3 edition of Temporal characteristics of solar EUV, UV and 10830-A full-disk fluxes found in the catalog.
Temporal characteristics of solar EUV, UV and 10830-A full-disk fluxes
by National Oceanic and Atmospheric Administration, Environmental Research Laboratories, Air Resources Laboratory in Silver Spring, Md
Written in English
|Statement||Richard F. Donnelly, Lawrence C. Puga, Wanda S. Busby.|
|Series||NOAA technical memorandum ERL ARL -- -146|
|Contributions||Puga, Lawrence C., Busby, Wanda S., Air Resources Laboratory., United States. National Oceanic and Atmospheric Administration|
|The Physical Object|
|Pagination||1 v. (various pagings)|
We analyze EUV spectra of the full solar disk from the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS) spanning a period of two years. The observations were obtained via a fortuitous off-axis light path in the -- Angstrom passband. X‐ray fluxes and EUV fluxes. However, if X‐ray fluxes are adjusted for the CMD factor, they would have a higher correlation with the EUV fluxes. Thus they can be a good proxy for the EUV flux. These results show again that the variation in EUV flux is much related to the flare site on the solar disc.
since January , SEM/SOHO has made daily measurements of solar EUV flux at nm . Since EUV flux is very important for studying solar-terrestrial effects, several workers in the past have studied the correlation between EUV fluxes and several solar indices, with a view to see whether any index could serve as a ‘proxy’ for EUV flux . We present spectral synthesis calculations of the solar extreme UV (EUV) in spherical symmetry carried out with the 'Solar Modeling in 3D' code. The calculations are based on one-dimensional atmospheric structures that represent a temporal and spatial mean of the .
Inﬂuence of the solar EUV ﬂux on the Martian plasma environment R. Modolo1, G. M. Chanteur1, E. Dubinin2, and A. P. Matthews3 1CETP-IPSL, avenue de l’Europe, V´elizy, France 2Max-Planck Institute fur Aeronomie, Katlenburg-Lindau, Germany¨. The temporal characteristics of the full-disk chromospheric El-JV fluxes agree well with those of the ground-based measurements of the chromospheric He I absorption line at 10, A and differ systematically from those of the coronal El-JV and cm flux.
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The temporal characteristics of full-disk solar EUV flux measurements from the AE-E satellite are examined for 15 wavelength groups and compared with independent NIMBUS-7 satellite measurements at UV wavelengths and ground-based measures of solar activity.
The temporal characteristics of the full‐disk chromospheric EUV fluxes agree well with those of the ground‐based measurements of the chromospheric He I absorption line at 10, Å and differ system Cited by: The temporal characteristics of the full-disk chromospheric EUV fluxes agree well with those of the ground-based measurements of the chromospheric He I absorption line at 10, A and differ systematically from those of the coronal EUV and cm flux.
Several progressions in the temporal characteristics of full-disk solar UV and EUV fluxes have been identified that raise many questions about the solar physics involved. The collective effect of numerous enhancements smaller than scaled plages contribute significantly to the solar cycle variations, especially for emissions from the cooler portions of the corona and the chromosphere.
Abstract. The temporal characteristics of the full-disk chromospheric EUV fluxes agree well with those of the ground-based measurements of the chromospheric He I absorption line at 10, A and differ systematically from those of the coronal EUV and cm flux.
The close similarity of their temporal characteristics shows that the ‐nm line is a better estimator of the UV flux than the classical indices of solar activity, the ‐cm radio flux and the sunspot number, for short time scales (days, weeks).
magnetic activity, at least as measured by the EUV and related indices. The reconstruction suggests that the EUV flux reaches the same low (but non–zero) value at every sunspot minimum (possibly including Grand Minima), representing an invariant ‘solar magnetic ground state’.
The temporal characteristics of full-disk solar EUV flux measurements from the AE-E satellite are examined for 15 wavelength groups and compared with independent NIMBUS-7 satellite measurements at. Introduction. Solar activity indices have been and are currently used to model solar spectral irradiances when direct measurements are not available (Hinteregger,Heath and Schlesinger,Cebula et al., ).In a series of papers, Donnelly and his colleagues studied, in great detail, the relationship of solar activity indices then available to direct measurements of EUV and UV.
e profile to infer the solar EUV flux, T ex, and meridional wind. They are the driving forces for an ionospheric model and Figure 1.
The uniqueness of the inferred EUV flux. The top panel shows the EUV-T ex correlation coefficient in fitting the F layer N e. solar activity fairly accurately, the solar EUV ( nm) and F cm ( MHz, 1 sfu = Wm-2 Hz-1) fluxes are widely used to describe the variations in the solar extreme ultra violet (EUV) irradiance.
Often, it is postulated that the relationship between EUV flux and F cm flux is invariant over different solar. Donnelly's 41 research works with citations and reads, including: Solar UV flux measurements from the SBUV2 monitor on the NOAA9 satellite.
Part 1:. The GOES data have a temporal resolution of 1min (Machol et al.,). A speciﬁc experiment to measure EUV spectral solar radiance calibrated in ﬂight is Solar Auto-Calibrating EUV/UV Spectrophotometers (SolACES) (Schmidtke et al., ,;Nikutowski et al.,) as a part of the ESA SOLAR ISS mission.
Generally, the time resolution of the. Introduction  Solar extreme ultraviolet (EUV) and X‐ray photons are the primary energy source of the ionosphere and thermosphere of the Earth [Mitra, ; Liu et al., ].The solar flare is a sudden eruption solar phenomenon, associated with significant enhancements in EUV and X‐ray radiations, with larger enhancements in X‐rays and short wavelength EUV and relatively smaller.
Extremely Large EUV Late Phase EVE observations measure the solar EUV differential irradiance from to nm with unprecedented spectral resolution of nm, temporal cadence of 10s, and accuracy of 20% (Woods et al. The EVE Level-2 processing produces a combined set of merged spectra provided in a pair.
The long-term variability of the solar ultraviolet flux is quite different from the one of classical solar indices. The most important differences are the surprisingly small variations of the EUV fluxes during the solar cy the early occurence of a “solar EUV minimum” (HINTEREGGER) and the drastic increase at the beginning of the solar cycle The phenomenon of a difference between solar EVV fluxesI λ (λsolar indices but in cycles of different amplitudes is studied.
The difference can reach 15–20%. The phenomenon is explained in terms of a two-component model of solar EUV variations (from the active regions and the “undisturbed” solar surface). 11 years during – The temporal variations of these properties are correlated with the solar cycle vari-ations.
As mentioned above, network is an important component which contributes to the solar irradiance. The two lines considered, He i Å and O v Å give us information about the two heights in the solar atmosphere.
in a UV channel (where three passbands can be selected at λ, ). EVE measures the full disk solar irradi-anceintheEUVandsoftX-rayenergyrange(from1toÅ), with a cadence of 10 spectral resolution is ∼1Å between 50 and Å (with the Multiple EUV Grating Spectrographs MEGS-A and MEGS-B), and 10Å in the 1–50Å range.
Solar EUV/UV Irradiance Spectrum I extends from 30 nm in the EUV to the visible ( nm) I spans roughly 5 orders of magnitude I contains about % of the total solar ﬂux I shows exponential increase in FUV to Al-edge ( nm) I for increasing λ, the spectrum is characterized by: I strong emission lines (– nm) I absorption lines (– nm) I line-blanketed continuum.
The response of exospheric temperature to variations in solar EUV radiation was measured by the Aeros-EUV spectrometer. Correlation of these parameters is strongly impeded by the competing influence of the solar wind and by the changes in EUV heating efficiency.
While the comparison of exospheric temperatures with those from the MSIS model gives rather good agreement for .Fig.!- Solar EUV measurements during solar cyc 22 and [Langmuir probe on PYO measured total solar EUV flux during major portions of solar cycles 21 while SOHO/SEM measured the EUV flux in the range nm and nm during solar cycle ] daily solar EUV flux at .They showed that the core-to-wing ratio of Mg II h and k lines was a good measure of the temporal variaitons of the solar UV flux, including long-term variations, because the ratio is relatively insensitive to drifts in instrument sensitivity.