Wavelet Decomposition of Submillimeter Solar Radio Bursts

Махмутов, В. С.; Raulin, Jean-Pierre; Castro, C. G. Giménez de; Kaufmann, P.; Correia, E.

doi:10.1023/b:sola.0000013047.26419.33

Cited by 17 publications

(5 citation statements)

References 26 publications

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“…Gaizauskas and Tapping 1980;Kaufmann et al 1980;Raulin et al 1998). Since the operation of the SST, similar pulses have been observed at sub-mm (Kaufmann et al, 2001Makhmutov et al 2003;Raulin et al 2003;Silva et al 2007). We note that the direct comparison of THz and microwave/mm-wave pulse structures has been difficult due to the typical flux saturation at microwaves during powerful events.…”

Section: Fast Time Variationsmentioning

confidence: 54%

Solar flares at submillimeter wavelengths

Krucker

Castro

Hudson

et al. 2013

Astron Astrophys Rev

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International audienceWe discuss the implications of the first systematic observations of solar flares at submillimeter wavelengths, defined here as observing wavelengths shorter than 3 mm (frequencies higher than 0.1 THz). The events observed thus far show that this wave band requires a new understanding of high-energy processes in solar flares. Several events, including observations from two different observatories, show during the impulsive phase of the flare a spectral component with a positive (increasing) slope at the highest observable frequencies (up to 405 GHz). To emphasize the increasing spectra and the possibility that these events could be even more prominent in the THz range, we term this spectral feature a "THz component". Here we review the data and methods, and critically assess the observational evidence for such distinct component(s). This evidence is convincing. We also review the several proposed explanations for these feature(s), which have been reported in three distinct flare phases. These data contain important clues to flare development and particle acceleration as a whole, but many of the theoretical issues remain open. We generally have lacked systematic observations in the millimeter-wave to far-infrared range that are needed to complete our picture of these events, and encourage observations with new facilities

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Section: Fast Time Variationsmentioning

confidence: 54%

Solar flares at submillimeter wavelengths

Krucker

Castro

Hudson

et al. 2013

Astron Astrophys Rev

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“…Moreover, the different timescales do not seem to form a continuum (from short to long timescales, for example), but many times shorter timescales appear as disconnected from the underlying longer timescale structures. Such changes through the flare time history are being reported and studied in more detail elsewhere for this event, as well as for other submillimeter events observed by the SST (Makhmutov et al 2003).…”

Section: Discussionmentioning

confidence: 75%

Properties of Fast Submillimeter Time Structures during a Large Solar Flare

Raulin

Kaufmann

Castro

et al. 2003

ApJ

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We report properties of fast varying submillimeter emission during one of the strongest solar radio flares of solar cycle 23. Emission was obtained by the Solar Submillimeter-Wave Telescope at 212 and 405 GHz and compared with hard X-ray and-ray counts up to few tens of MeV photon energy ranges. We employ different methods to detect and characterize flux density variations and find that during the impulsive phase of the event, the closer in time to the peak flare, the higher the occurrence of the fastest and brightest time structures. The good comparison with hard X-ray and-ray count rates indicates that fast submillimeter pulses are the signatures of primary energetic injections. The characteristics of the fast spikes at 212 and 405 GHz, such as their flux density and localization, compared to those of the underlying slower impulsive component, also suggest that their nature is different.

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“…Observations of solar flares in the sub-THz band have shown high quality second and sub-second quasi-periodic pulsations (e.g Makhmutov et al 2003;Kaufmann et al 2009a). Thus, revealing the nature of the dependence of the flaring emission intensity on the frequency in the GHz and sub-THz band would be incomplete without quantifying them in detail and explaining the nature of quasi-periodic pulsations in this band.…”

Section: Quasi-periodic Pulsationsmentioning

confidence: 99%

Solar Science with the Atacama Large Millimeter/Submillimeter Array—A New View of Our Sun

et al. 2015

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The Atacama Large Millimeter/submillimeter Array (ALMA) is a new powerful tool for observing the Sun at high spatial, temporal, and spectral resolution. These capabilities can address a broad range of fundamental scientific questions in solar physics. The radiation observed by ALMA originates mostly from the chromosphere -a complex and dynamic region between the photosphere and corona, which plays a crucial role in the transport of energy and matter and, ultimately, the heating of the outer layers of the solar atmosphere. Based on first solar test observations, strategies for regular solar campaigns are currently being developed. State-of-the-art numerical simulations of the solar atmosphere and modeling of instrumental effects can help constrain and optimize future observing modes for ALMA. Here we present a short technical description of ALMA and an overview of past efforts and future possibilities for solar observations at submillimeter and millimeter wavelengths. In addition, selected numerical simulations and observations at other wavelengths demonstrate ALMA's scientific potential for studying the Sun for a large range of science cases.

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Wavelet Decomposition of Submillimeter Solar Radio Bursts

Cited by 17 publications

References 26 publications

Solar flares at submillimeter wavelengths

Solar flares at submillimeter wavelengths

Properties of Fast Submillimeter Time Structures during a Large Solar Flare

Solar Science with the Atacama Large Millimeter/Submillimeter Array—A New View of Our Sun

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