Solar Physics最新文献

{"title":"The Solar FUV-UV Spectra Measurement Experiment in the Near Space by High Altitude Balloon","authors":"Fei Wei,&nbsp;Xuanyi Zhang","doi":"10.1007/s11207-024-02396-7","DOIUrl":"10.1007/s11207-024-02396-7","url":null,"abstract":"<div><p>An experiment measuring the solar far-ultraviolet-ultraviolet (FUV-UV) irradiance with spectral resolution better than 0.1 nm in the wavelength range from 170 to 400 nm was carried out by the “HongHu-6” high-altitude balloon that flew to the bottom region of the near-space in September 2022. This experiment was based on the fact that solar FUV-UV penetrates through a complex cross-section window of the upper atmosphere, from outer to near space. The solar FUV-UV deposits energy in the upper atmosphere, which provides a key to answer scientific questions on the most important energy contributor to overall heating sources of the near space and how the near-space environment responds to solar activities. In the wavelength range between 150 and 210 nm, irradiance maps from active regions of the solar corona, the comparative small cross-section of molecular oxygen allows certain wavelengths of the band to arrive at altitudes between 20 and 30 km above the ground, indicating solar flares could directly impact the bottom region of the near space. Solar UV irradiance in the wavelength range 210 – 400 nm is absorbed by the upper atmosphere as a function of wavelength, and energy is deposited vertically in the lower regions of the near space. This experiment historically provides measurement data to fill a gap in the wavelength shorter than 280 nm in the lower regions of the near space. The solar FUV-UV spectrometer (SUVS) is a compact instrument based on improved Roland circle optics to adapt to the “HongHu-6” balloon payload platform. In this paper, we introduce the scientific goals of the solar FUV-UV spectrum measurement experiment, provide information on the SUVS instrument preflight calibration, and present the first results from the flight data.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02396-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142524378","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}

{"title":"Calibration and Release of Magnetograms/Dopplergrams Obtained at the Mt. Wilson 150-Foot Tower Telescope (MWO)","authors":"Roger K. Ulrich,&nbsp;John Boyden,&nbsp;Tham Tran","doi":"10.1007/s11207-024-02390-z","DOIUrl":"10.1007/s11207-024-02390-z","url":null,"abstract":"<div><p>The Mt. Wilson Observatory archive of observations of solar disk magnetic fields, Doppler velocities, and spectral line intensities is a resource for studying the Sun’s state from 1967 to 2013. Instrument changes/upgrades during this time must be considered when interpreting this record. Portions of this record have been previously released. This publication documents the data record in order to allow its independent interpretation. The archive is available through two directory trees which can be accessed at http://sha.stanford.edu/mwo/msm.html. The calibration of the observations is impacted by the solar surface convective flows, which produce offsets for both differential rotation and meridional circulation functions. The effects of these offsets have been reduced in this and other publications by temporal averaging.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02390-z.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142519028","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}

{"title":"Long-Term Trends in Subsurface Flows of Solar Cycle 23 to 25","authors":"Rudolf Komm","doi":"10.1007/s11207-024-02397-6","DOIUrl":"10.1007/s11207-024-02397-6","url":null,"abstract":"<div><p>We study the long-term variation of the zonal and meridional flows from Solar Cycle 23 to 25 derived with ring-diagram analysis applied to <i>Global Oscillation Network Group</i> (GONG) and <i>Helioseismic and Magnetic Imager</i> (HMI) Dopplergrams. We focus mainly on the subsurface flows averaged over depths from 2.0 Mm to 11.6 Mm since their long-term variations are sufficiently similar. First, we examine their temporal variations for systematic artifacts. We find that the GONG-derived zonal flows increase almost linearly with time until about 2020, which we correct with a linear regression. Then we determine the average differences between the GONG- and HMI-derived flows. The average offset is <span>(0.15 pm 0.53)</span> m s⁻¹ for the zonal flow and <span>(0.65 pm 0.08)</span> m s⁻¹ for the meridional flow within <span>(pm 30.0^{circ })</span> latitude. The average difference of the meridional flow is nearly constant with latitude in this range, whereas that of the zonal flow varies similarly to that of the magnetic activity. At latitudes of 45.0^∘ and higher, the differences increase and are larger than those at lower latitudes, which is most likely due to the combined effect of different spatial resolution between GONG and HMI and geometric projection effects. Finally, we combine the GONG- and HMI-derived flows and find, as expected, that the solar-cycle variation is the dominant long-term variation. At each latitude within <span>(pm 30.0^{circ })</span>, the meridional-flow pattern appears ahead of the zonal-flow pattern by an average lag of <span>(0.926 pm 0.126)</span> years. The equatorward and poleward branches of the solar-cycle variation occur at 52.5^∘ with the poleward branches present near 60.0^∘ and the equatorward ones at lower latitudes. The zonal flows at 52.5^∘ and 60.0^∘ show an additional trend and decrease by <span>(2.9 pm 0. 3)</span> m s⁻¹ over 11 years. This decrease might nevertheless be related to the solar cycle and imply that the flow amplitudes are anticorrelated with the strength of the associated solar cycle.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142519030","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}

{"title":"Multi-fractal Analysis of Cosmic Rays over Mid- and High-Latitude Stations During Severe Geomagnetic Storms","authors":"Ashutosh Giri,&nbsp;Binod Adhikari,&nbsp;Subodh Dahal,&nbsp;K. S. S. Paula,&nbsp;M. J. A. Bolzan","doi":"10.1007/s11207-024-02393-w","DOIUrl":"10.1007/s11207-024-02393-w","url":null,"abstract":"<div><p>This study explores the multi-fractal properties of cosmic-ray (CR) counts collected from two mid-latitude neutron-monitor stations, Newark (NEWK) and Irkutsk 3 (IRK3), and two high-latitude stations, Thule (THUL) and Inuvik (INVK), during periods of severe geomagnetic storms. By employing multi-fractal along with time-series analysis, we did an in-depth examination of CR count variations to demonstrate the effectiveness of these methods in analyzing complex signals associated with astrophysical and solar phenomena. The findings reveal that CR count rates across stations at different latitudes exhibit multi-fractal characteristics, reflecting a range of scaling exponents that capture varying degrees of correlation and variability within the system. The results underscore that solar activity, geomagnetic events, and interactions with Earth’s magnetic field play a more crucial role in determining multi-fractality than the geographic location of the measurement station. Moreover, the study shows that geomagnetic events exert a stronger influence on the multi-fractal properties of CR count rate than the geographic location of station, underscoring the impact of solar storms and Earth’s magnetic field on the distribution and intensity of CRs. This work emphasizes the value of multi-fractal analysis as a powerful tool for investigating the complex nature of CR counts and its sensitivity to both extraterrestrial and terrestrial factors.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518400","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}

{"title":"Enhancing Solar Cycle 25 and 26 Forecasting with Vipin-Deep-Decomposed-Recomposed Rolling-window (vD2R2w) Model on Sunspot Number Observations","authors":"Vipin Kumar","doi":"10.1007/s11207-024-02389-6","DOIUrl":"10.1007/s11207-024-02389-6","url":null,"abstract":"<div><p>Effective predicting sunspot numbers (SSN) is the complex task of studying space weather, solar activity, satellite communication, and Earth’s climate. Developing a reliable SSN forecasting model is difficult because SSN time series exhibit complex patterns, nonlinearity, and nonstationarity characteristics. The state-of-the-art shows that deep-learning models often need help capturing SSN data’s intricate dynamics and long-term dependencies. The SSN time series’ decomposed trend and seasonal and residual characteristics may provide better information on long-term dependencies and associated dynamics for effective learning. In this research, the vipin-deep-decomposed-recomposed rolling-window (vD2R2w) models have been proposed with a combination of time-series decomposition, deep-learning models, and a rolling-window method to predict the SSN accurately. The proposed vD2R2w models have been evaluated over four datasets and consistently outperform traditional deep-learning models. The model improves the performance in terms of RMSE, MAPE, and <span>(R^{2})</span> over the datasets as SSN_Daily: 84.18% (RMSE), 10.38% (MAPE), and 3.504% (<span>(R^{2})</span>); SSN_Monthly: 39.5% (RMSE), 26.06% (MAPE), and 7.258% (<span>(R^{2})</span>); SSN_MonthlyMean: 178.32% (RMSE), 54.83% (MAPE), and 1.56% (<span>(R^{2})</span>); and SSN_Yearly: 6.06% (RMSE), 10.36% (MAPE), and 1.366% (<span>(R^{2})</span>). Further, the superiority of the vD2R2w models is validated through AIC &amp; BIC, Diebold Mariano test, and Friedman ranking statistical tests. Additionally, the vD2R2w model has forecasted the peak value of Solar Cycles (SC) and time, i.e., SC25: 127.16 (± 6.83) in 2025 and SC26: 191.71 (± 43.37) in 2035. The analysis of proposed model performances and statistical validation over various measures with four SSNs have concluded that the vD2R2w model outperforms the traditional models and is a reliable framework for SSN time series forecasting. Implementing the proposed model may benefit domains such as space-weather monitoring, satellite communication planning, and solar energy forecasting that rely on accurate SSN predictions.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518401","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}

{"title":"Observation of an Extraordinary Type V Solar Radio Burst: Nonlinear Evolution of the Electron Two-Stream Instability","authors":"Arnold O. Benz,&nbsp;Clemens R. Huber,&nbsp;Vincenzo Timmel,&nbsp;Christian Monstein","doi":"10.1007/s11207-024-02395-8","DOIUrl":"10.1007/s11207-024-02395-8","url":null,"abstract":"<div><p>Solar type V radio bursts are associated with type III bursts. Several processes have been proposed to interpret the association, electron distribution, and emission. We present the observation of a unique type V event observed by e-CALLISTO on 7 May 2021. The type V radio emission follows a group of U bursts. Unlike the unpolarized U bursts, the type V burst is circularly polarized, leaving room for a different emission process. Its starting edge drifts to higher frequency four times slower than the descending branch of the associated U burst. The type V processes seem to be ruled by electrons of lower energy. The observations conform to a coherent scenario where a dense electron beam drives the two-stream instability (causing type III emission) and, in the nonlinear stage, becomes unstable to another instability, previously known as the electron firehose instability (EFI). The secondary instability scatters some beam electrons into velocities perpendicular to the magnetic field and produces, after particle loss, a trapped distribution prone to electron cyclotron masering (ECM). A reduction in beaming and the formation of an isotropic halo are predicted for electron beams continuing to interplanetary space, possibly observable by Parker Solar Probe and Solar Orbiter.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02395-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142453060","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}

{"title":"Impact of Magnetic and Flow Fields on Penumbrae and Light Bridges of Three Leading Sunspots in an Active Region","authors":"R. Kamlah,&nbsp;M. Verma,&nbsp;C. Denker,&nbsp;N. Huang,&nbsp;J. Lee,&nbsp;H. Wang","doi":"10.1007/s11207-024-02386-9","DOIUrl":"10.1007/s11207-024-02386-9","url":null,"abstract":"<div><p>This study investigates penumbrae and light bridges based on photospheric and chromospheric flow fields and photospheric magnetic fields in active region NOAA 13096. The improved High-resolution Fast Imager (HiFI+) and the GREGOR Infrared Spectrograph (GRIS) acquired high-resolution imaging and spectropolarimetric data at the 1.5-meter GREGOR solar telescope at the Observatorio del Teide, Izaña, Tenerife, Spain. Background-Subtracted Activity Maps (BaSAMs) have been used to locate areas of enhanced activity, Local Correlation Tracking (LCT) provides horizontal proper motions, and near-infrared full-Stokes polarimetry offers access to magnetic fields and line-of-sight velocities. The results show that the decaying active region is characterized by a triangular region between the three leading, positive-polarity sunspots with unfavorable conditions for penumbra formation. This region has a spongy appearance in narrow-band H<span>(alpha )</span> images, shows signs of enhanced activity on small spatial scales, is free of divergence centers and exploding granules, lacks well-ordered horizontal flows, has low flow speeds, and is dominated by horizontal magnetic fields. Umbral cores are inactive, but the interface between pores and penumbral filaments often shows enhanced activity. Moat flows and superpenumbrae are almost always observed, when penumbral filaments are present, even in very small penumbral sectors. However, evidence of the moat flow can also be seen around pores, surviving longer than the decaying penumbral filaments. Light bridges have mainly umbral temperatures, reaching quiet-Sun temperatures in some places, show strong intensity variations, and exhibit weak photospheric horizontal flows, while narrow-band H<span>(alpha )</span> flow maps show substantial inflows.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142438809","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}

{"title":"The KIS Science Data Centre","authors":"Peter Caligari,&nbsp;Faezeh Aghaei,&nbsp;Janek Beck,&nbsp;Nazaret Bello González,&nbsp;Svetlana Berdyugina,&nbsp;Andreas Bührer,&nbsp;Andrea Diercke,&nbsp;Iaroslav Gorbachev,&nbsp;Andrei Y. Gorobets,&nbsp;Marco Günter,&nbsp;Kamal Hamdan,&nbsp;Alexander Hochmuth,&nbsp;Lea Hohl,&nbsp;Petri Kehusmaa,&nbsp;Markus Knobloch,&nbsp;Sani Patel,&nbsp;Markus Schmassmann,&nbsp;Gangadharan Vigeesh,&nbsp;Taras Yakobchuk,&nbsp;Morten Franz,&nbsp;Thomas Hederer,&nbsp;Carl Schaffer,&nbsp;Manuel Collados","doi":"10.1007/s11207-024-02388-7","DOIUrl":"10.1007/s11207-024-02388-7","url":null,"abstract":"<div><p>With the steady improvement of the observing capabilities and numerical simulations, an efficient data management of large data volumes has become mandatory. The Institute for Solar Physics (KIS) has developed the Science Data Centre (SDC), a data infrastructure to store, curate, and disseminate science-ready data from the German solar-observing facilities and other partner institutions. The SDC was also conceived to create and disseminate higher-level data products of added value like inversions from spectropolarimetric data. The SDC archive infrastructure consists of a back-end based on the Rucio science data-management and MongoDB systems and a front-end web interface that allows the user to search and discover data based on search parameters like instrument, date, wavelength range, and target. The SDC archive also provides data access via API and TAP services. The SDC currently offers access to 1299 science-ready datasets from the GRIS instrument at the GREGOR telescope (Tenerife) since 2014, a set of 610 spectra from the LARS at the Vacuum Solar Telescope (VTT, Tenerife) and 202 404 full-disc solar images from the Chromospheric Telescope (ChroTel). The SDC also offers to the community Milne–Eddington inversions of the GRIS spectropolarimetric archived data that can be downloaded as well as tools for data visualization and advanced analysis (e.g., GRISView tool). Many SDC activities have been carried out within the framework of large international data projects like the Horizon 2020 ASTERICS and ESCAPE EU-funded projects under the FAIR (Findable, Accessible, Interoperable, Reusable) principles. New and planned SDC activities include the ingestion of solar data from GREGOR context imaging instruments, flare observations from Ondřejov Observatory (Czech Republic), archiving and dissemination of in-house magnetohydrodynamic simulations, and creation of high-level data products using machine learning. The KIS Science Data Centre is a state-of-the-art data-management infrastructure that curates, archives, and provides access to ground-based science-ready spectropolarimetric and imaging solar data. SDC also provides advanced data visualization and analysis tools and invites data providers to publish their data to the solar and broader (astro)physics community via the SDC data archive.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142438808","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}

{"title":"Daytime Sky Brightness at Dome C, Antarctica: Results from All ESCAPE Campaigns","authors":"Hervé Haudemand,&nbsp;Gerardo Capobianco,&nbsp;Silvano Fineschi,&nbsp;Alessandro Liberatore,&nbsp;Massimo Del Guasta","doi":"10.1007/s11207-024-02387-8","DOIUrl":"10.1007/s11207-024-02387-8","url":null,"abstract":"<div><p>The study of the solar corona is a prominent focus in the field of solar physics. However, conducting ground-based observations of the corona is a challenging task due to the interference caused by the diffused sky brightness, which obscures the faint coronal signal. As a result, such observations are primarily carried out during total solar eclipses. The requirement of a sky-brightness level as low as <span>(10^{-6})</span> times the solar disk brightness (<span>(B_{odot })</span>) is met by few places on Earth, and currently there are only two sites hosting solar observatories that satisfy this criterion, Mauna Loa and Haleakala, both located in Hawaii. Nevertheless, another candidate coronagraphic site was discovered in the Concordia Station at Dome C plateau, Antarctica (<span>(simeq 3300)</span> m a.s.l.). In this article, we show the last results of the Extreme Solar Coronagraphy Antarctic Program Experiment (ESCAPE) during the 38th summer campaign of the Italian Piano Nazionale di Ricerche in Antartide (PNRA). Here, we report a model for estimating the air column, which allows for the first time to account for variations in the Sun’s altitude above the horizon during different observation periods, and we use it to compare the obtained results with previous campaigns. Our results confirm that Dome C is an ideal coronagraphic site with the required sky-brightness level, reaching <span>(1.0-0.7times 10^{-6}B_{odot })</span> in optimal conditions.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02387-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142438787","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}

{"title":"Heavy Elements Abundances Inferred from the First Adiabatic Exponent in the Solar Envelope","authors":"Vladimir A. Baturin,&nbsp;Anna V. Oreshina,&nbsp;Gaël Buldgen,&nbsp;Sergey V. Ayukov,&nbsp;Victor K. Gryaznov,&nbsp;Igor L. Iosilevskiy,&nbsp;Arlette Noels,&nbsp;Richard Scuflaire","doi":"10.1007/s11207-024-02384-x","DOIUrl":"10.1007/s11207-024-02384-x","url":null,"abstract":"<div><p>The first adiabatic exponent profile, noted <span>({{Gamma }_{1}})</span>, computed along adiabatic coordinates (<span>(T)</span>, <span>(rho )</span>), is in the focus of our study. Under conditions of almost fully ionized hydrogen and helium, the <span>({{Gamma }_{1}})</span> profile is quite sensitive to heavy elements ionization. <span>({{Gamma }_{1}})</span> decreases in regions where an element is partially ionized. The recent helioseismic structural inversion is obtained with an accuracy better than <span>({{10}^{-4}})</span> in the most of the adiabatic convective zone that allows to study ionization variations. The aim is to determine the major heavy elements content in the solar convective zone. The method of our research is synthesis of the <span>(Gamma _{1})</span> profile, which is based on a linear combination of the contributions of individual heavy elements. The idea of the approach was proposed and justified by Baturin et al. (2022). We find the best approximation of the inverted profile <span>({{Gamma }_{1}})</span> adjusting the abundances of major elements (C, N, O, Ne), meanwhile the abundances of elements heavier than neon are fixed. We synthesize the theoretical <span>({{Gamma }_{1}})</span> profile using the SAHA-S equation of state, and are able to reproduce the inverted profiles with an accuracy of <span>((1-2)cdot {{10}^{-5}})</span>. Total mass fraction of heavy elements found with this method is <span>(Z=0.0148pm 0.0004)</span>. The oxygen logarithmic abundance is <span>(8.70pm 0.03)</span>, carbon <span>(8.44pm 0.04)</span>, nitrogen <span>(8.12pm 0.08)</span>, and neon <span>(8.17pm 0.09)</span>. The obtained estimations of oxygen and carbon agree with spectroscopic abundances by Asplund, Amarsi, and Grevesse (2021).</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142411203","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}