First spectral observations of the diffuse background with the Extreme Ultraviolet Explorer

Details First spectral observations of the diffuse background with the Extreme Ultraviolet Explorer First spectral observations of the diffuse background with the Extreme Ultraviolet Explorer

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...442..653j&link_type=abstract

Astrophysical Journal (ISSN 0004-637X), vol. 442, no. 2, Part 1, p. 653-661

Astronomy and Astrophysics

Astronomy

50

Background Radiation, Diffuse Radiation, Extreme Ultraviolet Radiation, Interstellar Gas, Space Plasmas, Spaceborne Astronomy, Ultraviolet Astronomy, Ultraviolet Emission, Ultraviolet Spectra, X Ray Spectra, Absorptivity, Abundance, Astronomical Models, Astronomical Spectroscopy, Extreme Ultraviolet Explorer Satellite, Neutral Gases, Solar Neighborhood, X Ray Astronomy

Scientific paper

We present the first results from the analysis of the spectroscopic observations of diffuse extreme ultraviolet (EUV) emission taken with the Extreme Ultraviolet Explorer (EUVE) spectrometers in the wavelength range 160-740 A. Although not designed or optimized for diffuse observation, the EUVE spectrometers are the most sensitive diffuse EUV spectrometer in orbit. The spectral resolution for diffuse emission of the medium and long-wavelength spectrometers are 17 and 34 A FWHM, respectively. During the period from 1992 July 25 to 1992 August 19, the spectrometers surveyed a 2 x 20 deg field scanned from (l, b) = (24 deg, -28 deg) to (44 deg, -74 deg) with a total effective exposure time of 575,232 s. The only emission lines detected were those of He I and He II (584, 537, 304 A) with intensities consistent with local geocoronal and/or interplanetary scattering of solar radiation (584 A = 1.30 rayleighs; 537 A = 0.040 R; and 304 A = 0.029 R). Models of the soft X-ray background, which results from a 106 K plasma (Local Bubble) surrounding the neutral gas near the Sun (Local Cloud), predict that most of the flux from the hot plasma appears as emission lines in the EUV. We have compared these spectral predictions with our observations to place limits on the emission measure versus temperature of the proposed hot plasma. Using the same plasma model, we derived emissions measures for our data and the C and B soft X-ray bands of the Wisconsin rocket survey. We find that our limits for the plasma emission measure are a factor of 5-10 below the C- and B-band emission measures over the temperature range from 105.7 to 106.4 K. We explore possible scenarios that could reconcile our results with the X-ray surveys and conclude that depletion or a nonequilibrium plasma state rather than absorption are the more likely explanations of the discrepancy. We also show that our spectrum is inconsistent with the spectrum from the approximately 105 K gas at the conductive interface between the hot Local Bubble and the cooler Local Cloud given by Slavin (1989). In addition, we place new limits on the helium ionization parameter in the Sun's vicinity caused by the 106 K plasma in the Local Bubble.

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