The New 30 THz Solar Telescope in São Paulo, Brazil

Kudaka, A. S.; Cassiano, M. M.; Marcon, R.; Cabezas, Denis P.; Fernandes, L. O. T.; Ramirez, R. F. Hidalgo; Kaufmann, P.; Souza, R. V. de

doi:10.1007/s11207-015-0749-1

Cited by 4 publications

(6 citation statements)

References 20 publications

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“…A GOES SXR flare of class M2 was reported by NOAA Space Weather Prediction Center 1 on 1 August 2014 (14:43/14:48/14:57 UT) in active region 12130 (S09E35). This was the first impulsive burst observed by the new 30 THz telescope in Brazil (Kudaka et al 2015). It was also observed at Hα by the H-Alpha Solar Telescope of Argentina (HASTA; Bagalá et al 1999) and at sub-mm wavelengths by Solar Submillimeter-wave Telescope (SST; Kaufmann et al 2008).…”

Section: Observationsmentioning

confidence: 86%

“…We report here the first 30 THz impulsive flare observed by the new São Paulo telescope (Kudaka et al 2015). This event exhibits more complex spatial and temporal relationships between the 30 THz time profile and the microwave, Hα, EUV, soft X-ray (SXR), and metric−decimetric (m−dm) emissions than was seen in the two earlier events.…”

Section: Introductionmentioning

confidence: 82%

“…The 30 THz observation and calibration methods are described in detail in Kaufmann et al (2013Kaufmann et al ( , 2015; Kudaka et al (2015). The same procedures were used here.…”

Section: Observationsmentioning

confidence: 99%

“…Article published by EDP Sciences (Kudaka et al 2015). It was also observed at Hα by the H-Alpha Solar Telescope of Argentina (HASTA; Bagalá et al 1999) and at sub-mm wavelengths by Solar Submillimeter-wave Telescope (SST; Kaufmann et al 2008 (Jiricka et al 1993), and Nançay Observation Radiospectrographique pour Fedome et l'Étude des Eruptions Solaires (ORFEES) spectrometer in France (Klein et al 2013).…”

Section: Introductionmentioning

confidence: 96%

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Comparison of 30 THz impulsive burst time development to microwaves, Hα, EUV, and GOES soft X-rays

Miteva

Kaufmann

Cabezas

et al. 2016

A&A

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The recent discovery of impulsive solar burst emission in the 30 THz band is raising new interpretation challenges. One event associated with a GOES M2 class flare has been observed simultaneously in microwaves, Hα, EUV, and soft X-ray bands. Although these new observations confirm some features found in the two prior known events, they exhibit time profile structure discrepancies between 30 THz, microwaves, and hard X-rays (as inferred from the Neupert effect). These results suggest a more complex relationship between 30 THz emission and radiation produced at other wavelength ranges. The multiple frequency emissions in the impulsive phase are likely to be produced at a common flaring site lower in the chromosphere. The 30 THz burst emission may be either part of a nonthermal radiation mechanism or due to the rapid thermal response to a beam of high-energy particles bombarding the dense solar atmosphere.

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Section: Observationsmentioning

confidence: 86%

Section: Introductionmentioning

confidence: 82%

“…The 30 THz observation and calibration methods are described in detail in Kaufmann et al (2013Kaufmann et al ( , 2015; Kudaka et al (2015). The same procedures were used here.…”

Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

See 2 more Smart Citations

Comparison of 30 THz impulsive burst time development to microwaves, Hα, EUV, and GOES soft X-rays

Miteva

Kaufmann

Cabezas

et al. 2016

A&A

Self Cite

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“…Observations at λ = 10 μm ( ν = 30 THz) were carried out with the São Paulo 30‐THz telescope (SP30T ; Kudaka et al, ) which is a Newtonian system with a 15‐cm aperture, resulting in a diffraction limit

ϑ_{d} ≃ 1 7^{′′}

. The original setup described in Kudaka et al () was changed to have now a FLIR TermoVision TM A20 M camera with a Focal Plane Array uncooled microbolometer of 160 × 120 pixels that produces interpolated digital frames of 320 × 240 pixels with a temperature accuracy ±2 °C (internal calibration) or ±2%. The optical setup ensures that the real pixels have the same size as ϑ d .…”

Section: Mid‐infrared Observationsmentioning

confidence: 99%

The 6 September 2017 X9 Super Flare Observed From Submillimeter to Mid‐IR

et al. 2018

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Active Region 12673 is the most productive active region of solar cycle 24: in a few days of early September 2017, four X‐class and 27 M‐class flares occurred. SOL2017‐09‐06T12:00, an X9.3 flare also produced a two‐ribbon white light emission across the sunspot detected by Solar Dynamics Orbiter/Helioseismic and Magnetic Imager. The flare was observed at 212 and 405 GHz with the arcminute‐sized beams of the Solar Submillimeter Telescope focal array while making a solar map and at 10 μm, with a 17 arcsec diffraction‐limited infrared camera. Images at 10 μm revealed that the sunspot gradually increased in brightness while the event proceeded, reaching a temperature similar to quiet Sun values. From the images we derive a lower bound limit of 180‐K flare peak excess brightness temperature or 7,000 sfu if we consider a similar size as the white light source. The rising phase of mid‐IR and white light is similar, although the latter decays faster, and the maximum of the mid‐IR and white light emission is ∼200 s delayed from the 15.4‐GHz peak occurrence. The submillimeter spectrum has a different origin than that of microwaves from 1 to 15 GHz, although it is not possible to draw a definitive conclusion about its emitting mechanism.

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Science development study for the Atacama Large Aperture Submillimeter Telescope (AtLAST): Solar and stellar observations

Wedemeyer,

Barta,

Brajša

et al. 2024

Open Res Europe

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Observations at (sub-)millimeter wavelengths offer a complementary perspective on our Sun and other stars, offering significant insights into both the thermal and magnetic composition of their chromospheres. Despite the fundamental progress in (sub-)millimeter observations of the Sun, some important aspects require diagnostic capabilities that are not offered by existing observatories. In particular, simultaneously observations of the radiation continuum across an extended frequency range would facilitate the mapping of different layers and thus ultimately the 3D structure of the solar atmosphere. Mapping large regions on the Sun or even the whole solar disk at a very high temporal cadence would be crucial for systematically detecting and following the temporal evolution of flares, while synoptic observations, i.e., daily maps, over periods of years would provide an unprecedented view of the solar activity cycle in this wavelength regime. As our Sun is a fundamental reference for studying the atmospheres of active main sequence stars, observing the Sun and other stars with the same instrument would unlock the enormous diagnostic potential for understanding stellar activity and its impact on exoplanets. The Atacama Large Aperture Submillimeter Telescope (AtLAST), a single-dish telescope with 50m aperture proposed to be built in the Atacama desert in Chile, would be able to provide these observational capabilities. Equipped with a large number of detector elements for probing the radiation continuum across a wide frequency range, AtLAST would address a wide range of scientific topics including the thermal structure and heating of the solar chromosphere, flares and prominences, and the solar activity cycle. In this white paper, the key science cases and their technical requirements for AtLAST are discussed.

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The New 30 THz Solar Telescope in São Paulo, Brazil

Cited by 4 publications

References 20 publications

Comparison of 30 THz impulsive burst time development to microwaves, Hα, EUV, and GOES soft X-rays

Comparison of 30 THz impulsive burst time development to microwaves, Hα, EUV, and GOES soft X-rays

The 6 September 2017 X9 Super Flare Observed From Submillimeter to Mid‐IR

Science development study for the Atacama Large Aperture Submillimeter Telescope (AtLAST): Solar and stellar observations

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