Chinese Hα Solar Explorer (CHASE) – a complementary space mission to the ASO-S

Li, Chuan; Fang, Cheng; Li, Zhen; Ding, M. D.; Chen, Pengfei; Chen, Zhe; Lin, Liang-Kui; Chen, Changzheng; Chen, Changya; Tao, Hong-Jiang; You, Wei; Hao, Qing; Dai, Y.; Cheng, Xin; Guo, Yang; Hong, Jie; An, Minjie; Cheng, Weiqiang; Chen, Jianxin; Wang, Wei; Zhang, Wei

doi:10.1088/1674-4527/19/11/165

Cited by 32 publications

(9 citation statements)

References 16 publications

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“…In this Letter, we present an X1.0 WLF on 2022 October 2 well observed by the Chinese Hα Solar Explorer (CHASE; Li et al 2019Li et al , 2022, which provides spectral observations in the Fe I λ6569 and Hα lines simultaneously with a seeing-free condition. This is the first X-class flare captured by CHASE.…”

Section: Introductionmentioning

confidence: 99%

Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE

De-chao

Tian

et al. 2023

ApJL

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The heating mechanisms of solar white-light flares remain unclear. We present an X1.0 white-light flare on 2022 October 2 (SOL2022-10-02T20:25) observed by the Chinese Hα Solar Explorer that provides two-dimensional spectra in the visible light for the full solar disk with a seeing-free condition. The flare shows a prominent enhancement of ∼40% in the photospheric Fe i line at 6569.2 Å, and the nearby continuum also exhibits a maximum enhancement of ∼40%. For the continuum near the Fe i line at 6173 Å from the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, it is enhanced up to ∼20%. At the white-light kernels, the Fe i line at 6569.2 Å has a symmetric Gaussian profile that is still in absorption and the Hα line at 6562.8 Å displays a very broad emission profile with a central reversal plus a red or blue asymmetry. The white-light kernels are cospatial with the microwave footpoint sources observed by the Expanded Owens Valley Solar Array and the time profile of the white-light emission matches that of the hard X-ray emission above 30 keV from the Gamma-ray Burst Monitor (GBM) on Fermi. These facts indicate that the white-light emission is qualitatively related to a nonthermal electron beam. We also perform a radiative hydrodynamic simulation with the electron-beam parameters constrained by the hard X-ray observations from Fermi/GBM. The result reveals that the white-light enhancement cannot be well explained by a pure electron-beam heating together with its induced radiative backwarming but may need additional heating sources such as Alfvén waves.

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Section: Introductionmentioning

confidence: 99%

Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE

De-chao

Tian

et al. 2023

ApJL

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“…The CHASE mission was dubbed "Xihe" in Chinese -Goddess of the Sun. A brief introduction of the CHASE mission was previously reviewed by Li et al [15]. There have been many improvements in the satellite and scientific payload since then.…”

Section: -2mentioning

confidence: 99%

The Chinese Hα Solar Explorer (CHASE) mission: An overview

Li,

Fang,

et al. 2022

Preprint

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The Chinese Hα Solar Explorer (CHASE), dubbed "Xihe" -Goddess of the Sun, was launched on October 14, 2021 as the first solar space mission of China National Space Administration (CNSA). The CHASE mission is designed to test a newly developed satellite platform and to acquire the spectroscopic observations in the Hα waveband. The Hα Imaging Spectrograph (HIS) is the scientific payload of the CHASE satellite. It consists of two observational modes: raster scanning mode and continuum imaging mode. The raster scanning mode obtains full-Sun or region-of-interest spectral images from 6559.7 to 6565.9 Å and from 6567.8 to 6570.6 Å with 0.024 Å pixel spectral resolution and 1 minute temporal resolution. The continuum imaging mode obtains photospheric images in continuum around 6689 Å with the full width at half maximum of 13.4 Å. The CHASE mission will advance our understanding of the dynamics of solar activity in the photosphere and chromosphere. In this paper, we present an overview of the CHASE mission including the scientific objectives, HIS instrument overview, data calibration flow, and first results of on-orbit observations.

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“…之后, Aschwanden 在 2014 年对该模型做了进一步的推广 [31] . [53] 和 ASO-S [54] )和地基望远镜(口径 2.5 米 [55] 和 1.8 米 [56] ) 也会陆续投入使用. 这使得我们可以对全日面或者某一个活动区进行多波段、高时空分辨率的观测, 因而可用于进行太阳爆发研究的观测数据异常丰富.…”

Section: 引言unclassified