Evidence of photospheric vortex flows at supergranular junctions observed by FG/SOT (Hinode)

Attié, Raphaël; Innes, D. E.; Potts, H. E.

doi:10.1051/0004-6361:200811258

Cited by 85 publications

(95 citation statements)

References 12 publications

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“…The velocity magnitude in white light is consistent with the results in Krijger et al (2002) and Attie et al (2009), but smaller than those in and Roudier et al (1999). This should be the result of the different smoothing and averaging of the tracked velocity fields.…”

Section: Supergranular Horizontal Flows In the Photospheresupporting

confidence: 83%

“…This should be the result of the different smoothing and averaging of the tracked velocity fields. As mentioned in Attie et al (2009), a weaker smoothing and averaging will increase the velocity values. Our choice of the smoothing and averaging scales is a compromise between a more accurate velocity measurement and a higher resolution to distinguish flows with sharp gradient.…”

Section: Supergranular Horizontal Flows In the Photospherementioning

confidence: 89%

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Horizontal supergranule-scale motions inferred from TRACE ultraviolet observations of the chromosphere

Potts

Marsch

Attié

et al. 2010

A&A

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Aims. We study horizontal supergranule-scale motions revealed by TRACE observation of the chromospheric emission, and investigate the coupling between the chromosphere and the underlying photosphere. Methods. A highly efficient feature-tracking technique called balltracking has been applied for the first time to the image sequences obtained by TRACE (transition region and coronal explorer) in the passband of white light and the three ultraviolet passbands centered at 1700 Å, 1600 Å, and 1550 Å. The resulting velocity fields have been spatially smoothed and temporally averaged in order to reveal horizontal supergranule-scale motions that may exist at the emission heights of these passbands. Results. We find indeed a high correlation between the horizontal velocities derived in the white-light and ultraviolet passbands. The horizontal velocities derived from the chromospheric and photospheric emission are comparable in magnitude. Conclusions. The horizontal motions derived in the UV passbands might indicate the existence of a supergranule-scale magnetoconvection in the chromosphere, which may shed new light on the study of mass and energy supply to the corona and solar wind at the height of the chromosphere. However, it is also possible that the apparent motions reflect the chromospheric brightness evolution as produced by acoustic shocks which might be modulated by the photospheric granular motions in their excitation process, or advected partly by the supergranule-scale flow towards the network while propagating upward from the photosphere. To reach a firm conclusion, it is necessary to investigate the role of granular motions in the excitation of shocks through numerical modeling, and future high-cadence chromospheric magnetograms must be scrutinized.

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Section: Supergranular Horizontal Flows In the Photospheresupporting

confidence: 83%

Section: Supergranular Horizontal Flows In the Photospherementioning

confidence: 89%

Horizontal supergranule-scale motions inferred from TRACE ultraviolet observations of the chromosphere

Potts

Marsch

Attié

et al. 2010

A&A

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“…On larger spatial scales, i.e., granular sizes, vortical motions were observed by Brandt et al (1988), Tarbell et al (1991), and Title et al (1992). Signatures of photospheric vortex flows have also been observed on even larger scales such as supergranular junctions (Attie et al 2009). Vortical motions in the solar photosphere were studied by simulations (Zirker 1993, and references herein) and are understood to play an important role in the evolution of magnetic footpoints and heating in the upper solar atmosphere (Brandt et al 1988;Wang et al 1995).…”

Section: Introductionmentioning

confidence: 94%

Evidence of small-scale magnetic concentrations dragged by vortex motion of solar photospheric plasma

Balmaceda

Domínguez

Palacios³

et al. 2010

A&A

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Vortex-type motions have been measured by tracking bright points in high-resolution observations of the solar photosphere. These small-scale motions are thought to be determinant in the evolution of magnetic footpoints and their interaction with plasma and therefore likely to play a role in heating the upper solar atmosphere by twisting magnetic flux tubes. We report the observation of magnetic concentrations being dragged towards the center of a convective vortex motion in the solar photosphere from highresolution ground-based and space-borne data. We describe this event by analyzing a series of images at different solar atmospheric layers. By computing horizontal proper motions, we detect a vortex whose center appears to be the draining point for the magnetic concentrations detected in magnetograms and well-correlated with the locations of bright points seen in G-band and CN images.

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“…Recently, images from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamic Observatory (SDO) have allowed Movies are available in electronic form at http://www.aanda.org the study of solar tornados (Li et al 2012;Su et al 2012;Liu et al 2012a). The driving mechanism may be a coupling and expansion of a twisted flux rope into the coronal cavity (Li et al 2012) and/or be related to photospheric vortices at the footpoint of the tornado (Attie et al 2009;Wedemeyer-Böhm et al 2012;Su et al 2012). …”

Section: Introductionmentioning

confidence: 99%

A solar tornado triggered by flares?

Panesar

Innes

Tiwari

et al. 2013

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Context. Solar tornados are dynamical, conspicuously helical magnetic structures that are mainly observed as a prominence activity. Aims. We investigate and propose a triggering mechanism for the solar tornado observed in a prominence cavity by SDO/AIA on September 25, 2011. Methods. High-cadence EUV images from the SDO/AIA and the Ahead spacecraft of STEREO/EUVI are used to correlate three flares in the neighbouring active-region (NOAA 11303) and their EUV waves with the dynamical developments of the tornado. The timings of the flares and EUV waves observed on-disk in 195 Å are analysed in relation to the tornado activities observed at the limb in 171 Å. Results. Each of the three flares and its related EUV wave occurred within ten hours of the onset of the tornado. They have an observed causal relationship with the commencement of activity in the prominence where the tornado develops. Tornado-like rotations along the side of the prominence start after the second flare. The prominence cavity expands with the accelerating tornado motion after the third flare. Conclusions. Flares in the neighbouring active region may have affected the cavity prominence system and triggered the solar tornado. A plausible mechanism is that the active-region coronal field contracted by the "Hudson effect" through the loss of magnetic energy as flares. Subsequently, the cavity expanded by its magnetic pressure to fill the surrounding low corona. We suggest that the tornado is the dynamical response of the helical prominence field to the cavity expansion.

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Evidence of photospheric vortex flows at supergranular junctions observed by FG/SOT (Hinode)

Cited by 85 publications

References 12 publications

Horizontal supergranule-scale motions inferred from TRACE ultraviolet observations of the chromosphere

Horizontal supergranule-scale motions inferred from TRACE ultraviolet observations of the chromosphere

Evidence of small-scale magnetic concentrations dragged by vortex motion of solar photospheric plasma

A solar tornado triggered by flares?

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