White paper of the "soft X-ray imaging spectroscopy"

Narukage, Noriyuki; Ishikawa, Shin-­nosuke; Kawate, Tomoko; Imada, Shinsuke; Sakao, Taro

doi:10.48550/arxiv.1706.04536

Cited by 2 publications

(3 citation statements)

References 12 publications

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“…In combination with EUV and HXR observations, SXR imaging spectroscopy will greatly enhance our knowledge of the DEM of active regions. Recently, the FOXSI-3 sounding rocket flight successfully performed SXR photon-counting imaging spectroscopy observations of the solar corona demonstrating the scientific potential and technical feasibility to build a satellite mission Physics of Energetic and Non-thermal plasmas in the X region (PhoENiX) with a similar SXR imaging spectroscopy instrument (Narukage et al 2017).…”

Section: Discussionmentioning

confidence: 99%

Hot Plasma in a Quiescent Solar Active Region as Measured by RHESSI, XRT, and AIA

Ishikawa

Krucker

2019

ApJ

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This paper investigates a quiescent (non-flaring) active region observed on July 13, 2010 in EUV, SXR, and HXRs to search for a hot component that is speculated to be a key signature of coronal heating. We use a combination of RHESSI imaging and long-duration time integration (up to 40 min) to detect the active regions in the 3-8 keV range during apparently non-flaring times. The RHESSI imaging reveals a hot component that originates from the entire active region, as speculated for a nanoflare scenario where the entire active region is filled with a large number of unresolved small energy releases. An isothermal fit to the RHESSI data gives temperatures around ∼7 MK with emission measure of several times 10 46 cm −3 . Adding EUV and SXR observations taken by AIA and XRT, respectively, we derive a differential emission measure (DEM) that shows a peak between 2 and 3 MK with a steeply decreasing high-temperture tail, similar to what has been previously reported. The derived DEM reveals that a wide range of temperatures contributes to the RHESSI flux (e.g. 40% of the 4 keV emission being produced by plasma below 5 MK, while emission at 7 keV is almost exclusively from plasmas above 5 MK) indicating that the RHESSI spectrum should not be fitted with an isothermal. The hot component has a rather small emission measure (∼0.1% of the total EM is above 5 MK), and the derived thermal energy content is of the order of 10% for a filling factor of unity, or potentially below 1% for smaller filling factors.

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Section: Discussionmentioning

confidence: 99%

Hot Plasma in a Quiescent Solar Active Region as Measured by RHESSI, XRT, and AIA

Ishikawa

Krucker

2019

ApJ

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“…The corona emits X-rays, and its observations are important in understanding the physical processes of such phenomena. X-ray imaging spectroscopy is a desirable tool in deriving physical parameters such as temperature, emission measures, and spectral slope from a plasma with non-thermal energy distribution [2]. However, imaging spectroscopy of the Sun in the soft X-ray energy range of <10 keV, which is a typical energy range of the coronal emission, have not been fully developed yet owing to technical difficulties.…”

Section: Introductionmentioning

confidence: 99%

“…Since timescales of the coronal energy release phenomena are as short as a few tens of seconds, we must develop a spectrum in similar timescales to investigate such phenomena by X-ray imaging spectroscopy observations. High-speed single photon-counting techniques are a possible solution for the measurement of the energy of each X-ray photon [2,3]. To achieve this solution, we must measure the energy of more than one thousand X-ray photons in a region of interest every tens of seconds.…”

Section: Introductionmentioning

confidence: 99%

High-speed X-ray imaging spectroscopy system with Zynq SoC for solar observations

Ishikawa

Takahashi

Watanabe

et al. 2018

Nuclear Instruments and Methods in Physics Research Section A:

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We have developed a system combining a back-illuminated Complementary-Metal-Oxide-Semiconductor (CMOS) imaging sensor and Xilinx Zynq System-on-Chip (SoC) device for a soft X-ray (0.5-10 keV) imaging spectroscopy observation of the Sun to investigate the dynamics of the solar corona. Because typical timescales of energy release phenomena in the corona span a few minutes at most, we aim to obtain the corresponding energy spectra and derive the physical parameters, i.e., temperature and emission measure, every few tens of seconds or less for future solar X-ray observations. An X-ray photon-counting technique, with a frame rate of a few hundred frames per second or more, can achieve such results. We used the Zynq SoC device to achieve the requirements. Zynq contains an ARM processor core, which is also known as the Processing System (PS) part, and a Programmable Logic (PL) part in a single chip. We use the PL and PS to control the sensor and seamless recording of data to a storage system, respectively. We aim to use the system for the third flight of the Focusing Optics Solar X-ray Imager (FOXSI-3) sounding rocket experiment for the first photon-counting X-ray imaging and spectroscopy of the Sun.

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White paper of the "soft X-ray imaging spectroscopy"

Cited by 2 publications

References 12 publications

Hot Plasma in a Quiescent Solar Active Region as Measured by RHESSI, XRT, and AIA

Hot Plasma in a Quiescent Solar Active Region as Measured by RHESSI, XRT, and AIA

High-speed X-ray imaging spectroscopy system with Zynq SoC for solar observations

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