Achievements of Hinode in the first eleven years

Al-Janabi, K.; Antolin, Patrick; Baker, D.; Rubio, L. R. Bellot; Bradley, L.; Brooks, David H.; Centeno, R.; Culhane, J. L.; Zanna, G. Del; Doschek, G. A.; Fletcher, L.; Hara, Hirohisa; Harra, L. K.; Hillier, Andrew; Imada, Shinsuke; Klimchuk, J. A.; Mariska, J. T.; Pereira, Tiago M. D.; Reeves, Katharine K.; Sakao, Taro; Sakurai, Takashi; Shimizu, Toshifumi; Shimojo, Masataka; Shiota, Daikou; Solanki, S. K.; Sterling, Alphonse C.; Su, Yingna; Suematsu, Y.; Tarbell, T. D.; Tiwari, Sanjiv K.; Toriumi, Shin; Ugarte-Urra, Ignacio; Warren, H. P.; Watanabe, Tetsuya; Young, Peter R.

doi:10.1093/pasj/psz084

Cited by 86 publications

(32 citation statements)

References 1,151 publications

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“…A number of investigations have studied the on-disk source region of coronal jets, including the magnetic field properties at the base of the jets (e.g., Shimojo et al 1998;Huang et al 2012;Shen et al 2012Shen et al , 2017Young & Muglach 2014a;Adams et al 2014;Panesar et al 2016;Muglach 2021). See Shimojo & Shibata (2000), Raouafi et al (2016), Hinode Review Team et al (2019, and Shen (2021) for summaries and reviews of coronal jets.…”

Section: Introductionmentioning

confidence: 99%

Further Evidence for the Minifilament-Eruption Scenario for Solar Polar Coronal Jets

Baikie,

Sterling,

Moore

et al. 2022

Preprint

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We examine a sampling of 23 polar-coronal-hole jets. We first identified the jets in soft X-ray (SXR) images from the X-ray telescope (XRT) on the Hinode spacecraft, over 2014-2016. During this period, frequently the polar holes were small or largely obscured by foreground coronal haze, often making jets difficult to see. We selected 23 jets among those adequately visible during this period, and examined them further using Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) 171, 193, 211, and 304 Å images. In SXRs we track the lateral drift of the jet spire relative to the jet base's jet bright point (JBP). In 22 of 23 jets the spire either moves away from (18 cases) or is stationary relative to (4 cases) the JBP. The one exception where the spire moved toward the JBP may be a consequence of line-of-sight projection effects at the limb. From the AIA images, we clearly identify an erupting minifilament in 20 of the 23 jets, while the remainder are consistent with such an eruption having taken place. We also confirm that some jets can trigger onset of nearby "sympathetic" jets, likely because eruption of the minifilament field of the first jet removes magnetic constraints on the base-field region of the second jet. The propensity for spire drift away from the JBP, the identification of the erupting minifilament in the majority of jets, and the magnetic-field topological changes that lead to sympathetic jets, all support or are consistent with the minifilament-eruption model for jets.

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Section: Introductionmentioning

confidence: 99%

Further Evidence for the Minifilament-Eruption Scenario for Solar Polar Coronal Jets

Baikie,

Sterling,

Moore

et al. 2022

Preprint

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“…One way to disentangle intrinsic magnetic oscillations in the solar atmosphere is through the investigation of the phase lag between the polarization signals associated with magnetic field disturbances and other physical quantities such as intensity and Doppler velocity (Stangalini et al 2018(Stangalini et al , 2021. Oscillating physical quantities associated with MHD waves may have different phase relations depending on the MHD mode and the propagation state of the wave (Fujimura & Tsuneta 2009;Hinode Review Team et al 2019), thus the analysis of the phase relations between them can be exploited for their identification (Stangalini et al 2018) as well as the identification of the specific mode producing them.…”

Section: Introductionmentioning

confidence: 99%

Alfvénic Perturbations in a Sunspot Chromosphere Linked to Fractionated Plasma in the Corona

Baker

Stangalini

Valori

et al. 2021

ApJ

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In this study, we investigate the spatial distribution of highly varying plasma composition around one of the largest sunspots of solar cycle 24. Observations of the photosphere, chromosphere, and corona are brought together with magnetic field modeling of the sunspot in order to probe the conditions that regulate the degree of plasma fractionation within loop populations of differing connectivities. We find that, in the coronal magnetic field above the sunspot umbra, the plasma has photospheric composition. Coronal loops rooted in the penumbra contain fractionated plasma, with the highest levels observed in the loops that connect within the active region. Tracing field lines from regions of fractionated plasma in the corona to locations of Alfvénic fluctuations detected in the chromosphere shows that they are magnetically linked. These results indicate a connection between sunspot chromospheric activity and observable changes in coronal plasma composition.

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“…Observationally, MHD waves in the solar atmosphere are commonly identified as intensity and velocity oscillations [11,[25][26][27][28][29][30][31], although associated magnetic field oscillations are also expected from theory [1,2]. These quantities may have different phase relations depending on the MHD mode and the propagation state of the wave [32][33][34][35]. It is worth noting that the relevance of magnetic field perturbations goes well beyond the MHD wave field.…”

Section: Introductionmentioning

confidence: 99%

“…Recently, it was shown that magnetic perturbations may give rise to, through the generation of the ponderomotive force, the well-known FIP (first ionization potential) effect, an elemental abundance anomaly observed in the corona of the Sun and other Sun-like stars [36]. In recent years, and most notably with the in situ observations expected from the Solar Orbiter mission [37], the FIP effect has acquired new relevance as a powerful diagnostic of the solar wind, especially useful for linking the solar wind to its source regions [35,38].…”

Section: Introductionmentioning

confidence: 99%

Spectropolarimetric fluctuations in a sunspot chromosphere

Stangalini

Baker

Valori

et al. 2020

Phil. Trans. R. Soc. A.

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The instrumental advances made in this new era of 4 m class solar telescopes with unmatched spectropolarimetric accuracy and sensitivity will enable the study of chromospheric magnetic fields and their dynamics with unprecedented detail. In this regard, spectropolarimetric diagnostics can provide invaluable insight into magneto-hydrodynamic (MHD) wave processes. MHD waves and, in particular, Alfvénic fluctuations associated with particular wave modes were recently recognized as important mechanisms not only for the heating of the outer layers of the Sun’s atmosphere and the acceleration of the solar wind, but also for the elemental abundance anomaly observed in the corona of the Sun and other Sun-like stars (also known as first ionization potential) effect. Here, we take advantage of state-of-the-art and unique spectropolarimetric Interferometric BIdimensional Spectrometer observations to investigate the relation between intensity and circular polarization (CP) fluctuations in a sunspot chromosphere. Our results show a clear link between the intensity and CP fluctuations in a patch which corresponds to a narrow range of magnetic field inclinations. This suggests the presence of Alfvénic perturbations in the sunspot. This article is part of the Theo Murphy meeting issue ‘High-resolution wave dynamics in the lower solar atmosphere’.

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Achievements of Hinode in the first eleven years

Cited by 86 publications

References 1,151 publications

Further Evidence for the Minifilament-Eruption Scenario for Solar Polar Coronal Jets

Further Evidence for the Minifilament-Eruption Scenario for Solar Polar Coronal Jets

Alfvénic Perturbations in a Sunspot Chromosphere Linked to Fractionated Plasma in the Corona

Spectropolarimetric fluctuations in a sunspot chromosphere

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