Instruments:p4p

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Poker Flat 4 Channel Photometer

Contents


Contact Persons

Web Pages

Acknowledgments

The Aerospace 4 channel filter photometer at Poker Flat, Alaska was developed and supported by the Aerospace Technical Investment Program and the National Aeronautics and Space Administration (NASA).

Instrument/Model Description

The Aerospace 4 channel filter photometer at Poker Flat, Alaska (65.12N, 212.57E) was developed to estimate the energy flux of auroral electrons, their average energy Eo (usually from 0.1 to 30 keV using a modified Gaussian or Maxwellian shape), and a scale factor fo for the atomic oxygen densities [O] from an MSIS model atmosphere. The [O] densities using the scaling factor fo can be compared to GUVI/TIMED estimates. The technique is only valid for clear night conditions where the solar zenith angle (sza) is greater than 102 deg (code 4102=1), and there is enough auroral emission (427.8 nm brightness, code 2421). Poker Flat apex magnetic coordinates are (65.44, -95.56) at 110 km in 2001, with 0 UT corresponding to 12.93 MLT. The magnetic inclination and declination angles are 77.41 deg and 24.89 deg. The photometer looks up the magnetic field line with a field of view (fov) of about 1 deg. The data rate can be programmed, but typically each channel is integrated for 1 sec, where the whole cycle including filter moves takes about 8 sec.

The 4 channels correspond to:

  1. N2+ (427.8 nm, blue) first negative group (1NG) 0,1 molecular band
  2. OI (630.0 nm, red) forbidden
  3. OI (844.6 nm, eight) permitted
  4. N2 (871.0 nm or 871.4 nm) first positive group (1PG) 2,1 molecular band

The brightness (line emission rates, codes 2511-4) are calculated using site specific calibrations (codes 2521-4) from counts/sec to Rayleighs: initially 4.20, 11.70, 6.35 and 2.90 cts/s/R for channels 1-4. Background emission (codes 2571-4) is subtracted from the brightness where initial default values are 20 R, 80 R, 35 R and 10 R for channels 1-4. For custom processing, the background values can be chosen from the non-auroral data, which can be useful in moonlit (code 4103=0) or high airglow conditions. The background values were adjusted for much of the TIMED processing, and can result in small negative fluxes (unphysical) in low aurora cases. When sza<102 deg (code 4102=0), scattered sunlight increases the emissions. With clouds, 427.8 is absorbed more than 871.0(4), so the ratio goes to zero, as does the auroral energy flux. Nights with bad moon background light, bad clouds, or no aurora are not submitted to the CEDAR DB, although they are plotted on the web page http://gedds.pfrr.alaska.edu/aerospace/pokerflatdata.

A correction for atmospheric scattering is made after the backgrounds are removed using the ratio of 4278/8710 or 4278/8714. The nominal clear night sky diffuse aurora ratio of 4278/8710(4) is 2.60 for Poker Flat (code 2600). This ratio depends on the filters, band portions, and calibrations, and can be different using different filters. It is assumed to be constant otherwise, i.e., to be the same for different locations, seasons, magnetic activity and solar flux conditions. The normalized ratio (code 2601) is also the scattering correction factor (Icorr). 871.0(4) nm and 844.6 nm are assumed to have the same scattering (much smaller than the other two filters), and are not corrected for scattering. Icorr>1 means 4278 is being scattered into the fov, perhaps from a bright arc just outside the fov. Icorr<1 means 4278 is being scattered out of the fov, perhaps from a bright arc in the fov. Thus, the final 427.8 nm brightness must be divided by Icorr (code 2601), or the normalized 4278/8710(4) ratio, where the normalization is with respect to diffuse auroral conditions. Similarly, 630.0 nm emission is also corrected, but only half as much. The equations are:

  1. blue = 427.8 new = (427.8 brightness minus background) / Icorr
  2. red = 630.0 new = (630.0 brightness minus background)*(Icorr+1)/(2*Icorr)

The auroral electron energy flux is related to the corrected 4278 brightness:

  • energy flux (mW/m2) = blue (corrected 427.8 in kR) * 4.3
    This is independent of mean electron energy with an uncertainty of +/-20% (Strickland et al, 1989). Rearranging:
  • flux(mW/m2)=blue(R)/232
    The maximum flux is set to 327.67 mW/m2. Large values occur with sunlight.

The estimated auroral energy flux is found for all conditions, but the electron mean energy (Eo) and the scale factor for atomic oxygen (fo) are only found if there is sufficient 427.8 brightness. Eo and f0 are complex functions of the model conditions and the ratios of the calculated red/blue (rb, 6300/4278) and eight/blue (eb, 8446/4278) emissions. Plots of Eo and fo are given in Hecht et al (1989, 1999) and Strickland et al (1989) for various optical emission ratios where the x-axis is red/blue, and the y axis can be several different ratios. The red/blue ratio increases with smaller Eo, while the eight/blue ratio increases with larger fo. Increased solar flux or magnetic activity increases the neutral temperatures in models like MSIS, and decreases the O/N2 ratios at auroral emission heights, thus decreasing the eb ratio usually more than the rb ratio. The rb and eb ratios are also corrected for scattering after background emissions have been removed. The formulae are: rb=(6300/4278)*((Icorr-1)/2+1) and eb=8446/4278*Icorr.

The Strickland model (Strickland et al, 1989) takes an incoming auroral electron energy spectrum of a modified Maxwellian (code 2156=1) or Gaussian (code 2156=2) shape with average energy Eo, and transports it through a neutral atmosphere such as MSIS-1990 (Hedin, 1991) and a Chapman function ionosphere with a specified peak density, height and scale height. It then calculates the resulting auroral emissions. The average energy Eo is the energy flux over the number flux between 0.1 (formerly 1 keV) and 30 keV. The model is run at a particular location (codes 153, 156), for a specified day (code 22), solar local time (code 44) or UT, solar flux (code 350), and magnetic activity (code 340), with varying values of the auroral electron mean energy (Eo) in an atmosphere where the atomic oxygen is multiplied by various values of a scale factor (fo). The varying values of Eo and fo are interpolated in tables of the calculated red/blue (630.0 nm/427.8 nm) versus eight/blue (844.6 nm/427.8 nm) emission ratios provided the uncorrected 427.8 nm brightness (code 2421) is greater than 400 R. When Eo ~<0.3 keV or fo ~<0.2, the algorithm can fail and give negative (unphysical) values.

The estimated fo atomic oxygen scale factor must be used in conjuction with the original MSIS model atomic oxygen densities, or as an indication of change during the night from Joule or particle heating events that can cause local upwelling and decreased O/N2 ratios. The fo scaling factor applies to the whole MSIS [O] profile, which is given in kindat=18001 along with the temperature and molecular densities of [N2] and [O2] as a function of height between 82 and 390 km. There is a greater sensitivity to E region changes between 100 and 150 km where the auroral precipitation peaks, although the red line emission peaks around 200 km in aurora. This method really reflects changes in the O/N2 ratio, although only [O] is changed, not [N2]. This is approximately correct for the E region.

References

Hecht, J. H., A. B. Christensen, D. J. Strickland, R. R. Meier, Deducing composition and incident electron spectra from ground-based auroral optical measurements: Variations in oxygen density, J. Geophys. Res., 94, 13,553-13,563, 1989.
Hecht, J. H., A. B. Christensen, D. J. Strickland, T. Majeed, R. L. Gattinger, A. Vallance Jones, A comparison between auroral particle charateristics and atmospheric composition inferred from analyzing optical emission measurements alone and in combination with incoherent scatter radar measurements, J. Geophys. Res., 104, 33-44, 1999.
Hecht, J. H., D. L. McKenzie, A. B. Christensen, D. J. Strickland, J. P. Thayer and J. Watermann, Simultaneous observations of lower thermospheric composition change during moderate auroral activity from Kangerlussuaq and Narsarsuaq, Greenland, J. Geophys. Res., 105, 27,109-27,118, 2000.
Hedin, A. E., Extension of the MSIS thermospheric model into the middle and lower atmosphere, J. Geophys. Res, 96, 1159-1172, 1991.
Strickland, D. J., D. L. Book, T. P. Coffey and J. A. Fedder, Transport equation techniques for the deposition of auroral electrons, J. Geophys. Res., 81, 2755-2764, 1976.
Strickland, D. J., J. R. Jasperse and J. A. Whalen, Dependence of auroral FUV emissions on the incident electron spectrum and neutral atmosphere, J. Geophys. Res., 88, 8051-8062, 1983.
Strickland, D. J., R. R. Meier, J. H. Hecht and A. B. Christensen, Deducing composition and incident electron spectra from ground-based auroral optical measurements: Theory and model results, J. Geophys. Res., 94, 13,527-13,539, 1989.

Summary Plots for Model MSIS-1990 Values

Plots of the standard MSIS conditions that relate to the calculated atomic oxygen scaling factor fo. The atomic oxygen profile shows fo values of 0.25, 0.50, 1.00 (solid line) and 1.50.

Summary Plots for Poker Flat 4 channel photometer at the Poker Flat website

http://gedds.pfrr.alaska.edu/aerospace/pokerflatdata This web page gives plots of the data after each night of data taking. The data begin on April 10, 2001. During summer the instrument is turned off.

Summary Plots for Poker Flat 4 channel photometer

All these nights used the same model background. Nights with bad moon background light, bad clouds, or no aurora are not submitted to the CEDAR DB, although they are plotted on the web page http://gedds.pfrr.alaska.edu/aerospace/pokerflatdata. There is an overall nightly quality code for the data that are submitted. Good nights are marked 'good', while nights with some problem like moonlight, weak aurora, or some clouds, are marked 'OK'. Summary plots of the observed 427.8 nm brightness, the corrected 427.8 nm brightness (corrected = (observed - background)/Icorr), and the Icorr ratio (corrected 427.8/871.4 divided by the Poker Flat diffusive value 2.6) show that the corrected 427.8 nm emission is increased over the observed if Icorr is less than 1. The Icorr ratio corresponds to the scattering correction from the diffuse auroral condition. Also plotted are the auroral electron energy flux and mean electron energy, and the atomic oxygen scaling factor for a standard MSIS profile are given. The time when the solar zenith angle is 102 degrees (12 degrees below the horizon, or nautical twilight) is given as vertical dashed lines, and the calculated values are not shown beyond those times since they are not valid. The periods when it is moonlit are shown as a dark line at the top of each day. When the background correction for 427.8 nm emission is high and the emission is low, the calculated flux can be small negative (essentially zero). However, there are times when the 427.8 nm brightness is larger than 400 R, and yet the calculated Eo and fo are large negative as in Nov 6, 2001, or only fo is negative as in Oct 28, 2001. The algorithm fails for low Eo or low fo, but can be re-run in a different mode on a case-by-case basis in collaboration with the data supplier.


-Revised 30 Jan 2003 by Barbara Emery