Atm observations, X-ray results

Vaiana, G. S.; Krieger, A. S.; Timothy, A. F.; Zombeck, Martin V.

doi:10.1007/bf00640511

Cited by 68 publications

(56 citation statements)

References 10 publications

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“…Willson (1979, 1980) Weak or undetectable radio emission was found in the regions directly over%u 6 lying sunspots; but two small (' 10"), bright (ru 10 K) radio sources were found at the outer edges of one sunspot where the magnetic field gradient is large. Our observations are consistent with X-ray observations from rockets and the Skylab mission which indicate that a hot, dense plasma is contained within the arches of magnetic loops (Friedman, 1961, 'andini, Fossi, Krieger andVaiana, 1975;Vaiana, Krieger, Timothy and Zombeck, 1976;Vaiana and Rosner, 1978).…”

Section: S6supporting

confidence: 89%

“…The X-ray observations indicate T A 2.5 x 10 K and fN 2 dk; 2 x 10 cm e e for the hot plasma trapped in magnetic arches above other active regions (Landini, Fossi, Krieger and Vaiana, 1975;Vajana, 1976;Vaiana, Krieger, Timothy and Zombeck, 1976;Vaiana and Rosner, 1978). Assuming that the vertical extent, L, of the radio emitting region is equal to the scale height 6 ~t10 at 10 K, we have L 1 10 cm and an average electron density, Ne' of…”

Section: -5mentioning

confidence: 95%

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V.L.A. Observations of Solar-Active Regions. I. The Slowly Varying Component,

Felli¹,

Lang²,

Willson³

1980

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Section: S6supporting

confidence: 89%

Section: -5mentioning

confidence: 95%

V.L.A. Observations of Solar-Active Regions. I. The Slowly Varying Component,

Felli¹,

Lang²,

Willson³

1980

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“…However, the high res olution rocket and satellite observations have confirmed this supposition and led to the realization that the magnetic field topology dominates the entire solar atmosphere Noci 1973;Pneuman 1973;Tousey et al 1973;Vaiana et al 1973). …”

Section: Magnetic Fields and Active Region Structurementioning

confidence: 99%

“…Temporal Variations Vaiana and Rosner (1978) point out that there are no distinctly de fined time scales in the corona, even including flare events. There is complete continuum of time scales in the evolution of loops.…”

Section: 2mentioning

confidence: 99%

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Microwave, EUV, and X-ray Observations of Active Region Loops and Filaments

Schmahl

1980

Symp. - Int. Astron. Union

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IntroductionIn the early years of centimetrie radio astronomy, even before high resolution techniques were available, it was found that the apparent brightness temperature of the full disk is made up of a back ground level (the so-called quiet sun temperature) added to which is a contribution roughly proportional to the sum of the sunspot areas on the disk ( Hence the core emission are strictly a centimeter wavelength phenomenon.Until the advent of x-ray and EUV observations of coronal struc tures, radio observers were forced to rely on eclipse and coronagraph observations in white light and forbidden coronal lines for additional diagnostics of the high temperature microwave sources. While these data provided enough material for theoretical insight into the physics of active regions, there was no way to make direct, simultaneous com parison of coronal structures on the disk as seen at microwave and optical wavelengths.

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Soft X‐ray irradiance measured by the Solar Aspect Monitor on the Solar Dynamic Observatory Extreme ultraviolet Variability Experiment

et al. 2016

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The Solar Aspect Monitor (SAM) is a pinhole camera on the Extreme ultraviolet Variability Experiment (EVE) aboard the Solar Dynamics Observatory. SAM projects the solar disk onto the CCD through a metallic filter designed to allow only solar photons shortward of 7 nm to pass. Contamination from energetic particles and out‐of‐band irradiance is, however, significant in the SAM observations. We present a technique for isolating the 0.01–7 nm integrated irradiance from the SAM signal to produce the first results of broadband irradiance for the time period from May 2010 to May 2014. The results of this analysis agree with a similar data product from EVE's EUV SpectroPhotometer to within 25%. We compare our results with measurements from the Student Nitric Oxide Explorer Solar X‐ray Photometer and the Thermosphere Ionosphere Mesosphere Energetics and Dynamics Solar EUV Experiment at similar levels of solar activity. We show that the full‐disk SAM broadband results compared well to the other measurements of the 0.01–7 nm irradiance. We also explore SAM's capability toward resolving spatial contribution from regions of solar disk in irradiance and demonstrate this feature with a case study of several strong flares that erupted from active regions on 11 March 2011.

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Atm observations, X-ray results

Cited by 68 publications

References 10 publications

V.L.A. Observations of Solar-Active Regions. I. The Slowly Varying Component,

V.L.A. Observations of Solar-Active Regions. I. The Slowly Varying Component,

Microwave, EUV, and X-ray Observations of Active Region Loops and Filaments

Soft X‐ray irradiance measured by the Solar Aspect Monitor on the Solar Dynamic Observatory Extreme ultraviolet Variability Experiment

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