The Solar Optical Telescope of Solar-B (Hinode): The Optical Telescope Assembly

Suematsu, Y.; Tsuneta, S.; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Otsubo, Masahisa; Katsukawa, Y.; Nakagiri, M.; Noguchi, Motokazu; Tamura, Takuya; Kato, Yoshihiro; Hara, Hirohisa; Kubo, Masahito; Izumi, Mitsuru; Saitō, Hideo; Matsushita, Tadashi; Kawaguchi, Noboru; Nakaoji, Toshitaka; Nagae, Kazuhiro; Shimada, S.; Takeyama, Norihide; Yamamuro, Tomoyasu

doi:10.1007/s11207-008-9129-4

Cited by 367 publications

(272 citation statements)

References 7 publications

(6 reference statements)

Supporting

Mentioning

271

Contrasting

Order By: Relevance

“…The PSF, required for the spatially coupled inversion of the data, was constructed from the Hinode pupil function (Suematsu et al 2008), with 0.1 waves defocus added to account for the observed quiet sun contrast (Danilovic et al 2008). The atmospheric temperature T , line-of-sight velocity v LOS , magnetic field strength B, inclination γ and azimuth φ, and a microturbulent velocity v mic were fitted at three height nodes located at 10 log τ c = (−2.5, −0.9, 0.0) for spot 1 and 10 log τ c = (−2.5, −0.8, 0.0) for spot 2, where τ c is the optical depth of the local continuum at a wavelength of 6302.5 Å.…”

Section: Inversionsmentioning

confidence: 99%

Peripheral downflows in sunspot penumbrae

Noort

Lagg

Tiwari

et al. 2013

A&A

128

View full text Add to dashboard Cite

Context. Sunspot penumbrae show high-velocity patches along the periphery. Aims. The high-velocity downflow patches are believed to be the return channels of the Evershed flow. We aim to investigate their structure in detail using Hinode SOT/SP observations. Methods. We employ Fourier interpolation in combination with spatially coupled height dependent LTE inversions of Stokes profiles to produce high-resolution, height-dependent maps of atmospheric parameters of these downflows and investigate their properties. Results. High-speed downflows are observed over a wide range of viewing angles. They have supersonic line-of-sight velocities, some in excess of 20 km s −1 , and very high magnetic field strengths, reaching values of over 7 kG. A relation between the downflow velocities and the magnetic field strength is found, in good agreement with MHD simulations. Conclusions. The coupled inversion at high resolution allows for the accurate determination of small-scale structures. The recovered atmospheric structure indicates that regions with very high downflow velocities contain some of the strongest magnetic fields that have ever been measured on the Sun.

show abstract

Section: Inversionsmentioning

confidence: 99%

Peripheral downflows in sunspot penumbrae

Noort

Lagg

Tiwari

et al. 2013

A&A

128

View full text Add to dashboard Cite

show abstract

“…[10] In this paper, we continue the work of and apply the upward boundary integration computational scheme of DBIE method for NLFFF extrapolation to the photospheric vector magnetograms acquired by the Spectro-Polarimeter (SP) of the Solar Optical Telescope (SOT) [Tsuneta et al, 2008;Suematsu et al, 2008;Ichimoto et al, 2008;Shimizu et al, 2008] aboard Hinode satellite [Kosugi et al, 2007]. The Hinode satellite, which was formerly called Solar-B and was launched in September 2006, can obtain high-quality photospheric vector magnetograms of solar active regions by SOT-SP instrument, and the simultaneous coronal loop images of the same active regions in soft X-ray band by the X-Ray Telescope (XRT) Kano et al, 2008] as well as in extreme ultraviolet band by the EUV Imaging Spectrometer (EIS) [Culhane et al, 2007].…”

Section: Introductionmentioning

confidence: 99%

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

Wang

Yan

2011

J. Geophys. Res.

View full text Add to dashboard Cite

[1] The Hinode satellite can obtain high-quality photospheric vector magnetograms of solar active regions and the simultaneous coronal loop images in soft X-ray and extreme ultraviolet (EUV) bands. In this paper, we continue the work of and apply the newly developed upward boundary integration computational scheme for the nonlinear force-free field (NLFFF) extrapolation of the coronal magnetic field to the

show abstract

“…We chose the M-and X-class flares because WLFs are usually associated with relatively large flares, and 721 of these occurred among the 11, 387 events. We selected events that were observed using the Solar Optical Telescope (SOT) [23,24,25,26] onboard Hinode in the visible continuum bands (G-band, blue, green, and red) in the flare-observation mode (taking WL images every 20 s for each band); 101 were detected. Then, we performed statistical analyses of the hard X-ray data observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) [27].…”

Section: Event Selectionmentioning

confidence: 99%

Capability of the accelerated protons as the origin of white-light emission of solar flare

Watanabe¹,

Masuda²,

Ohno³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

View full text Add to dashboard Cite

In association with strong solar flares, we sometimes observe enhancements of visible continuum radiation, which is known as a "white-light flare". As most white-light (WL) events show close correlations in time and location with hard X-rays and/or radio emission, there is some consensus that WL emission originates from accelerated particles, especially non-thermal electrons. One model proposes that WL is emitted near the photosphere; however, non-thermal electrons are thermalized in the chromosphere and cannot reach the photosphere. Thus, there is a problem: how can the energy of non-thermal electrons − and/or other accelerated particles such as high-energy protons − propagate to the photosphere and produce WL emission? In the present study, we investigate the possibility that accelerated protons may produce the WL emission of solar flares. We found 51 WL events observed by Hinode/SOT. Among them, gamma-rays with energies greater than 1 MeV were observed only in the X1.8-class flare on October 23, 2012 and in the M7.9-class flare on June 25, 2015. Focusing on these flare events, we compare the energetics of WL emission and of accelerated ion fluxes. We find that it is difficult for accelerated ions to provide sufficient energy to account for WL emission.

show abstract

The Solar Optical Telescope of Solar-B (Hinode): The Optical Telescope Assembly

Cited by 367 publications

References 7 publications

Peripheral downflows in sunspot penumbrae

Peripheral downflows in sunspot penumbrae

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

Capability of the accelerated protons as the origin of white-light emission of solar flare

Contact Info

Product

Resources

About