发布求助
文献互助 智能选刊 最新文献

Geomagnetism and Aeronomy最新文献

筛选
英文 中文
Acceleration Parameters of Coronal Mass Ejections Associated with Solar Proton Events of February–July 2023 2023年2 - 7月与太阳质子事件相关的日冕物质抛射加速参数
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700373
V. A. Ozheredov, A. B. Struminskii, I. Yu. Grigor’eva
{"title":"Acceleration Parameters of Coronal Mass Ejections Associated with Solar Proton Events of February–July 2023","authors":"V. A. Ozheredov,&nbsp;A. B. Struminskii,&nbsp;I. Yu. Grigor’eva","doi":"10.1134/S0016793224700373","DOIUrl":"10.1134/S0016793224700373","url":null,"abstract":"<p>The methods proposed earlier by the authors to extrapolate the positions of coronal mass ejections (CMEs) to the propagation times from the beginning to the escape into interplanetary space by the SOHO/LASCO coronagraph data have been used. This makes it possible to obtain the CME kinematic parameters needed to refine the solar proton acceleration model for the events of February 17, 24–25, and 28 and July 16–17, 2023 (the most significant proton events of the ascending phase of solar cycle 25). For proton flares on the visible disk of the Sun, it is found that CMEs should have started to accelerate before the selected zero time (heating of the flare plasma to 12 MK (GOES), electron acceleration greater than 100 keV, and the onset of nonthermal emission (ACS SPI, RSTN). Particle and CME accelerations continue at least during the active phase of the flare (<i>T</i> &gt; 12 MK). Evidence has been obtained for the sequential acceleration of two CMEs, slow and fast, in the event of February 25, 2023, when the second CME caught up with the first and engulfed it (“cannibalism”).</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1273 - 1280"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423338","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Features of the Joule Dissipation in the Solar Atmosphere 太阳大气中焦耳耗散的特征
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700300
A. V. Stepanov, V. V. Zaitsev, E. G. Kupriyanova
{"title":"Features of the Joule Dissipation in the Solar Atmosphere","authors":"A. V. Stepanov,&nbsp;V. V. Zaitsev,&nbsp;E. G. Kupriyanova","doi":"10.1134/S0016793224700300","DOIUrl":"10.1134/S0016793224700300","url":null,"abstract":"<p>The decisive role of the neutral component of solar plasma in the dissipation of electric currents in magnetic flux tubes is shown. For the first time, the dependences of the Cowling resistivity and the rate of the Joule dissipation were obtained for various current magnitudes in a wide range of heights, from the photosphere to the corona. Based on the atmospheric model of Avrett and Loeser (2008) it was shown that the Cowling resistivity exceeds the classical (Spitzer) resistivity in the chromosphere and the transition region. The Spitzer resistivity prevails over the Cowling one at the altitudes less than 300–1000 km depending on the electric current magnitude. The Cowling resistivity plays the main role at the electric currents of more than 10<sup>9</sup> A in the corona with a relative density of neutral atoms ∼10<sup>–7</sup>. It was found that the maximum of the Joule dissipation is located at the altitude of about 2100 km, which creates favorable conditions for formation of the chromosphere-corona transition region and heating of the corona. Anomalous (turbulent) resistance requires a lot of tiny current filaments in a flux tube. The role of Joule dissipation in the heating of pre-flare plasma and in the formation of the sunspot light bridges is discussed.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1203 - 1214"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423225","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Ultraviolet and X-ray Precursors of Solar Flares 太阳耀斑的紫外线和x射线前体
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700531
T. D. Shohin, Yu. E. Charikov, A. N. Shabalin
{"title":"Ultraviolet and X-ray Precursors of Solar Flares","authors":"T. D. Shohin,&nbsp;Yu. E. Charikov,&nbsp;A. N. Shabalin","doi":"10.1134/S0016793224700531","DOIUrl":"10.1134/S0016793224700531","url":null,"abstract":"<p>We examined pre-flare brightenings in ultraviolet (UV) and X-ray emissions during flares on September 23, 2014, and January 11, 2013. We analyzed UV maps at nine wavelengths based on SDO/AIA data and RHESSI X-ray images over a one-hour interval before the onset of the flare. We obtained the temperature and emission measure dependencies of the quasi-thermal X-ray emission during the precursor periods. The plasma temperature in the precursor regions exceeded 1 MK. The emission in the extreme UV (EUV) lines was used to identify the filamentary structure. The SDO/HMI vector magnetic field data allows the reconstruction of the magnetic field pattern in the coronal part of the filaments using the NLFFF method. We found magnetic field structures containing flux ropes during the precursor phase. We discuss the role of magnetic flux ropes, their temporal evolution in the dynamics of the pre-flare stage, and the transition from the precursor to the explosive phase of the flares. We conclude that there is a causal relationship between the precursors of the flares on September 23, 2014, and January 11, 2013, and the events themselves.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1386 - 1394"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423137","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Comparison of Solar Wind Parameters with Characteristics of Coronal Holes 日冕洞特征与太阳风参数的比较
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700348
I. A. Berezin, A. G. Tlatov, E. A. Illarionov
{"title":"Comparison of Solar Wind Parameters with Characteristics of Coronal Holes","authors":"I. A. Berezin,&nbsp;A. G. Tlatov,&nbsp;E. A. Illarionov","doi":"10.1134/S0016793224700348","DOIUrl":"10.1134/S0016793224700348","url":null,"abstract":"<p>Determining the speed of the solar wind emanating from coronal holes near the Sun is a key problem for modeling plasma parameters throughout the heliosphere. Plasma temperature and density, in addition to speed, are the input parameters to global magnetohydrodynamics models, but the estimated temperature and density boundary conditions are calculated from the simulated solar wind speed. In this study, we analyzed how long-term variations in the properties of open magnetic field sources modeled from different series of magnetograph observations are related to the plasma parameters measured by satellite. The analysis also considers coronal holes based on SDO/AIA 193 Å and solar wind speed observations in the Wang-Sheeley-Arge approximation (WSA). We found that during the period 2015–2023, the areas of equatorial coronal holes correlate better with the observed solar wind speed than the results of WSA simulations. Among the three considered series of magnetographic observations (STOP, SDO/HMI, GONG), during the period of minimum solar activity, calculations based on STOP data perform better.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1250 - 1256"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423334","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
The Slope of the Magnetic Field in Sunspots of Leading and Tail Polarity 太阳前尾极性黑子磁场的斜率
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700403
K. A. Tlatova, A. G. Tlatov, V. G. Nagnibeda
{"title":"The Slope of the Magnetic Field in Sunspots of Leading and Tail Polarity","authors":"K. A. Tlatova,&nbsp;A. G. Tlatov,&nbsp;V. G. Nagnibeda","doi":"10.1134/S0016793224700403","DOIUrl":"10.1134/S0016793224700403","url":null,"abstract":"<p>In the paper, we examine the α inclination of the magnetic field of sunspots relative to the vertical. To determine the deviation angle α, a method to search for differences in the maximum of the longitudinal component of the magnetic field at various distances of spots from the central meridian in the eastern and western hemispheres of the Sun was used. Particular attention has been paid to the difference in the angles α for spots of leading and tail polarity of the magnetic field. Deviation angles α were shown to depend on the logarithm of the area while the dependences have opposite signs: α<sub>L</sub> = 0.45°(±0.5) + 2.085°(±0.5) log <i>S</i>, (<i>r</i> = 0.95) for nuclei of leading polarity spots (L) and α<sub>T</sub> = 5.43°(±1.0) – 3.95°(±0.7) log <i>S</i>, (<i>r</i> = 0.93) for nuclei of tail polarity (T). Here, the deviation of magnetic fields to the western limb is taken as a positive value. The found dependencies indicate the ascent of U-shaped force tubes.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1295 - 1298"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423339","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Parameters of Starspots on the Surface of the Red Dwarf V647 Her 红矮星V647 Her表面的星黑子参数
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700464
N. I. Bondar’, I. Yu. Alekseev, K. A. Antonyuk, N. V. Pit’
{"title":"Parameters of Starspots on the Surface of the Red Dwarf V647 Her","authors":"N. I. Bondar’,&nbsp;I. Yu. Alekseev,&nbsp;K. A. Antonyuk,&nbsp;N. V. Pit’","doi":"10.1134/S0016793224700464","DOIUrl":"10.1134/S0016793224700464","url":null,"abstract":"<p>Based on the available photometric data for the star V647 Her, including those obtained from photographic archives, we considered the yearly-mean brightness variability over the time interval 1939–2022. The dense data series obtained in 2019 and 2022 at CrAO as well as the sample for 2004 from the SuperWASP catalog showed changes in light curves and in color indices of the star with a period of 20.69 days. Changes in the <i>V–I</i> color index indicate the presence of cool spots on its surface. The parameters of starspots were calculated within the zonal model for each year and it was found that the temperature of the spots is 500–600 K lower than the temperature of the quiet photosphere with <i>T</i><sub>eff</sub> = 3300 K, the spots occupy from 8 to 30% of the entire surface of the star in different years. The spottedness of the star’s photosphere is an indicator of its activity, and according to the interval between the epochs of minimum spottedness, we derived a characteristic time between the minima in activity of V647 Her of about 60 years, and the duration of the maximum of activity of about 5 years.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1334 - 1341"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423088","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Ion Instabilities in the Vicinity of the Earth’s Bow Shock Front in the Case of Weakly Magnetized Plasma 弱磁化等离子体中地球弓形激波前沿附近离子的不稳定性
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700427
J. A. Kropotina, D. B. Matrosova, A. A. Petrukovich, O. M. Chugunova, A. M. Bykov
{"title":"Ion Instabilities in the Vicinity of the Earth’s Bow Shock Front in the Case of Weakly Magnetized Plasma","authors":"J. A. Kropotina,&nbsp;D. B. Matrosova,&nbsp;A. A. Petrukovich,&nbsp;O. M. Chugunova,&nbsp;A. M. Bykov","doi":"10.1134/S0016793224700427","DOIUrl":"10.1134/S0016793224700427","url":null,"abstract":"<p>The structure of the quasi-perpendicular bow shock of the Earth observed by the MMS spacecraft on 31 January 2017 with an Alfvén Mach number of approximately 10 and plasma parameter β of approximately 3, has been simulated using the Maximus hybrid kinetic code. We investigated types of instabilities governing the front structure and showed that in this case both ion Weibel and Alfvén ion cyclotron instabilities can arise at the shock foot simultaneously, thus leading to fast magnetic oscillations with a relative variation close to unity. Some signatures of the mirror instability were found in the near downstream. Simulation also showed that the front structure substantially differ for shock inclination angles of 50° and 75°.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1303 - 1309"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423336","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Maximum Energy of Solar Flares in the Modern Era 现代太阳耀斑的最大能量
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S0016793224700543
V. L. Merzlyakov
{"title":"Maximum Energy of Solar Flares in the Modern Era","authors":"V. L. Merzlyakov","doi":"10.1134/S0016793224700543","DOIUrl":"10.1134/S0016793224700543","url":null,"abstract":"<p>The maximum energy of a solar flare is found using a model of particle acceleration in a magnetic <i>X</i>-singularity. Based on a comparison of this model with observed extreme events, it was determined that flares with the highest possible energy have already been observed. These include events of 1859, 1940, 2003, which had an X-ray class of <i>X</i>40 ± 5 (according to the GOES classification). In this case, the maximum flare energy in the modern era does not exceed 5 × 10<sup>32</sup> erg, and such powerful flares occur at intervals of about 70 years.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1395 - 1397"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423093","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Contraction Effect of Coronal Loops during the Flare of February 24, 2023 2023年2月24日耀斑期间日冕环的收缩效应
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S001679322470052X
V. F. Melnikov, N. S. Meshalkina
{"title":"Contraction Effect of Coronal Loops during the Flare of February 24, 2023","authors":"V. F. Melnikov,&nbsp;N. S. Meshalkina","doi":"10.1134/S001679322470052X","DOIUrl":"10.1134/S001679322470052X","url":null,"abstract":"<p>In this paper, the dynamics of loop-like structures and related phenomena during the solar flare on February 24, 2023 are investigated. A new character of the dynamics of the coronal loop system during the flare has been studied, consisting in compression (lowering) of the loops both during the growth and decay phases of the flare. It was found that a sharp decrease in height began with the appearance of intense nonstationary plasma fluxes (ejections) observed mainly in the vicinity of the eastern footpoints of the coronal loop system. It was concluded that the rapid (at a speed of up to 25 km/s) compression of the coronal loop system can be explained by a decrease in free magnetic energy (a decrease in the vortex phi-component of the magnetic field) caused by the observed non-stationary plasma eruptions from the vicinity of the loops, as well as possible Joule dissipation of electric currents in the loops.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1381 - 1385"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423103","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Statistical Characteristics of Active Regions and Flare Ribbons Associated with Large Flares 与大耀斑相关的活动区域和耀斑带的统计特征
IF 0.7 4区 地球科学
Geomagnetism and Aeronomy Pub Date : 2025-02-14 DOI: 10.1134/S001679322470035X
O. S. Gopasyuk
{"title":"Statistical Characteristics of Active Regions and Flare Ribbons Associated with Large Flares","authors":"O. S. Gopasyuk","doi":"10.1134/S001679322470035X","DOIUrl":"10.1134/S001679322470035X","url":null,"abstract":"<p>We present the results of a statistical study of the characteristics of active regions (ARs) and ribbons associated with flares of <i>GOES</i> class M5.0 and larger, occurring from February 2011 to December 2022 within 40° of the central meridian. A total of 60 flares met these criteria, of which 39 were eruptive and 21 confined. We used <i>SDO</i>/HMI and <i>SDO</i>/AIA data to obtain the magnetic reconnection fluxes and rates. Magnetic reconnection fluxes and ribbon areas of confined and eruptive flares correlate with the flares <i>GOES</i> class. For flares of the same <i>GOES</i> class in confined events, compared to eruptive ones, the mean magnetic flux density in the ribbon is higher. Reconnection rates in confined and eruptive flares showed a temporal evolution similar to observed hard X-ray (HXR) emission. The fraction of AR involved in reconnection is larger in eruptive flares and for both types of events it decreases with increasing distance between the flare and the AR center. For the same fraction of AR involved in the flare, eruptive events, compared to confined ones, are located at distances twice as far from the AR center. Eruptive flares tend to occur in compact ARs at the periphery, while confined ones occur in extended ARs near the center.</p>","PeriodicalId":55597,"journal":{"name":"Geomagnetism and Aeronomy","volume":"64 8","pages":"1257 - 1266"},"PeriodicalIF":0.7,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423337","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
首页 上一页 下一页 尾页
0
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
提示
您的信息不完整，为了账户安全，请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
现在去查看 取消
×
提示
确定
请完成安全验证×
相关产品
×
本文献相关产品
联系我们：info@booksci.cn Book学术提供免费学术资源搜索服务，方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。 Copyright © 2023 布克学术 All rights reserved.
京ICP备2023020795号-1
ghs 京公网安备 11010802042870号
Book学术文献互助
Book学术文献互助群
群 号：604180095
Book学术官方微信
小红书