Solar Physics最新文献

Desynchronization Events in Solar Indices as a Manifestation of the North-South Asymmetry

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-20 DOI: 10.1007/s11207-024-02419-3

Elena Blanter, Mikhail Shnirman

{"title":"Desynchronization Events in Solar Indices as a Manifestation of the North-South Asymmetry","authors":"Elena Blanter, Mikhail Shnirman","doi":"10.1007/s11207-024-02419-3","DOIUrl":"10.1007/s11207-024-02419-3","url":null,"abstract":"<div><p>We suggest the Kuramoto chain model with four coupled oscillators as a way to describe the phase evolution and departures from synchronization of solar indices at low and high latitudes in the northern and southern hemispheres. Our model simulates the basic properties of the phase differences between the near-equatorial sunspot areas and the polar facula series provided by the Pulkovo and Mount Wilson (MWO) observatories. Temporal variations of the meridional circulation are represented through slow, regular oscillations of natural frequencies. We consider the Gleissberg range (GR) oscillations to have the North-South asymmetry and the 22-year oscillation to be symmetric. The overall synchronization of polar and equatorial solar indices is confirmed. We use it to reconstruct model parameters from the phase difference of solar indices. The synchronization allows for reducing the space of model parameters to a 2D plane, where the eventual departures from the synchronization cut out a narrow zone of accurate estimates. We discuss revealed relations between the low-frequency variations of the solar meridional circulation, the North-South asymmetry, and the desynchronization events.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143455678","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

Data-Constrained Magnetohydrodynamics Simulation of a Confined X-Class Flare in NOAA Active Region 11166

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-13 DOI: 10.1007/s11207-025-02426-y

Sanjay Kumar, Pawan Kumar, Sadashiv, Sushree S. Nayak, Satyam Agarwal, Avijeet Prasad, Ramit Bhattacharyya, Ramesh Chandra

{"title":"Data-Constrained Magnetohydrodynamics Simulation of a Confined X-Class Flare in NOAA Active Region 11166","authors":"Sanjay Kumar, Pawan Kumar,  Sadashiv, Sushree S. Nayak, Satyam Agarwal, Avijeet Prasad, Ramit Bhattacharyya, Ramesh Chandra","doi":"10.1007/s11207-025-02426-y","DOIUrl":"10.1007/s11207-025-02426-y","url":null,"abstract":"<div><p>In this paper, we present a magnetohydrodynamics simulation of NOAA active region 11166 to understand the origin of a confined X-class flare that peaked at 23:23 UT on 2011 March 9. The simulation is initiated with a magnetic field extrapolated from the corresponding photospheric magnetogram, using a non-force-free-field extrapolation technique. Importantly, the initial magnetic configuration identifies three-dimensional (3D) magnetic nulls and quasi-separatrix layers (QSLs), which nearly agree with the bright structures appeared in multi-wavelength observations. The Lorentz force associated with the extrapolated field self-consistently generates the dynamics that leads to the magnetic reconnections at the 3D nulls and the QSLs. These reconnections are found to contribute to the pre-flare activities and, ultimately, lead to the development of the flare ribbons. Notably, the anchored spine of the 3D null and the complete absence of flux rope in the flaring region are congruent with the confined nature of the flare. Furthermore, the simulation also suggests the role of reconnections at the 3D null with an open spine in the onset of a jet away from the flaring site.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143404237","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

Periodic Variation of Anomalous Cosmic Ray Oxygen During Solar Cycles 23 and 24

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-13 DOI: 10.1007/s11207-024-02420-w

Pieter Kotzé, Kalevi Mursula

{"title":"Periodic Variation of Anomalous Cosmic Ray Oxygen During Solar Cycles 23 and 24","authors":"Pieter Kotzé, Kalevi Mursula","doi":"10.1007/s11207-024-02420-w","DOIUrl":"10.1007/s11207-024-02420-w","url":null,"abstract":"<div><p>We investigate the evolution of the Rieger periodicity at 152 – 156 days, the 27-day synodic rotation period as well as the 13.5- and 9-day harmonic periodicities in anomalous cosmic ray (ACR) oxygen (O) fluxes at the energy range between 8 – 25 MeV/n observed by the <i>Advanced Composition Explorer</i> (ACE) satellite during Solar Cycles 23 and 24. The ACR oxygen flux data is analysed using the Lomb–Scargle periodogram and Morlet wavelet spectral analysis techniques. Daily mean oxygen fluxes during solar quiet times are used to identify how the ACR oxygen at different energies varies with the Rieger periodicity and the solar rotation periodicities in each year. This is the first investigation of the periodicity evolution of ACR oxygen ions. Previous investigations have mostly concentrated on the spectral behaviour of GCR particles during various solar cycles of opposite polarities, in particular the 27-day and 13.5-day periodicities. Our analysis revealed a significant temporal and energy dependence in the spectral behaviour of ACR oxygen during both cycles. An important finding of this investigation, not reported before in the literature, is the significant increase in the power of the different ACR oxygen periodicities during the minimum of Cycle 24/25 (characterised by a positive solar polarity) in comparison to the minimum of Cycle 23/34 (dominated by a negative solar polarity).</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02420-w.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143404241","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

Analyses of Features of Magnetic Cycles at Different Amounts of Dynamo Supercriticality: Solar Dynamo Is About Two Times Critical

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-13 DOI: 10.1007/s11207-025-02428-w

Sanket Wavhal, Pawan Kumar, Bidya Binay Karak

引用次数: 0

Effect of Solar Parameters on Geomagnetic Storm Formation in the Ascending Phase of the 25th Solar Cycle

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-13 DOI: 10.1007/s11207-025-02427-x

Zehra Can, Hasan Şafak Erdağ

{"title":"Effect of Solar Parameters on Geomagnetic Storm Formation in the Ascending Phase of the 25th Solar Cycle","authors":"Zehra Can, Hasan Şafak Erdağ","doi":"10.1007/s11207-025-02427-x","DOIUrl":"10.1007/s11207-025-02427-x","url":null,"abstract":"<div><p>In this paper, starting from solar storms, which are the main cause of geomagnetic storms, the effects of the speed (v) and density (Np) of solar plasma coming to the Earth on geomagnetic storms are investigated. During the ascending phase of the 25th solar cycle (2021 – 2022), various geomagnetic storms from G1 to G4 were examined. Multiple linear regression models are created to examine the effects of solar parameters that cause changes in geomagnetic storm processes. The effects of the speed and charge density of solar wind, coronal mass ejections (CMEs), corotating interaction regions (CIRs), and CME-CME interactions on the Dst index, which reflects disturbances in the Earth’s magnetic field and the scale of geomagnetic storms, are statistically analyzed. It is determined that a one-unit change in speed in 82 geomagnetic storms in the statistical models created a decrease in Dst of approximately −0.25 nT. In contrast, it is determined that a unit increase in particle density also reduces the effect and duration of a geomagnetic storm. However, if there is an increase in density during the main phase of the storm, then the storm level increases. We believe that our results will significantly contribute to predicting the formation of geomagnetic storms and their possible effects on space weather.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02427-x.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143404239","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

On a Possible Scenario of Solar Coherent Bursts

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-13 DOI: 10.1007/s11207-025-02433-z

S. V. Lesovoi, Dale E. Gary, M. V. Globa, E. F. Ivanov

{"title":"On a Possible Scenario of Solar Coherent Bursts","authors":"S. V. Lesovoi, Dale E. Gary, M. V. Globa, E. F. Ivanov","doi":"10.1007/s11207-025-02433-z","DOIUrl":"10.1007/s11207-025-02433-z","url":null,"abstract":"<div><p>The first burst of solar microwave coherent emission observed simultaneously with two multifrequency two-dimensional radio telescopes is reported, making it possible to unambiguously interpret the mechanism of the radiation and to propose a scenario that explains all the observed features of the burst. Recently, many studies have appeared that explain coherent bursts of radio emission from the Earth’s magnetosphere and solar corona by an electron cyclotron maser (ECM) driven by horseshoe distribution. The result of this study is that the observed coherent burst near the frequency 4.8 GHz is caused by a hollow beam distribution formed by the oblique injection of electrons into a magnetic loop. If the pitch-angle is large enough, then the absence of HXR and the relatively large (about 1 s) pulse duration can be explained. The measured size of the ECM source, <span>(approx 2.2^{prime prime })</span>, corresponds to a brightness temperature of <span>(approx 5.8times 10^{10}text{ K})</span>. The displacement of the spike sources with respect to the gyroresonance source is consistent to the second-harmonic ECM emission, whereas the gyroresonance source is consistent to the third gyrolayer.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143404240","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

Travel Time Estimation from Numerical Simulations of f-Mode Propagation Through Sunspot Models and Plages

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-12 DOI: 10.1007/s11207-025-02436-w

Khalil Daiffallah, Omar Boumia

引用次数: 0

The SOLARNET Virtual Observatory: An Effective Way to Search Solar Datasets and Cross-Search with Solar Events

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-11 DOI: 10.1007/s11207-025-02424-0

Benjamin Mampaey, Véronique Delouille, Robbe Vansintjan

{"title":"The SOLARNET Virtual Observatory: An Effective Way to Search Solar Datasets and Cross-Search with Solar Events","authors":"Benjamin Mampaey, Véronique Delouille, Robbe Vansintjan","doi":"10.1007/s11207-025-02424-0","DOIUrl":"10.1007/s11207-025-02424-0","url":null,"abstract":"<div><p>The volume and diversity of solar physics data have grown exponentially in the last three decades. In view of making solar datasets easily accessible to the scientific community, we have developed the SOLARNET Virtual Observatory (SVO), an IT service that collects metadata from a large range of solar observational datasets in a common catalog to allow smooth data search and access. It follows the virtual observatories (VO) principle, with a provider layer, core metadata database, and user layer. The user layer contains a user-friendly web application, Python and IDL libraries, and a RESTful API. The SVO enables metadata to be searched either across all datasets or within a specific dataset by applying more precise search conditions. Additionally, it allows researchers to query solar events from the HEK database and identify data that overlaps with these events. Data can be previewed and downloaded from the web application. The Python and IDL libraries allow the integration of the SVO data search and functionality with complex data processing pipelines. On the provider side, datasets are ingested through tailored scripts. Recently, a TAP client layer has been added to the SVO, hence, it is possible to populate the SVO automatically with a dataset that is available as a TAP or EPN-TAP service. We describe the service, user, and provider side of the SVO and illustrate its capabilities with four scientific use cases.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02424-0.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143388709","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

Long-Lived Sunspots in Historical Records: A Case Study Analysis from 1660 to 1676

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-11 DOI: 10.1007/s11207-025-02432-0

Nadezhda Zolotova, Mikhail Vokhmyanin

引用次数: 0

A Method of Extracting Flat Field from Real Time Solar Observation Data

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-02-10 DOI: 10.1007/s11207-025-02435-x

YaHui Jin, Hui Liu, KaiFan Ji, ZhenYu Jin, WeiJie Meng

{"title":"A Method of Extracting Flat Field from Real Time Solar Observation Data","authors":"YaHui Jin, Hui Liu, KaiFan Ji, ZhenYu Jin, WeiJie Meng","doi":"10.1007/s11207-025-02435-x","DOIUrl":"10.1007/s11207-025-02435-x","url":null,"abstract":"<div><p>Existing methods for obtaining a flat field rely on observed data collected under specific observation conditions to determine the flat field. However, the telescope pointing and the column-fixed pattern noise of the CMOS detector change during actual observations. This leads to the residual signals in real-time observation data after flat field correction, such as interference fringes and column-fixed pattern noise. In actual observations the wind causes the telescope to wobble slightly, which leads to shifts in the observed data. In this paper, we propose a method of extracting the flat field from the real-time solar observation data. Firstly, the average flat field obtained by multiframe averaging is used as the initial value. A set of real-time observation data is input into the KLL method to calculate the correction amount for the average flat field. Secondly, the average flat field is corrected using the calculated correction amount to obtain the real flat field for the current observation conditions. To overcome the residual solar structures caused by atmospheric turbulence in the correction amount, real-time observation data are grouped to calculate the correction amounts. These residual solar structures are suppressed by averaging multiple groups, improving the accuracy of the correction amount. The test results from diffraction-limited and ground-based simulated data demonstrate that our method can effectively calculate the correction amount for the average flat field. The New Vacuum Solar Telescope (NVST) He I 10830 Å/H<span>(alpha )</span> data were also tested. High-resolution reconstruction confirms that the correction amount effectively corrects the average flat field to obtain the real flat field for the current observation conditions. Our method works for chromosphere and photosphere data.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143373216","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