The Hard X-ray Imager (HXI) on the Advanced Space-based Solar Observatory (ASO-S)

Su, Yang; Zhang, Zhe; Gan, Weiqun; Wu, Jian; Jiang, Xian-Kai

doi:10.1007/978-981-16-4544-0_156-1

Cited by 2 publications

(2 citation statements)

References 18 publications

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“…This suggests that the white-light emissions are related to a nonthermal electron-beam heating either directly or indirectly. It is a pity that the HXR imaging for the footpoint sources cannot be obtained from Fermi/GBM or the Hard X-ray Imager (Su et al 2022) on ASO-S, the latter of which was significantly influenced by some energetic particles from background at the observation time. We speculate that some of the white-light emissions can be directly caused by the electron precipitation, whereas the secondary effects, such as the radiative back-warming and chromospheric condensation, cannot be excluded in contributing to these ribbon emissions.…”

Section: Summary and Discussionmentioning

confidence: 99%

The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE

Li,

Jing,

Song

et al. 2024

ApJL

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The white-light continuum emissions in solar flares (i.e., white-light flares) are usually observed on the solar disk but, in a few cases, off the limb. Here we present on-disk as well as off-limb continuum emissions at 3600 Å (in the Balmer continuum) in an X2.1 flare (SOL2023-03-03T17:52) and an X1.5 flare (SOL2023-08-07T20:46), respectively, observed by the White-light Solar Telescope on the Advanced Space-based Solar Observatory. These continuum emissions are seen at the ribbons for the X2.1 flare and on loops during the X1.5 event, in which the latter also appears in the decay phase. These emissions also show up in the pseudocontinuum images at Fe i λ6173 from the Helioseismic and Magnetic Imager on the Solar Dynamics Observatory. In addition, the ribbon sources in the X2.1 flare exhibit significant enhancements in the Fe i line at 6569.2 Å and the nearby continuum observed by the Chinese Hα Solar Explorer. It is found that the on-disk continuum emissions in the X2.1 flare are related to a nonthermal electron-beam heating either directly or indirectly, while the off-limb emissions in the X1.5 flare are associated with thermal plasma cooling or due to Thomson scattering. These comprehensive continuum observations provide good constraints on flare energy deposition models, which helps us to better understand the physical mechanism of white-light flares.

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Section: Summary and Discussionmentioning

confidence: 99%

The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE

Li,

Jing,

Song

et al. 2024

ApJL

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“…The Hard X-ray Imager (HXI: Zhang et al, 2019;Su et al, 2022) onboard ASO-S is an HXR imaging spectrometer observing the Sun in an energy range of ≈ 10 -300 keV with energy and angular resolutions of ≈ 16.5% at 32 keV and 3.1 , respectively. The HXI L1 data are used in the present study.…”

Section: Datamentioning

confidence: 99%

Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H$\alpha $ Solar Explorer (CHASE)

Li,

et al. 2024

Sol Phys

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Solar white-light flares are characterized by an enhancement in the optical continuum, which are usually large flares (X- and M-class flares). Here, we report a small C2.3 white-light flare (SOL2022-12-20T04:10) observed by the Advanced Space-based Solar Observatory and the Chinese H$\alpha $ α Solar Explorer (CHASE). This flare exhibits an increase of ≈ 6.4% in the photospheric Fe i line at 6569.2 Å and ≈ 3.2% in the nearby continuum. The continuum at 3600 Å also shows an enhancement of ≈ 4.7%. The white-light bright kernels are mainly located at the flare ribbons and co-spatial with nonthermal hard X-ray sources, which implies that the enhanced white-light emissions are related to nonthermal electron-beam heating. At the bright kernels, the Fe i line displays an absorption profile that has a good Gaussian shape, with a redshift up to ≈ 1.7 km s−1, while the H$\alpha $ α line shows an emission profile having a central reversal. The H$\alpha $ α line profile also shows a red or blue asymmetry caused by plasma flows with a velocity of several to tens of km s−1. It is interesting to find that the H$\alpha $ α asymmetry is opposite at the conjugate footpoints. It is also found that the CHASE continuum increase seems to be related to the change in the photospheric magnetic field. Our study provides comprehensive characteristics of a small white-light flare that help understand the energy release process of white-light flares.

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The Hard X-ray Imager (HXI) on the Advanced Space-based Solar Observatory (ASO-S)

Cited by 2 publications

References 18 publications

The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE

The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE

Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H$\alpha $ Solar Explorer (CHASE)

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