The Nightglow

Roach, F.E.

doi:10.1016/s0065-2539(08)60832-x

Cited by 8 publications

(4 citation statements)

References 37 publications

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“…The keograms are plotted in units of spectral density in rayleighs per nanometer, and both channels show values mostly between 5 and 15 R/nm with some areas of sky reaching 20 R/nm. Comparing these values to two classic measurements of the nightglow over North America confirms that these values are what one would expect: Roach [] quotes the spectral density of atmospheric nightglow at 5 R/nm and the starlight contribution to the range of 5–15 R/nm for these wavelengths, and Vatsia et al . [] show spectra in radiant sterance that work out to around 9 R/nm in this wavelength range (if one calculates from 3 × 10 −12 W/cm 2 /sr/10 nm as a typical value).…”

Section: Calibration and Initial Field Datasupporting

confidence: 59%

A dedicated H‐beta meridian scanning photometer for proton aurora measurement

et al. 2017

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An instrument designed to measure the location and brightness of auroral emissions from energetic proton precipitation is described. This photometer scans from the north to south horizon with a stepper motor and mirror. The scans are configured in software for a 30 s cadence with equally spaced samples along a meridian at constant altitude. Broadband light is separated into two channels with a novel optical splitter. This splitter uses a filter that has high transmission for the signal channel and high reflection on both the long‐ and short‐wavelength sides to reflect the combined background passbands, directing each channel to its respective detector. The half‐cone angle and angle of incidence of this splitter filter allow for an overall compact optical design that also provides superior sensitivity in both signal and background channels. The signal channel is 3 nm wide full width at half maximum (FWHM) at 486.1 nm, and the background channel comprises two 3 nm wide FWHM passbands at 480 nm and 495 nm created by a single filter. Both of these channels are measured with photomultiplier tubes in photon‐counting mode. Calibrations indicate a response of around 1000 c/s per rayleigh. Data are currently acquired in 5 ms bins with a Nyquist frequency of 100 Hz. The first system (Forty‐Eight Sixty‐One (FESO)‐1) has been operating at Athabasca University since February 2014, and the second system (FESO‐2) was deployed at Lucky Lake, Saskatchewan, in October 2015. The improved sensitivity over legacy instruments and the simultaneous measurement of signal and background enable operation during intervals with dynamic electron aurora and scattered moonlight.

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Section: Calibration and Initial Field Datasupporting

confidence: 59%

A dedicated H‐beta meridian scanning photometer for proton aurora measurement

et al. 2017

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“…A common problem in airglow photometry is the OH contamination of the observations. Roach [1963], Davis and Smith [1965], and Smith and Owen [1966] have all discussed this problem. The 5577 A observations in this study are not seriously contaminated because the OH band (7-1) with its bandhead near 556.2 A has an estimated zenith intensity of only 20 rayleighs [Krassovsky et al, 1962], and the 5577 A emission normally has an intensity greater than 100 rayleighs.…”

Section: Oh Contaminationmentioning

confidence: 99%

Night airglow intensity variations in the [O I] 5577 A, [O I] 6300 A, and NaI 5890-96 A emission lines

Smith¹,

Steiger²

1968

J. Geophys. Res.

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“…Krassovsky et al [1962] give an average value for the continuum of 2 R/A between 4000 and 7000 A. Roach [1963Roach [ , 1964…”

Section: Similar Regression Plots As the Distance Separating The Twomentioning

confidence: 99%

Airglow observations from OSO-B2 satellite

Sparrow¹,

Ney²,

Burnett³

et al. 1968

J. Geophys. Res.

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Four photometers sensitive to three wide spectral bands observed the continuum airglow in profile once per orbit from the satellite OSO-B2. The tangential enhancement (factor of 35) gave good discrimination against zodiacal light and background starlight. Airglow intensity in the astronomical visible spectral region varied between 0.1 and 0.9 R/A and from 0.06 to 0.5 R/A in the blue spectral region. No significant latitude variation was found although a considerable temporal change occurred during the ten months of satellite operation. No correlation was found between airglow intensity and the South Atlantic geomagnetic anomaly or with solar events.

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The Nightglow

Cited by 8 publications

References 37 publications

A dedicated H‐beta meridian scanning photometer for proton aurora measurement

A dedicated H‐beta meridian scanning photometer for proton aurora measurement

Night airglow intensity variations in the [O I] 5577 A, [O I] 6300 A, and NaI 5890-96 A emission lines

Airglow observations from OSO-B2 satellite

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