Building the world's largest optical solar telescope

Rimmelé, Thomas

doi:10.1117/2.1200712.0963

Cited by 19 publications

(22 citation statements)

References 8 publications

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“…The twisted or sheared emerging flux may carry enough magnetic free energy, some of them may be released during the flare, and the rest may contribute to the increase of the local shear. Recent three-dimensional MHD simulations ( Fan 2001;Magara & Longcope 2001, 2003Magara 2004;Manchester et al 2004) have modeled the emergence of a twisted magnetic flux tube from solar convection zone through photosphere and chromosphere into the corona. In these simulations, a twisted flux tube is initially placed in the convection zone at a depth of about a few times the photospheric pressure scale height and the central segment of the twisted tube rises buoyantly toward the photosphere (Fan 2004).…”

Section: Summary and Discussionmentioning

confidence: 99%

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Multiwavelength Study of Flow Fields in Flaring Super Active Region NOAA 10486

Deng

Guo

et al. 2006

ApJ

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We present high-resolution observations of horizontal flow fields measured by local correlation tracking from intensity images in three wavelengths, i.e., G band (GB), white light (WL), and near-infrared (NIR). The observations were obtained on 2003 October 29 within the flaring super active region NOAA 10486, which was the source of several X-class flares, including an X10 flare that occurred near the end of the observing run. The data were obtained at National Solar Observatory/Sacramento Peak ( NSO/SP) using the newly developed high-order adaptive optics (AO) system. We also use Dopplergrams and magnetograms from MDI on board SOHO to study the line-of-sight flow and magnetic field. We observe persistent and long-lived (at least 5 hr) strong horizontal and vertical shear flows (both in the order of 1 km s À1 ) along the magnetic neutral line ( NL) until the X10 flare occurred. From lower photospheric level ( NIR), the direction of the flows does not change up to the upper photosphere (GB), while the flow speeds in the shear motion regions decrease and, on the contrary, those in regions without shear motions increase with increasing altitude. Right after the X10 flare, the magnetic gradient decreased, while both horizontal and vertical shear flows dramatically enhanced near the flaring NL. Our results suggest that photospheric shear flows and local magnetic shear near the NL can increase after the flare, which may be the result of shear release in the overlying largescale magnetic system or the reflection of a twisted or sheared flux emergence carrying enough energy from the subphotosphere.

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Section: Summary and Discussionmentioning

confidence: 99%

“…The high-order AO system was used to achieve diffraction-limited imaging with a high signal-to-noise ratio ( Rimmele 2000;Rimmele et al 2003). AO-corrected data were simultaneously acquired in GB, WL, and NIR.…”

Section: High-resolution Observation In Gb Wl and Nirmentioning

confidence: 99%

Multiwavelength Study of Flow Fields in Flaring Super Active Region NOAA 10486

Deng

Guo

et al. 2006

ApJ

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“…During the acquisition, the high-order adaptive optics system of the NSO/DST (Rimmele 2004) was tracking on the pore, achieving good performance and stability. Due to the anisoplanatism, the good spatial resolution of the images degrades towards the edges of the FOV.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

High cadence spectropolarimetry of moving magnetic features observed around a pore

Criscuoli

Moro

Giannattasio

et al. 2012

A&A

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Context. Moving magnetic features (MMFs) are small-size magnetic elements that are seen to stream out from sunspots, generally during their decay phase. Several observational results presented in the literature suggest them to be closely related to magnetic filaments that extend from the penumbra of the parent spot. Nevertheless, few observations of MMFs streaming out from spots without penumbra have been reported. The literature still lacks analyses of the physical properties of these features. Aims. We investigate physical properties of monopolar MMFs observed around a small pore that had developed penumbra in the days preceding our observations and compare our results with those reported in the literature for features observed around sunspots.Methods. We analyzed NOAA 11005 during its decay phase with data acquired at the Dunn Solar Telescope in the Fe i 617.3 nm and the Ca ii 854.2 nm spectral lines with IBIS, and in the G-band. The field of view showed monopolar MMFs of both polarities streaming out from the leading negative polarity pore of the observed active region. Combining different analyses of the data, we investigated the temporal evolution of the relevant physical quantities associated with the MMFs as well as the photospheric and chromospheric signatures of these features. Results. We show that the characteristics of the investigated MMFs agree with those reported in the literature for MMFs that stream out from spots with penumbrae. Moreover, observations of at least two of the observed features suggest them to be manifestations of emerging magnetic arches.

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“…Rimmele (2004). Such sensors divide the wavefront by an array of lenslets, and each wavefront element forms a separate image on the detector.…”

Section: Introductionmentioning

confidence: 99%

Phase sensor for solar adaptive-optics

Kellerer

2011

A&A

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Context. Wavefront sensing in solar adaptive-optics is currently done with correlating Shack-Hartmann sensors, although the spatialand temporal-resolutions of the phase measurements are then limited by the extremely fast computing required to correlate the sensor signals at the frequencies of daytime atmospheric-fluctuations. Aims. To avoid this limitation, a new wavefront-sensing technique is presented, that makes use of the solar brightness and is applicable to extended sources. Methods. The wavefront is sent through a modified Mach-Zehnder interferometer. A small, central part of the wavefront is used as reference and is made to interfere with the rest of the wavefront. Results. The contrast of two simultaneously measured interference-patterns provides a direct estimate of the wavefront phase, no additional computation being required. The proposed optical layout shows precise initial alignment to be the critical point in implementing the new wavefront-sensing scheme.

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Building the world's largest optical solar telescope

Abstract: A 4m high-powered solar telescope will dissect the origins and mechanisms of the sun's magnetic fields.Continued on next page

Cited by 19 publications

References 8 publications

Multiwavelength Study of Flow Fields in Flaring Super Active Region NOAA 10486

Multiwavelength Study of Flow Fields in Flaring Super Active Region NOAA 10486

High cadence spectropolarimetry of moving magnetic features observed around a pore

Phase sensor for solar adaptive-optics

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