Solar EUV Irradiance Measurements by the Auto-Calibrating EUV Spectrometers (SolACES) Aboard the International Space Station (ISS)

Schmidtke, G.; Nikutowski, B.; Jacobi, Christoph; Brunner, Raimund; Erhardt, Christian; Knecht, St.; Scherle, J.; Schlagenhauf, J.

doi:10.1007/s11207-013-0430-5

Cited by 32 publications

(43 citation statements)

References 15 publications

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“…The spectral characterization of reflecting, transmitting, and dispersive optical elements (mirrors, filters, gratings) can additionally be conducted at the respective beamlines using a reflectometer. Prominent past examples for complete instrument calibrations are the LYRA (LYman-alpha RAdiometer) instrument [19] and the SOL-ACES (SOLar Auto-Calibrating EUV/UV Spectrophotometers) experiment [20], the latter being still operable on-board the international space station ISS. With the new vacuum vessel, when operated at a beamline with monochromatized radiation, it will be possible to extend the DB calibration to even larger complete space instruments.…”

Section: Detector-based Calibrationsmentioning

confidence: 99%

Calibration of space instruments at the Metrology Light Source

Klein¹,

Fliegauf²,

Gottwald³

et al. 2016

AIP Conference Proceedings

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Abstract. PTB has more than 20 years of experience in the calibration of space-based instruments using synchrotron radiation to cover the UV, VUV and X-ray spectral range. New instrumentation at the electron storage ring Metrology Light Source (MLS) opens up extended calibration possibilities within this framework. In particular, the set-up of a large vacuum vessel that can accommodate entire space instruments opens up new prospects. Moreover, a new facility for the calibration of radiation transfer source standards with a considerably extended spectral range has been put into operation. Besides, characterization and calibration of single components like e.g. mirrors, filters, gratings, and detectors is continued.

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Section: Detector-based Calibrationsmentioning

confidence: 99%

Calibration of space instruments at the Metrology Light Source

Klein¹,

Fliegauf²,

Gottwald³

et al. 2016

AIP Conference Proceedings

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“…21 (Schmidtke, 1976b). Replacing the monochromator by narrow bandpass filters the in-flight calibration is repeatedly applied on demand as accomplished with the instrument Solar Auto-Calibrating EUV/UV Spectrometers (SolACES) aboard the payload SOLAR at 12 G. Schmidtke: Extreme ultraviolet spectral irradiance measurements the Columbus Module of the International Space Station (Schmidtke et al, 2006a(Schmidtke et al, , 2014 as shown in Figs. 22a-d.…”

Section: Euv-ssi Data Derived After the Year 2000mentioning

confidence: 99%

“…-SOLAR/SolACES (Schmidtke et al, 2006a(Schmidtke et al, , 2014: since the launch of the payload SOLAR on 8 February 2008 with the SolACES, it measures SSI EUV data in the spectral range from 16 to 150 nm. The mission is extended to February 2017.…”

Section: Euv-ssi Data Derived After the Year 2000mentioning

confidence: 99%

“…Hence, today's primary requirement is achieving the highest possible radiometric accuracy with minimum efforts on determining efficiency changes in order to increase the working time for science. Following the credo of the author applying ionization chambers as performed with SolACES (Schmidtke et al, 2014), the radiometric accuracy can be improved to 3-5 % depending on wavelength. In this way cross-calibration can be realized between SolACES-like instruments and others used for solar-terrestrial and/or solar research.…”

Section: Conclusion and Future Needsmentioning

confidence: 99%

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Extreme ultraviolet spectral irradiance measurements since 1946

Schmidtke

2015

Hist. Geo Space. Sci.

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Abstract. In the physics of the upper atmosphere the solar extreme ultraviolet (EUV) radiation plays a dominant role controlling most of the thermospheric/ionospheric (T/I) processes. Since this part of the solar spectrum is absorbed in the thermosphere, platforms to measure the EUV fluxes became only available with the development of rockets reaching altitude levels exceeding 80 km. With the availability of V2 rockets used in space research, recording of EUV spectra started in 1946 using photographic films. The development of pointing devices to accurately orient the spectrographs toward the sun initiated intense activities in solar-terrestrial research. The application of photoelectric recording technology enabled the scientists placing EUV spectrometers aboard satellites observing qualitatively strong variability of the solar EUV irradiance on short-, medium-, and longterm scales. However, as more measurements were performed more radiometric EUV data diverged due to the inherent degradation of the EUV instruments with time. Also, continuous recording of the EUV energy input to the T/I system was not achieved. It is only at the end of the last century that there was progress made in solving the serious problem of degradation enabling to monitore solar EUV fluxes with sufficient radiometric accuracy. The data sets available allow composing the data available to the first set of EUV data covering a period of 11 years for the first time. Based on the sophisticated instrumentation verified in space, future EUV measurements of the solar spectral irradiance (SSI) are promising accuracy levels of about 5 % and less. With added low-cost equipment, real-time measurements will allow providing data needed in ionospheric modeling, e.g., for correcting propagation delays of navigation signals from space to earth. Adding EUV airglow and auroral emission monitoring by airglow cameras, the impact of space weather on the terrestrial T/I system can be studied with a spectral terrestrial irradiance camera (STI-Cam) and also be used investigating real-time space weather effects and deriving more detailed correction procedures for the evaluation of Global Navigation Satellite System (GNSS) signals. Progress in physics goes with achieving higher accuracy in measurements. This review historically guides the reader on the ways of exploring the impact of the variable solar radiation in the extreme ultraviolet spectral region on our upper atmosphere in the altitude regime from 80 to 1000 km.

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“…Solid blue dots are added that show the time lag with maximum correlation which can, however, only be provided at an accuracy of one day. We also analyzed a EUV-TEC proxy after Unglaub et al (2011), based on the combined SDO/EVE and SolACES (Schmidtke et al, 2014) spectra in this wavelength interval. EUV-TEC is calculated as the primary ionization using a NRLMSISE-00 (Picone et al, 2002) Sun and Solar Activity 31 Figure 2 shows that at short time scales of few days, the correlation is weak.…”

mentioning

confidence: 99%

Book of Proceedings: Seventh Workshop, Sunny Beach, Bulgaria, 1-5 June 2015

2015

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Kalinichenko, A.A. Konovalenko1 A.I.Brazhenko, V.V. Solov'ev CME Bubnov, A.A. Stanislavsky, A.A. Konovalenko, S. Yerin, A.A. Gridin, A.A. Koval Advances in solar bursts observations by the low-frequency radio telescopes of a new age Abstract.The GOES data for the flare proton energies of 10 -100 MeV are analyzed. Proton fluxes ~ 10 32 acceleration takes at the current sheet decay. Proton acceleration of in a flare occurs along a singular line of the current sheet by the Lorentz electric field, as in the pinch gas discharge. The pulse of protons duration is by 2 -3 orders of magnitude longer than the duration of flares. The high-energy proton flow from the flares that appear on the Western part of the solar disk arrive to Earth with the time of flight. These particles propagate along magnetic lines of the Archimedes spiral connecting the flare with the Earth. Protons from the flare on the Eastern part of the solar disk begin to register with a delay of more than three hours. Such particles cannot get on the magnetic field line connecting the flare with the Earth. These protons reach the Earth, moving across the interplanetary magnetic field. The particles captured by the magnetic field of the solar wind are transported with solar wind and due to diffusion across the magnetic field. The patterns of solar cosmic rays generation demonstrated in this report are not detected during the small (Ф ≤ 1 см -2 с -1 стер -1 ) proton events. IntroductionAbout 30% of big flares (class X and even less class M) are accompanied by a flux of relativistic protons. Part of these protons hits the Sun and causes nuclear reactions. The other part of the protons propagates into the interplanetary medium. Despite decades of the effort, the relativistic flare protons remain the least studied manifestation of the flare [1]. The energy of the charged particles in the interplanetary plasma can change only due to the emission or movement along the electric field MdV/dt = eE + e[V×B]/c. The change of the energy of a particle moving in the field is dW = eE r dr. The electric field may be of different origin: the field of another charged particle (at a collision), space charge field, in particular due to polarization of charges in the plasma, the field induction dB/dt, etc. At the scattering by inhomogeneities of the magnetic field the particle can change the energy only due to motion in the electric field associated with a magnetic field fluctuation. This was clearly articulated in the well known work of Berezhko E. G., and Krymsky G. F. [2]: "Possibility of charged particles acceleration in the plasma in the related electric fields." The change of the energy at scattering by a magnetic fluctuation is determined by the magnitude and spatial scale of the electric field in such fluctuations Two possibilities of solar cosmic rays generation are discussed in the literature: a). Proton acceleration in the Lorentz electric field E rec = -V rec ×B cs /c along the singular lines (in particular the line B=0) in the current sheet during magnetic r...

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Solar EUV Irradiance Measurements by the Auto-Calibrating EUV Spectrometers (SolACES) Aboard the International Space Station (ISS)

Cited by 32 publications

References 15 publications

Calibration of space instruments at the Metrology Light Source

Calibration of space instruments at the Metrology Light Source

Extreme ultraviolet spectral irradiance measurements since 1946

Book of Proceedings: Seventh Workshop, Sunny Beach, Bulgaria, 1-5 June 2015

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