Solar Physics最新文献_第5页

Inflight Performance and Calibrations of the Lyman-Alpha Solar Telescope on Board the Advanced Space-Based Solar Observatory 先进天基太阳观测站搭载的莱曼-阿尔法太阳望远镜的飞行性能和校准

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-29 DOI: 10.1007/s11207-024-02354-3

Bo Chen, Li Feng, Guang Zhang, Hui Li, Lingping He, Kefei Song, Quanfeng Guo, Ying Li, Yu Huang, Jingwei Li, Jie Zhao, Jianchao Xue, Gen Li, Guanglu Shi, Dechao Song, Lei Lu, Beili Ying, Haifeng Wang, Shuang Dai, Xiaodong Wang, Shilei Mao, Peng Wang, Kun Wu, Shuai Ren, Liang Sun, Xianwei Yang, Mingyi Xia, Xiaoxue Zhang, Peng Zhou, Chen Tao, Yang Liu, Sibo Yu, Xinkai Li, Shuting Li, Ping Zhang, Qiao Li, Zhengyuan Tian, Yue Zhou, Jun Tian, Jiahui Shan, Xiaofeng Liu, Zhichen Jing, Weiqun Gan

{"title":"Inflight Performance and Calibrations of the Lyman-Alpha Solar Telescope on Board the Advanced Space-Based Solar Observatory","authors":"Bo Chen, Li Feng, Guang Zhang, Hui Li, Lingping He, Kefei Song, Quanfeng Guo, Ying Li, Yu Huang, Jingwei Li, Jie Zhao, Jianchao Xue, Gen Li, Guanglu Shi, Dechao Song, Lei Lu, Beili Ying, Haifeng Wang, Shuang Dai, Xiaodong Wang, Shilei Mao, Peng Wang, Kun Wu, Shuai Ren, Liang Sun, Xianwei Yang, Mingyi Xia, Xiaoxue Zhang, Peng Zhou, Chen Tao, Yang Liu, Sibo Yu, Xinkai Li, Shuting Li, Ping Zhang, Qiao Li, Zhengyuan Tian, Yue Zhou, Jun Tian, Jiahui Shan, Xiaofeng Liu, Zhichen Jing, Weiqun Gan","doi":"10.1007/s11207-024-02354-3","DOIUrl":"10.1007/s11207-024-02354-3","url":null,"abstract":"<div><p>The Ly<span>(alpha )</span> Solar Telescope (LST) is the first instrument to achieve imaging of the full solar disk and the coronal region in both white light (WL) and ultraviolet (UV) H <span>i</span> Ly<span>(alpha )</span>, extending up to 2.5 solar radii (Rs), contributing to solar physics research and space weather forecasting. Since its launch on 9 October 2022, LST has captured various significant solar activity phenomena, including flares, filaments, prominences, and coronal mass ejections (CMEs). On-orbit observation and test results show that LST covers a continuous spatial range and the wavelengths of 121.6, 360, and 700 nm. The Ly<span>(alpha )</span> Solar Disk Imager (SDI) has a field of view (FOV) of 38.4′ and a spatial resolution of around 9.5″, while the White-Light Solar Telescope (WST) has an FOV of 38.43′ and a spatial resolution of around 3.0″. The FOV of the Ly<span>(alpha )</span> Solar Corona Imager (SCI) reaches 81.1′ and its spatial resolution is 4.3″. The stray-light level in the 700 nm waveband is about 7.8 × 10<sup>−6</sup> MSB at 1.1 Rs and 7.6 × 10<sup>−7</sup> MSB at 2.5 Rs, and in Ly<span>(alpha )</span> waveband it is around 4.3 × 10<sup>−3</sup> MSB at 1.1 Rs and 4.1 × 10<sup>−4</sup> MSB at 2.5 Rs (MSB: mean solar brightness). This article will detail the results from on-orbit tests and calibrations.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219168","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Flux Calibration of Coronal Magnetic Field 日冕磁场的磁通量校准

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-29 DOI: 10.1007/s11207-024-02364-1

Marek Vandas, Evgeny Romashets

引用次数: 0

Hemispheric Sunspot Number Prediction for Solar Cycles 25 and 26 Using Spectral Analysis and Machine Learning Techniques 利用光谱分析和机器学习技术预测太阳周期 25 和 26 的半球太阳黑子数

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-28 DOI: 10.1007/s11207-024-02363-2

José-Víctor Rodríguez, Víctor Manuel Sánchez Carrasco, Ignacio Rodríguez-Rodríguez, Alejandro Jesús Pérez Aparicio, José Manuel Vaquero

{"title":"Hemispheric Sunspot Number Prediction for Solar Cycles 25 and 26 Using Spectral Analysis and Machine Learning Techniques","authors":"José-Víctor Rodríguez, Víctor Manuel Sánchez Carrasco, Ignacio Rodríguez-Rodríguez, Alejandro Jesús Pérez Aparicio, José Manuel Vaquero","doi":"10.1007/s11207-024-02363-2","DOIUrl":"10.1007/s11207-024-02363-2","url":null,"abstract":"<div><p>The present study uses machine learning and time series spectral analysis to develop a novel technique to forecast the sunspot number (S<sub>N</sub>) in both hemispheres for the remainder of Solar Cycle 25 and Solar Cycle 26. This enables us to offer predictions for hemispheric S<sub>N</sub> until January 2038 (using the 13-month running average). For the Northern hemisphere, we find maximum peak values for Solar Cycles 25 and 26 of 58.5 in April 2023 and 51.5 in November 2033, respectively (root mean square error of 6.1). For the Southern hemisphere, the predicted maximum peak values for Solar Cycles 25 and 26 are 77.0 in September 2024 and 70.1 in November 2034, respectively (root mean square error of 6.8). In this sense, the results presented here predict a Southern hemisphere prevalence over the Northern hemisphere, in terms of S<sub>N</sub>, for Solar Cycles 25 and 26, thus continuing a trend that began around 1980, after the last period of Northern hemisphere prevalence (which, in turn, started around 1900). On the other hand, for both hemispheres, our findings predict lower maxima for Solar Cycles 25 and 26 than the preceding cycles. This fact implies that, when predicting the total S<sub>N</sub> as the sum of the two hemispheric forecasts, Solar Cycles 24 – 26 may be part of a centennial Gleissberg cycle’s minimum, as was the case in the final years of the 19th century and the start of the 20th century (Solar Cycles 12, 13, and 14).</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02363-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219150","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Predicting Solar Cycle 26 Using the Polar Flux as a Precursor, Spectral Analysis, and Machine Learning: Crossing a Gleissberg Minimum? 利用极地通量作为前兆、光谱分析和机器学习预测太阳周期 26：跨越格莱斯伯格极小期？

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-28 DOI: 10.1007/s11207-024-02361-4

José-Víctor Rodríguez, Víctor Manuel Sánchez Carrasco, Ignacio Rodríguez-Rodríguez, Alejandro Jesús Pérez Aparicio, José Manuel Vaquero

{"title":"Predicting Solar Cycle 26 Using the Polar Flux as a Precursor, Spectral Analysis, and Machine Learning: Crossing a Gleissberg Minimum?","authors":"José-Víctor Rodríguez, Víctor Manuel Sánchez Carrasco, Ignacio Rodríguez-Rodríguez, Alejandro Jesús Pérez Aparicio, José Manuel Vaquero","doi":"10.1007/s11207-024-02361-4","DOIUrl":"10.1007/s11207-024-02361-4","url":null,"abstract":"<div><p>This study introduces a novel method for predicting the sunspot number (<span>(mathrm{S}_{mathrm{N}})</span>) of Solar Cycles 25 (the current cycle) and 26 using multivariate machine-learning techniques, the Sun’s polar flux as a precursor parameter, and the fast Fourier transform to conduct a spectral analysis of the considered time series. Using the 13-month running average of the version 2 of the <span>(mathrm{S}_{mathrm{N}})</span> provided by the World Data Center—SILSO, we are thus able to present predictive results for the <span>(mathrm{S}_{mathrm{N}})</span> until January 2038, giving maximum peak values of 131.4 (in July 2024) and 121.2 (in September 2034) for Solar Cycles 25 and 26, respectively, with a root mean square error of 10.0. These predicted dates are similar to those estimated for the next two polar flux polarity reversals (April 2024 and August 2034). Furthermore, the values for the <span>(mathrm{S}_{mathrm{N}})</span> maxima of Solar Cycles 25 and 26 have also been forecasted based on the known correlation between the absolute value of the difference between the polar fluxes of both hemispheres at an <span>(mathrm{S}_{mathrm{N}})</span> minimum and the maximum <span>(mathrm{S}_{mathrm{N}})</span> of the subsequent cycle, obtaining similar values to those achieved with the previous method: 142.3 ± 34.2 and 126.9 ± 34.2 for Cycles 25 and 26, respectively. Our results suggest that Cycle 25 will have a maximum amplitude that lies below the average and Cycle 26 will reach an even lower peak. This suggests that Solar Cycles 24 (with a peak of 116.4), 25, and 26 would belong to a minimum of the centennial Gleissberg cycle, as was the case in the final years of the 19th and the early 20th centuries (Solar Cycles 12, 13, and 14).</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02361-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219167","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Hysteresis Near the Transition of the Large-Scale Dynamo in the Presence of the Small-Scale Dynamo 存在小尺度动力机制时大尺度动力机制过渡附近的滞后现象

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-23 DOI: 10.1007/s11207-024-02360-5

Vindya Vashishth

{"title":"Hysteresis Near the Transition of the Large-Scale Dynamo in the Presence of the Small-Scale Dynamo","authors":"Vindya Vashishth","doi":"10.1007/s11207-024-02360-5","DOIUrl":"10.1007/s11207-024-02360-5","url":null,"abstract":"<div><p>In the Sun and solar-type stars, there is a critical dynamo number for the operation of a large-scale dynamo, below which the dynamo ceases to operate. This region is known as the subcritical region. Previous studies showed the possibility of operating the solar-like large-scale (global) dynamo in the subcritical region without a small-scale dynamo. As in the solar convection zone, both large- and small-scale dynamos are expected to operate at the same time and location, we check the robustness of the previously identified subcritical dynamo branch in a numerical model in which both large- and small-scale dynamos are excited. For this, we use the <span>Pencil Code</span> and set up an <span>(alpha Omega )</span> dynamo model with uniform shear and helically forced turbulence. We have performed a few sets of simulations at different relative helicity to explore the generation of large-scale oscillatory fields in the presence of small-scale dynamo. We find that in some parameter regimes, the dynamo shows hysteresis behavior, i.e., two dynamo solutions are possible depending on the initial parameters used. A decaying solution when the dynamo was started with a weak field and a strong oscillatory solution if the dynamo was initialized with a strong field. Thus, the existence of the sub-critical branch of the large-scale dynamo in the presence of small-scale dynamo is established. However, the regime of hysteresis is quite narrow with respect to the case without the small-scale dynamo. Our work supports the possible existence of large-scale dynamo in the sub-critical regime of slowly rotating stars.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219169","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Periods and Frequency Drifts of Groups of the Decimetric Spikes in Two Solar Flares 两个太阳耀斑中各组十进制尖峰的周期和频率漂移

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-21 DOI: 10.1007/s11207-024-02359-y

Marian Karlický, Jaroslav Dudík, Ján Rybák

{"title":"Periods and Frequency Drifts of Groups of the Decimetric Spikes in Two Solar Flares","authors":"Marian Karlický, Jaroslav Dudík, Ján Rybák","doi":"10.1007/s11207-024-02359-y","DOIUrl":"10.1007/s11207-024-02359-y","url":null,"abstract":"<div><p>We studied the radio emission occurring as narrowband decimetric spikes observed during the 10 May 2022 and 26 August 2022 flares. In the radio spectra, these spikes were distributed in groups that occurred quasi-periodically with the periods 5.1 s in the 10 May 2022 flare and 9.1 s in the 26 August 2022 flare. In some parts of these groups, even subgroups of spikes distributed with the quasi-periods of 0.19 s (10 May 2022 flare), and 0.17 s and 0.21 s (26 August 2022 flare) were found. Some of these subgroups even drifted to higher or lower frequencies, which was observed for the first time. At the time of the dm-spikes observation, a pair of reconnecting loops are identified in the SDO/AIA EUV observations of the 10 May 2022 flare, one of which is interpreted as belonging to a small erupting filament. We propose that these loops reconnect in the dynamic quasi-periodic regime (the period 0.19 s) and this reconnection is modulated by an oscillation of one of the interacting loops (the period 5.1 s). Accelerated electrons from this process are trapped in reconnecting plasma outflows, and thus the drifting groups of spikes are generated. The 26 August 2022 flare is a complex event with several systems of bright loops; nevertheless, it also shows a disintegrating erupting filament similar to the 10 May 2022 flare, meaning that the dm-spikes are likely generated by similar reconnection processes.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02359-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219171","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Triangulation of Hard X-Ray Sources in an X-Class Solar Flare with ASO-S/HXI and Solar Orbiter/STIX 利用 ASO-S/HXI 和 Solar Orbiter/STIX 对 X 级太阳耀斑中的硬 X 射线源进行三角测量。

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-21 DOI: 10.1007/s11207-024-02341-8

Daniel F. Ryan, Paolo Massa, Andrea F. Battaglia, Ewan C. M. Dickson, Yang Su, Wei Chen, Säm Krucker

{"title":"Triangulation of Hard X-Ray Sources in an X-Class Solar Flare with ASO-S/HXI and Solar Orbiter/STIX","authors":"Daniel F. Ryan, Paolo Massa, Andrea F. Battaglia, Ewan C. M. Dickson, Yang Su, Wei Chen, Säm Krucker","doi":"10.1007/s11207-024-02341-8","DOIUrl":"10.1007/s11207-024-02341-8","url":null,"abstract":"<div><p>HXI on ASO-S and STIX onboard Solar Orbiter are the first simultaneously operating solar hard X-ray imaging spectrometers. ASO-S’s low Earth orbit and Solar Orbiter’s periodic displacement from the Sun–Earth line enables multi-viewpoint solar hard X-ray spectroscopic imaging analysis for the first time. Here, we demonstrate the potential of this new capability by reporting the first results of 3D triangulation of hard X-ray sources in the SOL2023-12-31T21:55 X5 flare. HXI and STIX observed the flare near the east limb with an observer separation angle of 18°. We triangulated the brightest regions within each source, which enabled us to characterise the large-scale hard X-ray geometry of the flare. The footpoints were found to be in the chromosphere within uncertainty, as expected, while the thermal looptop source was centred at an altitude of 15.1 ± 1 Mm. Given the footpoint separation, this implies a more elongated magnetic-loop structure than predicted by a semi-circular model. These results show the strong diagnostic power of joint HXI and STIX observations for understanding the 3D geometry of solar flares. We conclude by discussing the next steps required to fully exploit their potential.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC11339132/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142054621","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Fabry-Pérot Interferometer Based Imaging Spectrometer for Fe I Line Observation and Line-of-Sight Velocity Measurement 基于法布里-佩罗干涉仪的成像光谱仪，用于铁 I 线观测和视线速度测量

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-21 DOI: 10.1007/s11207-024-02353-4

Xingcheng Hu, Jinsheng Yang, Xuejun Rao, Dingkang Tong, Jiawen Yao, Zhimao Du, Qing Lin, Changhui Rao

{"title":"Fabry-Pérot Interferometer Based Imaging Spectrometer for Fe I Line Observation and Line-of-Sight Velocity Measurement","authors":"Xingcheng Hu, Jinsheng Yang, Xuejun Rao, Dingkang Tong, Jiawen Yao, Zhimao Du, Qing Lin, Changhui Rao","doi":"10.1007/s11207-024-02353-4","DOIUrl":"10.1007/s11207-024-02353-4","url":null,"abstract":"<div><p>High spectral resolution imaging spectroscopy plays a crucial role in solar observation, regularly serving as a backend instrument for solar telescopes. These instruments find direct application in deriving Doppler velocity from hyperspectral images, offering insights into the dynamic motion of matter on the solar surface. In this study, we present the development of a Fabry–Pérot interferometer (FPI) based imaging spectrometer operating at the Fe I (617.3 nm) wavelength for precise Doppler velocity measurements. The spectrometer features a moderate spectral resolution of <span>(lambda/Deltalambdaapprox60{,}000)</span>, aiming to balance the imaging signal-to-noise ratio (SNR). The instrument underwent successful observational experiments on the 65-cm Educational Adaptive-Optics Solar Telescope (EAST) at the Shanghai Astronomy Museum. Obtained Doppler velocities were compared with data from the Helioseismic and Magnetic Imager (HMI), the maximum column and row correlation coefficients are 0.9261 and 0.9603, respectively. The estimated cut-off normalized frequency of the power spectral density (PSD) curve for velocity map is approximately 0.4/0.21 times higher than that observed in the HMI data, with potentially higher spatial resolution achievable under better seeing conditions. Based on the estimated imaging SNR levels, the accuracy of velocity measurements is approximately 50 m s<sup>−1</sup>.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219170","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Solar Poloidal Magnetic Field Generation Rate from Observations and Mean-Field Dynamos 从观测和平均场动力学角度看太阳极面磁场生成率

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-20 DOI: 10.1007/s11207-024-02357-0

Valery Pipin

引用次数: 0

Optimization of Solar-Wind Speed Models Using Interplanetary Scintillation Observations 利用行星际闪烁观测优化太阳风速模型

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2024-08-19 DOI: 10.1007/s11207-024-02356-1

Munetoshi Tokumaru, Ken’ichi Fujiki, Haruto Watanabe

{"title":"Optimization of Solar-Wind Speed Models Using Interplanetary Scintillation Observations","authors":"Munetoshi Tokumaru, Ken’ichi Fujiki, Haruto Watanabe","doi":"10.1007/s11207-024-02356-1","DOIUrl":"10.1007/s11207-024-02356-1","url":null,"abstract":"<div><p>Improvement of the model providing the boundary condition of the solar-wind speed near the Sun is essential for gaining a better forecast of space weather. We optimized the parameters of the distance from the coronal hole boundary (DCHB) model and the Wang–Sheeley (WS) model, which enabled the determination of solar-wind speed from observations of the Sun’s magnetic field. In this study, we used solar-wind speed data derived from interplanetary scintillation (IPS) observations at the Institute for Space-Earth Environmental Research (ISEE) for six Carrington rotations in Solar Cycle 23 as reference data. A comparison of IPS observations and optimized DCHB models demonstrated strong-to-moderate positive correlations and small deviations, except for solar maximum data. The degraded correlation at the solar maximum is ascribed to the effect of the rapid structural evolution of the solar wind and coronal magnetic field. The performance of the optimized DCHB model was better than that of the optimized WS model. To solve a limitation of the DCHB model in reproducing slow-wind speeds, we propose a modified version of the DCHB model and optimize it for IPS observations. The optimized solutions for the modified DCHB model demonstrate performance comparable to that of the original model. The results obtained in this study suggest that the DCHB acts better as a controlling parameter for the solar-wind speed than the expansion factor and that both the optimized DCHB model and its modified version are useful for improving the estimation of the solar-wind speed at the source surface from magnetograph observations.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 8","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-08-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142219173","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0