Solar Physics最新文献

{"title":"Investigating Solar Wind Outflows from Open–Closed Magnetic Field Structures Using Coordinated Solar Orbiter and Hinode Observations","authors":"Nawin Ngampoopun,&nbsp;Roberto Susino,&nbsp;David H. Brooks,&nbsp;Roberto Lionello,&nbsp;Lucia Abbo,&nbsp;Daniele Spadaro,&nbsp;Deborah Baker,&nbsp;Lucie M. Green,&nbsp;David M. Long,&nbsp;Stephanie L. Yardley,&nbsp;Alexander W. James,&nbsp;Marco Romoli,&nbsp;Silvio M. Giordano,&nbsp;Aleksandr Burtovoi,&nbsp;Federico Landini,&nbsp;Giuliana Russano","doi":"10.1007/s11207-025-02438-8","DOIUrl":"10.1007/s11207-025-02438-8","url":null,"abstract":"<div><p>ESA/NASA’s Solar Orbiter (SO) enables us to study the solar corona at closer distances and from different perspectives, which helps us to gain significant insights into the origin of the solar wind. In this work, we present the analysis of solar wind outflows from two locations: a narrow open-field corridor and a small, mid-latitude coronal hole. These outflows were observed off-limb by the Metis coronagraph onboard SO and on-disk by the Extreme Ultraviolet Imaging Spectrometer (EIS) onboard Hinode. Magnetic field extrapolations suggest that the upflow regions seen in EIS were the sources of the outflowing solar wind observed with Metis. We find that the plasma associated with the narrow open-field corridor has higher electron densities and lower outflow velocities compared to the coronal hole plasma in the middle corona, even though the plasma properties of the two source regions in the low corona are found to be relatively similar. The speed of the solar wind from the open-field corridor also shows no correlation with the magnetic field expansion factor, unlike the coronal hole. These pronounced differences at higher altitudes may arise from the dynamic nature of the low-middle corona, in which reconnection can readily occur and may play an important role in driving solar wind variability.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02438-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143761708","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":"Transverse Oscillations in Thin Magnetic Tubes with Elliptical Cross-Sections: The Effect of Field Aligned Flow","authors":"Igor Lopin","doi":"10.1007/s11207-025-02460-w","DOIUrl":"10.1007/s11207-025-02460-w","url":null,"abstract":"<div><p>The effect of longitudinal plasma flow on transverse oscillations in the thin magnetic tubes with elliptical cross-sections is examined. The backward propagating waves of the <span>(M)</span>-kink mode (polarized along the major axis) and <span>(m)</span>-kink mode (polarized along the minor axis) are found to reverse their propagation direction at certain flow thresholds. The critical flow for the <span>(M)</span>-kink mode is lower than in a circular tube and is close to the internal Alfvén speed. This result is of particular interest within the concept of existence of negative energy waves in solar waveguides. Both modes are subjected to the Kelvin–Helmholtz (KH) instability, and the <span>(M)</span>-mode is more stable than the <span>(m)</span>-mode. Magnetic tubes with significant ellipticity are more resistant to the KH instability than circular tubes. In the quasi-standing wave regime, the frequencies of both modes decrease and the frequency ratio <span>(omega _{m}/omega _{M})</span> increases with faster flows. The obtained results are used to interpret the observed transverse oscillations of the solar limb spicules and their helical motions in terms of the <span>(M)</span>- and <span>(m)</span>-kink modes.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143749170","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":"A New Implementation of a Fourth-Order CESE Scheme for 3D MHD Simulations","authors":"Chaowei Jiang,&nbsp;Ling Zhang","doi":"10.1007/s11207-025-02452-w","DOIUrl":"10.1007/s11207-025-02452-w","url":null,"abstract":"<div><p>This paper is devoted to the description and validation of a new implementation of a fourth-order space–time conservation-element and solution-element (CESE) scheme to numerically solve the time-dependent, three-dimensional (3D) magnetohydrodynamic (MHD) equations. The core of the scheme is that, with the aid of a grid staggered in space and time, the conservative variables are advanced by integration of the controlling equation in the space–time four-dimensional domain by utilizing Taylor expansion, and their spatial derivatives are computed by finite difference with <span>(p)</span> order derivatives from <span>(p-1)</span> order ones. The new scheme achieves fourth-order accuracy in both space and time simultaneously, using a compact stencil identical to that in the second-order CESE scheme. We provide a general framework for convenience of programming such that the scheme can be easily extended to arbitrarily higher order by including higher-order terms in the Taylor series. A suite of 3D MHD tests demonstrate that the fourth-order CESE scheme at relatively low grid resolutions can obtain reliable solution comparable to the second-order CESE scheme at four-times higher resolution, and showing a very high efficiency in computing by using only around <span>(5%)</span> of the computing resources.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143716806","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":"Arecibo Multifrequency IPS Observations: Solar-Wind Density Turbulence Scale Sizes and Their Anisotropy","authors":"P. K. Manoharan,&nbsp;C. J. Salter","doi":"10.1007/s11207-025-02445-9","DOIUrl":"10.1007/s11207-025-02445-9","url":null,"abstract":"<div><p>We present an analysis of interplanetary scintillation (IPS) observations conducted with the Arecibo 305-m radio telescope during the minimum phase at the end of Solar Cycle 24 and the onset of Solar Cycle 25. These observations span a broad frequency range of ∼ 300 to 3100 MHz, encompassing the P-, L-, and S-bands, and cover heliocentric distances from ∼ 5 to 200 solar radii. Each L-band observation provided simultaneous measurements across a bandwidth of approximately 600 MHz. Furthermore, whenever feasible, the near-simultaneous measurements of a source acquired across all three frequency bands were useful to study the scintillation characteristics over a much wider frequency band along the same line of sight through the heliosphere. The dynamic spectrum of the scintillations obtained at the L-band shows a systematic decrease in the scintillation index from the lowest to the highest frequency, offering valuable insight into the influence of the solar wind density microstructures responsible for scintillation. Analyses of the scintillation index (<span>(m)</span>) for multiple sources at the L-band, along with near-simultaneous observations of selected sources covering the P-, L-, and S-bands, clearly demonstrate a wavelength dependence of <span>(m propto lambda ^{omega })</span>, which inherently leads to a dependence of <span>(m)</span> on the Fresnel scale, when considering the effective distance to the scattering screen, <span>(z)</span>. The index <span>(omega )</span> ranges between ∼ 1 and 1.8. The average <span>(omega )</span> value of a source, determined from observations made on multiple days (i.e., at a range of solar offsets to mitigate the influence of possible day-to-day variations in solar-wind turbulence) exhibits variability across sources. The results on the radial dependence of scintillation agree with earlier IPS measurements. The temporal power spectra obtained over the wide frequency range exhibit a power-level evolution in accordance with the wavelength dependence and a broadening with an increasing observation frequency. Furthermore, the increased temporal–frequency rounding of the “Fresnel knee” in the spectrum with the observing frequency suggests a novel phenomenon: an increase in anisotropy as the scale size of the density–turbulence structure decreases.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143716809","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":"Influence of the Deformation of Coronal Mass Ejections on Their in-Situ Fitting with Circular-Cross-Section Flux Rope Models","authors":"Bin Zhuang,&nbsp;Noé Lugaz,&nbsp;Nada Al-Haddad,&nbsp;Charles J. Farrugia,&nbsp;Ute Amerstorfer,&nbsp;Emma E. Davies,&nbsp;Manuela Temmer,&nbsp;Hannah T. Rüdisser,&nbsp;Wenyuan Yu,&nbsp;Tingyu Gou,&nbsp;Réka M. Winslow","doi":"10.1007/s11207-025-02444-w","DOIUrl":"10.1007/s11207-025-02444-w","url":null,"abstract":"<div><p>Understanding the properties, especially the magnetohydrodynamic (MHD) invariants, of coronal mass ejections (CMEs) measured in-situ is key to bridging the CME properties from the Sun to interplanetary space. In order to investigate CMEs based on in-situ measurements that provide a one-dimensional (1D) cut of the CME parameters over the spacecraft trajectory, various magnetic flux rope (MFR) models have been developed, among which the models with a circular cross section are the most popular and widely used. CMEs are found to be deformed during their propagation in interplanetary space, in which the cross section may be flattened in the direction of propagation, leading to the development of an elliptical or even pancake-like shape. We use numerical MHD simulations in 2.5D to investigate the influence of the CME deformation on the in-situ fitting using two linear force-free MFR models with a circular cross section, and we focus on the axial and poloidal magnetic fluxes, which are conserved in the ideal MHD frame. We quantitatively compare the fitted axial and poloidal fluxes with those in the simulations. We find that both models underestimate the axial flux compared to that in the simulations and that such underestimations depend on the CME deformation. However, the fitting of the poloidal flux is independent of the deformation. We discuss the reasons for the axial flux underestimation and the implication of the CME deformation for the CME in-situ fitting.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143707131","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":"Aditya Solar Wind Particle Experiment (ASPEX) on Board Aditya—L1: The Solar Wind Ion Spectrometer (SWIS)","authors":"Prashant Kumar,&nbsp;Bhas Bapat,&nbsp;Manan S. Shah,&nbsp;Hiteshkumar L. Adalja,&nbsp;Arpit R. Patel,&nbsp;Pranav R. Adhyaru,&nbsp;M. Shanmugam,&nbsp;Dibyendu Chakrabarty,&nbsp;Swaroop B. Banerjee,&nbsp;K. P. Subramanian,&nbsp;Aveek Sarkar,&nbsp;Tinkal Ladiya,&nbsp;Jacob Sebastian,&nbsp;Abhishek Kumar,&nbsp;Sushil Kumar,&nbsp;Nishant Singh,&nbsp;M. B. Dadhania,&nbsp;Santosh V. Vadawale,&nbsp;Shiv Kumar Goyal,&nbsp;Neeraj Kumar Tiwari,&nbsp;Aaditya Sarda,&nbsp;Deepak Kumar Painkra,&nbsp;Piyush Sharma,&nbsp;Abhishek J. Verma,&nbsp; Yogesh,&nbsp;P. Janardhan,&nbsp;Anil Bhardwaj","doi":"10.1007/s11207-025-02443-x","DOIUrl":"10.1007/s11207-025-02443-x","url":null,"abstract":"<div><p>The Solar Wind Ion Spectrometer (SWIS) instrument is a part of the Aditya Solar Wind Particle Experiment (ASPEX), one of the three in situ observation instruments on board India’s Aditya-L1 spacecraft. SWIS comprises two Top-Hat analysers (THA-1 and THA-2), which have a 360^∘ angular coverage in the ecliptic plane and in the plane perpendicular to the ecliptic plane, respectively, with opening angles of <span>(pm 1.5^{circ })</span>. Both are electrostatic scanning instruments designed to measure the flux, the energy distribution and the angular distribution of the solar wind particles, covering the energy range of 0.1 – 20.0 keV with a 5 s cadence and 8% energy resolution. THA-1 has an additional species separation capability, based on a magnetic mass analyser (MMA) primarily designed to separate H⁺ and He²⁺, giving us the ability to measure the energy-, angle-, and time-dependent variation of the all-important helium abundance ratio in the ambient solar wind and in transient structures like interplanetary coronal mass ejections (ICME), stream interaction regions (SIR) passing through the location of the spacecraft. Over the life of the mission, the multidirectional observational capabilities of SWIS are expected to provide valuable data on the variations in the primary composition of solar wind, its velocity distribution, and its directional anisotropy. The SWIS instrument will also capture the low-energy end of the supra-thermal population in the solar wind. A special feature of the instrument is its user-level configurability for specific studies. The instrument will generate detailed information on helium abundance, its variability, and its connection to the solar wind speed.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143698530","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":"Aditya Solar Wind Particle Experiment on Board Aditya–L1: The Supra-Thermal and Energetic Particle Spectrometer","authors":"Shiv Kumar Goyal,&nbsp;Neeraj Kumar Tiwari,&nbsp;Arpit R. Patel,&nbsp;M. Shanmugam,&nbsp;Santosh V. Vadawale,&nbsp;Dibyendu Chakrabarty,&nbsp;Jacob Sebastian,&nbsp;Bijoy Dalal,&nbsp;Piyush Sharma,&nbsp;Aveek Sarkar,&nbsp;Aaditya Sarda,&nbsp;Tinkal Ladiya,&nbsp;Abhishek J. Verma,&nbsp;Nishant Singh,&nbsp;Sushil Kumar,&nbsp;Deepak Kumar Painkra,&nbsp;Prashant Kumar,&nbsp;Manan S. Shah,&nbsp;Pranav R. Adhyaru,&nbsp;Hiteshkumar L. Adalja,&nbsp;Swaroop B. Banerjee,&nbsp;K. P. Subramanian,&nbsp;Bhas Bapat,&nbsp;M. B. Dadhania,&nbsp;Abhishek Kumar,&nbsp;P. Janardhan,&nbsp;Anil Bhardwaj","doi":"10.1007/s11207-025-02441-z","DOIUrl":"10.1007/s11207-025-02441-z","url":null,"abstract":"<div><p>Aditya–L1, the first dedicated Indian solar mission, was launched on 02 September 2023 and has been placed in a halo orbit around the first Lagrange point (L1) of the Sun-Earth system on 06 January 2024. Aditya Solar wind Particle EXperiment (ASPEX) is one of the three in situ science experiments on board the Aditya–L1 mission that provides measurements of primarily protons and alpha particles in the solar wind, suprathermal, and energetic particles in the energy range from 100 eV to 6 MeV/nucleon. ASPEX consists of two independent spectrometers: the Solar Wind Ion Spectrometer (SWIS: 100 eV – 20 keV) and Supra Thermal and the Energetic Particle Spectrometer (STEPS: 20 keV/nucleon – 6 MeV/nucleon). In this article, we provide the details of the STEPS configuration, ground calibration, and in–flight performance. After the launch of Aditya–L1, two STEPS units were switched–on during the Earth-bound phase on 10 September 2023. STEPS has carried out measurements in the Earth-bound orbit for altitudes <span>(gtrsim 8)</span> R_<i>E</i>, and also in the cruise phase from the Earth to the halo orbit, and has been continuously operational after insertion to the L1 orbit. The performance of STEPS is as expected during all the phases of the mission so far and all its observations are found to be consistent with similar measurements from other contemporary instruments at the L1 point.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143667982","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":"Evolution of Photospheric Magnetic Field and Electric Currents During the X1.6 Flare in Active Region NOAA 12192","authors":"Partha Chowdhury,&nbsp;Belur Ravindra,&nbsp;Sanjiv Kumar Tiwari","doi":"10.1007/s11207-025-02451-x","DOIUrl":"10.1007/s11207-025-02451-x","url":null,"abstract":"<div><p>The dynamics of magnetic fields in the Sun’s active regions play a key role in triggering solar eruptions. Studies have shown that changes in the photosphere’s magnetic field can destabilize the large-scale structure of the corona, leading to explosive events such as flares and coronal mass ejections (CMEs). This paper delves into the magnetic field evolution associated with a powerful X1.6 class flare that erupted on October 22, 2014, from the flare-rich active region NOAA 12192. We track these changes using high-resolution vector magnetograms from the Helioseismic and Magnetic Imager (HMI) on NASA’s Solar Dynamic Observatory (SDO). Our analysis reveals that a brightening, a precursor to the flare, began near the newly emerged, small-scale bipolar flux regions. During the X1.6 flare, the magnetic flux in both polarities displayed emergence and cancellation. The total current within the active region peaked during the flare. However, it is a non-CME event, and the ratio of direct-to-return current value remains close to 1. The large flare in this active region occurred when the net current in both polarities attained the same sign. This implies that the Lorentz force, a consequence of the interaction between currents and magnetic fields, would have pushed the field lines together in this scenario. This reconnection of opposing magnetic fields is believed to be the driving force behind the major flare in this active region.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143667983","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":"N-S Asymmetry and Periodicity of Solar Activity from Solar Cycles 21 – 24","authors":"S. F. Ibrahim,&nbsp;N. K. Hafez,&nbsp;M. A. El-Borie,&nbsp;A. A. Bishara,&nbsp;A. M. El-Taher","doi":"10.1007/s11207-025-02442-y","DOIUrl":"10.1007/s11207-025-02442-y","url":null,"abstract":"<div><p>Continuous wavelet power spectrum approach has been utilized to examine the short- and long-term fluctuations of solar plage area (PA), solar flare index (SFI), and sunspot numbers (SSNs) from 1976 to 2022. Based on the distribution of monthly data from the hemisphere SSNs, the monthly average of the solar parameters under consideration has been divided into northern and southern groups. Besides, the N-S asymmetry, the periodicity, the interconnection, and phase synchronization between the northern and southern groups of the solar flare index and plage area have been presented using the wavelet technique. The findings show that the northern group of PAs has short and intermediate periods of 0.9, 1.5, 2.5, and 3.5 years, whereas the southern group shows the prevalence of periods of 0.7, 1.9, and 3.2 years. In contrast, the northern group of SFI displays periods of 0.6, 0.8, 1.5, and 3.5 years, whereas the southern group confirms the presence of discrete periods of 0.7 and 1.9 years. The PA and SFI data sets for the Solar Cycles (SCs) 21 – 24 show little correlation and fewer short periods in the cross-wavelet power spectra (XWT) and wavelet coherence (WTC) spectra between the northern and southern hemispheres.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02442-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143655195","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":"The Fluxgate Magnetometer (MAG) on Board Aditya-L1 Spacecraft","authors":"Vipin K. Yadav,&nbsp;Y. Vijaya,&nbsp;B. Krishnam Prasad,&nbsp;P. T. Srikar,&nbsp;Monika Mahajan,&nbsp;K. V. L. N. Mallikarjun,&nbsp;Syeeda N. Zamani,&nbsp;Satyanarayana Kumari B.,&nbsp;K. A. Lohar,&nbsp;M. M. Kandpal,&nbsp;S. Narendra,&nbsp;Vijay S. Rai,&nbsp;Abhijit A. Adoni,&nbsp;D. R. Veeresha,&nbsp;Smaran T.S.,&nbsp;Kalpana A.,&nbsp;Nandita Srivastava,&nbsp;Geeta Vichare","doi":"10.1007/s11207-025-02440-0","DOIUrl":"10.1007/s11207-025-02440-0","url":null,"abstract":"<div><p>The Fluxgate Magnetometer (MAG) is one of the seven instruments on board Aditya-L1 spacecraft to sample the local magnetic field environment around the first Lagrangian point (L1) while continuously observing the Sun. These in situ magnetic field measurements are crucial in detecting coronal mass ejections (CMEs), as well for space weather studies in the vicinity of the Earth, and the apparent detection of solar plasma wave signatures at L1. The MAG payload has a set of fluxgate magnetic sensors mounted on the Sun-viewing panel deck and is configured to deploy along the negative roll direction of the spacecraft. Two sets of triaxial fluxgate sensors are mounted on a 6-m long boom with one set at the tip of the boom and the other at the centre of the boom around 3 m away from the spacecraft towards the boom tip. The boom is mounted to be deployed along the –roll axis of the spacecraft. The power supply and the processing electronics for the MAG payload are enclosed in a box, which is placed inside the +yaw panel of the spacecraft. Each of the two triaxial fluxgate sensors measures the interplanetary magnetic field vectors at L1 in the default range of ± 256 nT per axis once every 125 ms. The observed magnetic field data is time stamped at the spacecraft with the on board clock and transmitted to ground once every day when the visibility is for 12 hours, along with the house-keeping parameters, ephemeris, and the science data from the other six payloads.</p><p>In this technical paper, the Aditya-L1 MAG instrument details are presented, along with the initial observations in the halo-orbit around L1.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143638451","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}