectra and the Franck‐Condon factors to υ″ = 0. This precludes any cascade process to the a ¹Π g state, which significantly changes the relative populations. Altitude profiles of the various bands can be reproduced by theory. Dissociation of N 2 can account for N I lines at 1134, 1200, and 1493 Å, and N II 1085 Å. Contrary to previous observations of auroras and the dayglow, there is no evidence of multiple scattering of 1200‐Å radiation by atomic nitrogen in the present observations. The atomic oxygen density required to explain the O I 1356, 1304, and 989‐Å emissions is 4×10 10 cm −3 at 120 km, a factor of 3.5 lower than the Jacchia (1971) model.

Electron precipitation

Ultraviolet

Extreme ultraviolet

10.1029/ja087ia04p02444

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Citations (53)

<title>AURIC airglow modules - Phase 1 development and application</title>

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (1993)

R. Link D. J. Strickland R. E. Daniell

The Atmospheric Ultraviolet Radiance Integrated Code's modules have been developed to calculate the 1000-6500 A thermospheric emission spectra and radiances of dayglow, nightglow, twilight, and electron aurora, while also accounting for solar, photoelectron, auroral electron, and chemical excitation processes as well as pure and self absorption and multiple scattering effects. An account is presently given of the overal architecture of the codes; attention is given to the design and implementation of the photoionization and electron flux modules, together with samples of the input data and generated output.

Airglow

Ultraviolet

10.1117/12.140843

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Citations (6)

The transport of resonance radiation in a nonisothermal medium—the effect of a varying Doppler width

Journal of Geophysical Research Atmospheres (1979)

D. J. Strickland

A method is presented for treating the transport of resonance radiation under the influence of a varying Doppler width resulting from temperature changes. The method is applied to transport of resonance photons in the earth's thermosphere for media of modest and large optical depths. The drop in temperature below the exosphere can lead to almost a factor of two reduction in the nadir viewing intensity observed, e.g., from satellites. The effect is weaker, however, for zenith viewing intensities, especially in the isothermal region.

Exosphere

Zenith

Isothermal process

Radiant intensity

10.1029/ja084ia10p05890

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Citations (29)