The Hinode (Solar-B) Mission: An Overview

Kosugi, T.; Matsuzaki, Keiichi; Sakao, Taro; Shimizu, T.; Sone, Yoshitsugu; Tachikawa, Sumitaka; Hashimoto, Tatsuaki; Minesugi, Kenji; Ohnishi, Akira; Yamada, Takahiro; Tsuneta, S.; Hara, Hirohisa; Ichimoto, Kiyoshi; Suematsu, Y.; Shimojo, Masataka; Watanabe, T.; Shimada, S.; Davis, John M.; Hill, L. D.; Owens, J. K.; Title, A. M.; Culhane, J. L.; Harra, L. K.; Doschek, G. A.; Golub, L.

doi:10.1007/978-0-387-88739-5_3

Cited by 99 publications

(106 citation statements)

References 13 publications

(1 reference statement)

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“…There are additional instrumental artifacts that may or may not be mitigated fully. In this section, some rudimentary evaluation of the evolution of AR #11158 features are discussed in light of the limitations of the data, and a brief qualitative comparison is presented with simultaneous observations from the Hinode/SpectroPolarimeter (Kosugi et al, 2007;Tsuneta et al, 2008;Lites et al, 2013). Comparisons beyond the qualitative presentations made here are beyond the scope of this paper.…”

Section: Limits and Validationmentioning

confidence: 99%

The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance

et al. 2014

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The Helioseismic and Magnetic Imager (HMI) began near-continuous full-disk solar measurements on 1 May 2010 from the Solar Dynamics Observatory (SDO). An automated processing pipeline keeps pace with observations to produce observable quantities, including the photospheric vector magnetic field, from sequences of filtergrams. The basic vector-field frame list cadence is 135 seconds, but to reduce noise the filtergrams are combined to derive data products every 720 seconds. The primary 720 s observables were released in mid-2010, including Stokes polarization parameters measured at six wavelengths, as well as intensity, Doppler velocity, and the line-of-sight magnetic field. More advanced products, including the full vector magnetic field, are now available. Automatically identified HMI Active Region Patches (HARPs) track the location and shape of magnetic regions throughout their lifetime.The vector field is computed using the Very Fast Inversion of the Stokes Vector (VFISV) code optimized for the HMI pipeline; the remaining 180 • azimuth ambiguity is resolved with the Minimum Energy (ME0) code. The Milne-Eddington inversion is performed on all full-disk HMI observations. The disambiguation, until recently run only on HARP regions, is now implemented for the full disk. Vector and scalar quantities in the patches are used to derive active region indices potentially useful for forecasting; the data maps and indices are collected in the SHARP data series, hmi.sharp_720s. Definitive SHARP processing is completed only after the region rotates off the visible disk; quick-look products are produced in near real time. Patches are provided in both CCD and heliographic coordinates.HMI provides continuous coverage of the vector field, but has modest spatial, spectral, and temporal resolution. Coupled with limitations of the analysis and interpretation techniques, effects of the orbital velocity, and instrument performance, the resulting measurements have a certain dynamic range and sensitivity and are subject to systematic errors and uncertainties that are characterized in this report.

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Section: Limits and Validationmentioning

confidence: 99%

The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance

et al. 2014

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“…An example of this type of PCS is the correlation tracker and the tip-tilt mirror system (CTM) used in solar optical telescope of SOLAR-B (Hinode). 2 The disturbance transfer function of the assumed PCS is as follows, where the dead time delay is approximated by the first order ordinary delay:…”

Section: Transient Response Of Pointing Error With Pcsmentioning

confidence: 99%

“…As a matter of fact, internal disturbances are often the largest sources of LOS pointing error in a satellite that requires very high pointing stability of the optical payload. 2,3) However, specifying internal disturbances is neither simple nor straightforward, because the disturbance forces/torques as well as their transfer characteristics affect the final performance.…”

Section: Introductionmentioning

confidence: 99%

Proposed Criteria and Control Parameters for Transient Internal Disturbances in Spacecraft

Yoshida

2014

AEROSPACE TECHNOLOGY JAPAN

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Spacecraft internal disturbances are defined as internal forces or torques generated within the spacecraft that produce undesirable movement or behavior of the mission payload and/or the spacecraft. The line-of-sight pointing error of the optical payload caused by internal disturbances is often one of the most critical issues for a satellite with very high payload pointing requirements. The control and management of internal disturbances are, however, not simple, since disturbance forces and torques as well as their transfer characteristics affect the final performance. The transfer characteristics are strongly related to the attitude/structural dynamics, the attitude/pointing control system and the optical properties, and are therefore also affected by the properties of the disturbance itself. Consequently, for a given target performance, the individual disturbance sources must be specified, taking all these factors into consideration. In this paper, it is discussed how to specify transient disturbances, and a set of control parameters is proposed.

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“…Recently, the Hinode (formerly called Solar-B; Kosugi et al 2007), which is a Japanese solar mission for high-resolution observation from the photosphere to the corona, was launched on 2006 September 22. The main purpose of Hinode is to address key questions in solar physics such as coronal heating, driving mechanism of explosive events, and source of the solar magnetic fields.…”

Section: Introductionmentioning

confidence: 99%

Estimation of Spicule Magnetic Field Using Observed MHD Waves by the Hinode Sot

Kim

Bong²,

Park³

et al. 2008

Journal of The Korean Astronomical Society

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Using the MHD coronal seismology technique, we estimated the magnetic field for three spicules observed in 2008 June. For this study, we used the high resolution Ca II H line (3968.5Å) images observed by the Hinode SOT and considered a vertical thin flux tube as a spicule model. To our knowledge, this is the first attempt to estimate the spicule magnetic field using the Hinode observation. From the observed oscillation properties, we determined the periods, amplitudes, minimum wavelengths, and wave speeds. We interpreted the observed oscillations as MHD kink waves propagating through a vertical thin flux tube embedded in a uniform field environment. Then we estimated spicule magnetic field assuming spicule densities. Major results from this study are as follows : (1) we observed three oscillating spicules having durations of 5-7 minutes, oscillating periods of 2-3 minutes, and transverse displacements of 700-1000 km. (2) The estimated magnetic field in spicules is about 10-18 G for lower density limit and about 43-76 G for upper density limit. (3) In this analysis, we can estimate the minimum wavelength of the oscillations, such as 60000 km, 56000 km, and 45000 km. This may be due to the much longer wavelength comparing with the height of spicules. (4) In the first event occurred on 2008 June 03, the oscillation existed during limited time (about 250 s). This means that the oscillation may be triggered by an impulsive mechanism (like low atmospheric reconnection), not continuous. Being compared with the ground-based observations of spicule oscillations, our observation indicates quite different one, i.e., more than one order longer in wavelength, a factor of 3-4 larger in wave speed, and 2-3 times longer in period.

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The Hinode (Solar-B) Mission: An Overview

Abstract: Abstract:The Hinode satellite (formerly Solar-

Cited by 99 publications

References 13 publications

The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance

The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance

Proposed Criteria and Control Parameters for Transient Internal Disturbances in Spacecraft

Estimation of Spicule Magnetic Field Using Observed MHD Waves by the Hinode Sot

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