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1825 Articles

Published in last 50 years

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  • Occurrence Of Flares
  • Occurrence Of Flares
  • Major Flares
  • Major Flares
  • Flare Events
  • Flare Events
  • X-ray Flares
  • X-ray Flares
  • Bright Flare
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  • Large Flares

Articles published on Flaring Activity

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Latitudinal and Solar Cycle Distribution of Extreme (≥X5) Flares During 1976–2018

Abstract We studied the latitudinal and solar cycle distribution of extreme (≥X5) solar flares spanning 1976–2018. We found that all such flares were confined within the latitudinal range of [S30, N35]. Nonetheless, the majority of these flares during different solar cycles were confined in different latitudinal scopes. Statistical results showed that the southeast quadrant experienced the highest activity of extreme flares. 47.5% of the extreme flares occurred within the latitudes ≤15° of the two hemispheres, with 26.2%, 31.1%, and 42.6% in the latitudinal bands [5°, 10°], >20° and [11°, 20°] of both hemispheres, respectively. Significant N–S asymmetries were observed in the ascending phase of SC 21, the descending phase of SC 23, and both phases of SC 24. Other phases showed asymmetries primarily in latitudinal distribution. The proportion of extreme flares in the ascending phases of SCs 21–24 was 22.2%, 33.3%, 38.9%, and 50%, respectively. Stronger flares (≥X10) were more likely to occur in the descending phase, with 39% of X5–X9 flares and 20% of (≥X10) flares occurring in the ascending phase. On average, 83.6% of extreme flares occurred within a period extending from two years prior to three years following the solar peak, according to our statistical analysis, with specific percentages for each cycle being 88.9%, 100%, 61.1%, and 75%.

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  • Research in Astronomy and Astrophysics
  • Dec 1, 2024
  • Qi Li + 2
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Elevated serum interferon-α2 associates with activity and flare risk in Juvenile-onset Systemic Lupus Erythematosus.

This study investigated serum IFN-α2 as a putative marker of disease activity and predictor of disease flares in juvenile systemic lupus erythematosus (jSLE). 222 serum samples were analysed, including 28 healthy controls (HCs), 88 JSLE (159 samples), and 35 juvenile idiopathic arthritis (JIA) patients. IFN-α2 levels were determined using Single-molecule array (Simoa). Cross-sectionally, median IFN-α2 levels were compared between patient groups and disease activity state sub-groups. Time to flare was analysed by linear regression. Longitudinally, the ability of the IFN-α2 and other traditional biomarkers (erythrocyte sedimentation rate/ESR, low C3 and anti-dsDNA antibodies) to detect and predict flares was assessed via a generalised linear mixed model. Cross-sectional analysis showed higher median IFN-α2 levels in the active/intermediate group (median 3,185 fg/mL, IQR 48-13,703) compared to the LDAS (571 fg/mL, IQR 57-1,310 fg/mL, p = 0.04) and remission sub-groups (271 fg/mL, IQR 3-56, p < 0.001). IFN-α2 was higher in all JSLE patients (median 587 fg/mL, IQR 11-2,774) as compared to JIA patients (median 7 fg/mL, IQR 3-236, p = 0.0017) and HCs (p = 0.017). JSLE patients in remission or LDAS with abnormal IFN-α2 levels had a shorter time to flare over the subsequent six months compared to those with normal IFN-α2 levels (p = 0.022). Longitudinally, multivariable analysis demonstrated high IFN-α2 to be the only predictor of an ongoing flare (p = 0.028). Serum IFN-α2 levels associate with disease activity and can predict ongoing and future flares in jSLE. These findings suggest that quantification of IFN-α2 may support risk stratification and disease monitoring in these patients.

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  • Rheumatology (Oxford, England)
  • Nov 26, 2024
  • Valentina Natoli + 7
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Recurring tidal disruption events a decade apart in IRAS F01004-2237

In theory, recurring tidal disruption events (TDEs) may occur when a close stellar binary encounters a supermassive black hole, if one star is captured and undergoes repeating partial TDEs, or if both stars are tidally disrupted (double TDEs). In addition, independent TDEs may be observed over decades in some special galaxies where the TDE rate is extremely high. Exploring the diversity of recurring TDEs and probing their natures with rich observational data helps us to understand these mechanisms. We report the discovery of a second optical flare that occurred in September 2021 in IRAS F01004-2237, where a first flare that occurred in 2010 had already been reported. We also present a detailed analysis of multi-band data. We aim to understand the nature of the flare and explore the possible causes of the recurring flares. We describe our analysis of the position of the flare, the multi-band light curves (LCs), the optical and ultraviolet (UV) spectra, and the X-ray LC and spectra. The position of the flare coincides with the galaxy centre with a precision of 650 pc. The flare peaks in $ days with an absolute magnitude of $ and fades in two years, roughly following $L $. It maintains a nearly constant blackbody temperature of sim 22,000 K in later stages. Its optical and UV spectra show hydrogen and helium broad emission lines with full width at half maxima of 7,000--21,000 km s$^ $ and a He II/Halpha ratio of 0.3--2.3. It shows weak X-ray emission relative to UV emission, with X-ray flares lasting for $&lt;2-3$ weeks, during which the spectrum is soft with a power-law index of $ $. These characters are consistent with a TDE, ruling out the possibilities of a supernova or an active galactic nucleus flare. With a TDE model, we infer a peak UV luminosity of $3.3 $ erg s$^ $ and an energy budget of $4.5 $ erg. A TDE caused the flare that occurred in 2021. The two optical flares separated by $10.3 years can be interpreted as repeating partial TDEs, double TDEs, or two independent TDEs. Although no definitive conclusion can be drawn, the partial TDEs interpretation predicts a third flare around 2033, and the independent TDEs interpretation predicts a high TDE rate of $ $ yr$^ $ in F01004-2237, both of which can be tested by future observations.

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  • Astronomy &amp; Astrophysics
  • Nov 20, 2024
  • Luming Sun + 18
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Swift Observations of Mrk 421 in Selected Epochs. IV. Physical Implications of X-Ray Flaring Activity and Features of Relativistic Magnetic Reconnection in 2018 April–2023 December

We present the spectral and timing results obtained during the intense observations of Mrk 421 by the Swift-based ultraviolet to X-ray instruments during 2018 April–2023 December. The source showed various strengths of X-ray flaring activity, exceeding a level of 3.5 × 10−9 erg cm−2 s−1 during the strongest 0.3–10 keV flares. Our study identifies a number of intraday brightness variability, including 61 instances that occurred within 1 ks exposures that are consistent with the shock-in-jet scenario and accompanied by significant, fast spectral changes. The source exhibited extreme spectral properties with dominance of the log-parabolic distributions of photons with energy and the frequent occurrence of hard photon indices in the 0.3–10 keV and 0.3–300 GeV bands, with the peak of synchrotron spectral energy distribution E p detected at the energies beyond 29 keV for the first time. The source showed very fast transitions of log-parabolic-to-power-law spectra, most plausibly caused by turbulence-driven relativistic magnetic reconnection. Our spectral results also demonstrate the importance of the first-order Fermi mechanism within the magnetic field of different confinement efficiencies, stochastic acceleration, transitions in the turbulence spectrum, and hadronic cascades. The X-ray, UV, and γ-ray fluxes showed a lognormal variability, which hints at the imprint of accretion disk instabilities on the blazar jet, as well as the possible presence of hadronic cascades. The UV and γ-ray variabilities demonstrated weak correlations with the X-ray flaring activity, which is not consistent with simple synchrotron self-Compton models and requires more complex particle acceleration and emission scenarios.

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  • The Astrophysical Journal Supplement Series
  • Nov 12, 2024
  • B Kapanadze + 2
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Searching for Stellar Activity Cycles Using Flares: The Short- and Long-timescale Activity Variations of TIC-272272592

We examine 4 yr of Kepler 30 minutes data, and five sectors of Transiting Exoplanet Survey Satellite 2 minutes data for the dM3 star KIC-8507979/TIC-272272592. This rapidly rotating (P = 1.2 day) star has previously been identified as flare active, with a possible long-term decline in its flare output. Such slow changes in surface magnetic activity are potential indicators of solar-like activity cycles, which can yield important information about the structure of the stellar dynamo. We find that while TIC-272272592 shows evidence for both short- and long-timescale variations in its flare activity, it is unlikely physically motivated. Only a handful of stars have been subjected to such long-baseline point-in-time flare studies, and we urge caution in comparing results between telescopes due to differences in bandpass, signal-to-noise ratio, and cadence. In this work, we develop an approach to measure variations in the flare frequency distributions over time, which is quantified as a function of the observing baseline. For TIC-272272592, we find a 2.7σ detection of a sector which has a flare deficit, therefore indicating the short-term variation could be a result of sampling statistics. This quantifiable approach to describing flare-rate variation is a powerful new method for measuring the months-to-years changes in surface magnetic activity, and provides important constraints on activity cycles and dynamo models for low-mass stars.

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  • The Astronomical Journal
  • Nov 1, 2024
  • Tobin M Wainer + 4
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Solar active region evolution and imminent flaring activity through color-coded visualization of photospheric vector magnetograms

Context. The emergence of magnetic flux, its transition to complex configurations, and the pre-eruptive state of active regions are probed using photospheric magnetograms. Aims. Our aim is to pinpoint different evolutionary stages in emerging active regions, explore their differences, and produce parameters that could advance flare prediction using color-coded maps of the photospheric magnetic field. Methods. The three components of the photospheric magnetic field vector are combined to create color-combined magnetograms (COCOMAGs). From these, the areas occupied by different color hues are extracted, creating appropriate time series (color curves). These COCOMAGs and color curves are used as proxies of the active region evolution and its complexity. Results. The morphology of COCOMAGs showcases typical features of active regions, such as sunspots, plages, and sheared polarity inversion lines. The color curves represent the area occupied by photospheric magnetic field of different orientation and contain information pertaining to the evolutionary stages of active regions. During emergence, most of the region area is dominated by horizontal or highly inclined magnetic field, which is gradually replaced by more vertical magnetic field. In complex regions, large parts are covered by highly inclined magnetic fields, appearing as abrupt color changes in COCOMAGs. The decay of a region is signified by a domination of vertical magnetic field, indicating a gradual relaxation of the magnetic field configuration. The color curves exhibit a varying degree of correlation with active region complexity. Particularly the red and magenta color curves, which represent strong, purely horizontal magnetic field, are good indicators of future flaring activity. Conclusions. Color-combined magnetograms facilitate a comprehensive view of the evolution of active regions and their complexity. They offer a framework for the treatment of complex observations and can be used in pattern recognition, feature extraction, and flare-prediction schemes.

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  • Astronomy &amp; Astrophysics
  • Nov 1, 2024
  • I Kontogiannis + 5
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Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis

A rich spectrum of molecular hydrogen (H2) emission lines is seen in sensitive observations from the far-ultraviolet (FUV) channels of the Interface Region Imaging Spectrograph (IRIS) during flare activity in solar active region NOAA Active Region 11861. Based on this observation, we have determined 37 new line identifications by comparing synthetic spectra produced using 1D modeling of H2 fluorescence. To avoid misidentification of the H2 lines, we have also compiled a complete list of atomic line identifications for the IRIS FUV bandpasses from previous work. We carry out analysis of the spatially resolved H2 emission that occurs during the flares and find the following: (1) in spatially resolved observations the H2 line ratios may show optically thick line formation, contrary to previous results; (2) comparison of the spatial distribution of H2 Doppler velocities with those measured from other species reveals that H2 remote sensing probes an intermediate depth in the atmosphere between the photosphere and chromosphere, consistent with expectations from modeling; (3) the relationship between H2 line intensity and the observed intensity of its exciter is related to the atmospheric stratification; however, (4) H2 fluorescence can sometimes occur in response to radiation from distant sources many megameters away across the solar surface.

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  • The Astrophysical Journal
  • Nov 1, 2024
  • Sarah A Jaeggli + 1
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The Role of Magnetic Skeleton in Solar Flare Filaments Activity

We report an M9.3 flare and filaments activities from NOAA Active Region 11261 that are strongly modulated by the 3D magnetic skeleton. Magnetic field extrapolation from the vector magnetic field suggests complex magnetic connectivity and the existence of a high coronal null point southeast of the active region. A small filament over the inversed V-shaped polarity inversion line erupted and resulted in the M9.3 flare associated with a weak ejection in the EUV hot channel and the formation of a relatively large filament. Both the weak ejection and the eruption of the large filament were toward the southeast. Comparative analyses have disclosed the following new facts. First, the trajectory of looptop hard X-ray emission provides solid evidence that the magnetic reconnection site propagated up toward the coronal null point as the flare and filaments erupted. Second, the EVU observations show coronal mass ejection-like eruption features in the ejection region of the magnetic skeleton. Third, the closed fan confined the west end of the large filament and the corresponding flare ribbons. We demonstrate a spatiotemporal relationship between the magnetic skeleton and the flare filament activity. We conclude that the magnetic skeleton can modulate and determine almost all the characteristics of the studied activity in the corresponding scale.

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  • The Astrophysical Journal
  • Nov 1, 2024
  • Juan Guo + 9
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Lupus nephritis: redefining the treatment goals

The course of proliferative lupus nephritis (LN) is characterized by flares of activity alternating with periods of quiescence, against a background of chronic immune dysregulation. An accurate assessment of disease activity is of unassailable importance to tailor therapy. In the present communication, we discuss the available clinical, serological and histological tools to evaluate disease activity and how they may be applied to redefine the treatment goals in LN. Traditionally, treatment response is judged by the degree of proteinuria reduction and improvement of kidney function, but this fails to differentiate ongoing inflammatory disease from chronic damage. Despite intensive research, no novel biomarker has proved useful for clinical practice, and we continue to rely on anti-double-stranded DNA antibody levels (anti-dsDNA) to assess serological activity. Repeat kidney biopsies sometimes reveal persistent inflammation despite apparent clinical remission, giving credibility to the conviction that histological remission should be a treatment goal and protocol biopsies part of the decision-making process. However, the discrepancies between clinical and histological responses to therapy can be explained by persistent systemic autoimmunity with low-grade immune complex deposition or, alternatively, by delayed clearance of intrarenal inflammation once immunological remission has been achieved. Since persistent immune dysregulation is the motor of disease activity in LN, it should be the principal focus of therapy and monitoring. We propose to replace the traditional induction-remission maintenance protocol by a more dynamic and individualized approach, and aim for 3 treatment goals, concomitantly rather than sequentially: 1) Clinical remission, by attenuating renal inflammation, using microscopic hematuria, proteinuria, eGFR and complement levels as biomarkers; 2) Immunological remission, by decreasing immune complex generation, using anti-dsDNA as biomarker; 3) Preservation of kidney function, by curtailing chronic kidney damage, using eGFR slope as biomarker.

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  • Kidney International
  • Nov 1, 2024
  • An S De Vriese + 2
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Hot spots around Sagittarius A*

Context. Observations of Sagittarius A* (Sgr A*) in the near-infrared (NIR) show irregular flaring activity. Flares coincide with the astrometric rotation of the brightness centroid and with looping patterns in fractional linear polarization. These signatures can be explained with a model of a bright hot spot, transiently orbiting the black hole. Aims. We extend the capabilities of the existing algorithms to perform parameter estimation and model comparison in the Bayesian framework using NIR observations from the GRAVITY instrument, and simultaneously fitting the astrometric and polarimetric data. Methods. Using the numerical radiative transfer code ipole, we defined several geometric models describing a hot spot orbiting Sgr A*, threaded with a magnetic field, and emitting synchrotron radiation. We then explored the posterior space of our models with a nested sampling code dynesty. We used Bayesian evidence to make comparisons between the models. Results. We have used 11 models to sharpen our understanding of the importance of various aspects of the orbital model, such as non-Keplerian motion, hot-spot size, and off-equatorial orbit. All considered models converge to realizations that fit the data well, but the equatorial super-Keplerian model is favoured by the currently available NIR dataset. Conclusions. We have inferred an inclination of ∼155 deg, which corroborates previous estimates, a preferred period of ∼70 minutes, and an orbital radius of ∼12 gravitational radii with the orbital velocity of ∼1.3 times the Keplerian value. A hot spot with a diameter smaller than 5 gravitational radii is favoured. Black hole spin is not constrained well.

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  • Astronomy &amp; Astrophysics
  • Nov 1, 2024
  • A.I Yfantis + 4
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Magnetic Field Evolution of the Solar Active Region 13664

On 2024 May 10–11, the strongest geomagnetic storm since 2003 November occurred, with a peak Dst index of −412 nT. The storm was caused by NOAA active region (AR) 13664, which was the source of a large number of coronal mass ejections and flares, including 12 X-class flares. Starting from about May 7, AR 13664 showed a steep increase in its size and (free) magnetic energy, along with increased flare activity. In this study, we perform 3D magnetic field extrapolations with the NF2 nonlinear force-free code based on physics-informed neural networks (R. Jarolim et al.). In addition, we introduce the computation of the vector potential to achieve divergence-free solutions. We extrapolate vector magnetograms from the Solar Dynamics Observatory’s Helioseismic and Magnetic Imager at the full 12 minute cadence from 2024 May 5 00:00 to 11 04:36 UT, in order to understand the AR’s magnetic evolution and the large eruptions it produced. A decrease in the calculated relative free magnetic energy can be related to solar flares in ∼90% of the cases, and all considered X-class flares are reflected by a decrease in the relative free magnetic energy. Regions of enhanced free magnetic energy and depleted magnetic energy between the start and end times of major X-class flares show spatial alignment with brightness increases in extreme-ultraviolet observations. We provide a detailed analysis of the X3.9-class flare on May 10, where we show that the interaction between separated magnetic domains is directly linked to major flaring events. With this study, we provide a comprehensive data set of the magnetic evolution of AR 13664 and make it publicly available for further analysis.

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  • The Astrophysical Journal Letters
  • Nov 1, 2024
  • Robert Jarolim + 4
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P45 Lupus flare with myositis: an atypical presentation in the absence of elevated creatine kinase

Abstract Introduction Systemic lupus erythematosus (SLE) is a multi-systemic disease, but the coexistence of inflammatory myositis in SLE has not been extensively studied. Myositis, a rare complication, is typically associated with elevated creatine kinase (CK) levels. We report a case of SLE presenting with a lupus flare and an atypical manifestation of myositis, confirmed by MRI despite low CK levels. This case underscores the complex nature of lupus flares and the challenges in diagnosing and managing such atypical presentations. The diagnostic dilemma of myositis with low CK levels adds a layer of complexity to understanding and treating SLE-related complication. Case description A 25-year-old lady, known patient of systemic lupus erythematosus (SLE), positive ANA, dsDNA, and anti-Ro antibodies, managed with hydroxychloroquine, experienced generalized body stiffness, aches, and lower limb weakness for the past 3 months. She was admitted with worsening lower limb pain and weakness, oral ulcers, arthralgias, myalgias and alopecia despite intramuscular steroids. On examination, her lower limb power was reduced to 3/5 with normal sensation. A detailed neurological assessment was difficult due to severe pain. Her chest was clear with normal heart sounds, and the rest of the examination was unremarkable. Her erythrocyte sedimentation rate (ESR) was 69 mm/hr, and her C-reactive protein (CRP) was 50 mg/L, with a normal white cell count and normal kidney and liver function. Her urine protein-creatinine ratio (PCR) was 50.9 mg/mmol. An ECG and chest X-ray were unremarkable. Initially, she was treated for a urinary tract infection (UTI) due to urinary symptoms, and further investigations were done to check for myositis and a lupus flare. Her CK was low at 36 U/L, with normal lactate dehydrogenase (LDH). Her complement levels were low with raised anti-dsDNA levels. An MRI of the spine was normal. Given the history and clinical signs suggestive of myositis, an MRI of the hip was performed, revealing active myositis. She was started on IV methylprednisolone for the active flare. A renal opinion was sought due to the positive urine PCR, and they advised a possible biopsy. However, her repeat urine PCR came back negative, and the renal team concluded that the abnormal result was likely secondary to the UTI, negating the need for a biopsy. Her condition and muscle power improved (4+/5) with steroid and mycophenolate mofetil. Upon tapering the steroid to 10 mg, her arthralgia recurred, but myositis was improving. Further follow-up has been arranged. Discussion This case highlights the complex nature of systemic lupus erythematosus (SLE) and the challenges in managing its multi-systemic manifestations. The patient’s presentation with generalized body stiffness, lower limb weakness, and pain, alongside oral ulcers, arthralgias, myalgias, and alopecia, exemplifies the diverse clinical spectrum of SLE. The initial differential diagnosis included a lupus flare and myositis. The elevated ESR and CRP levels, alongside low complement levels and increased anti-dsDNA titres, were indicative of active disease. Interestingly, the patient’s CK levels were low, which devi-ates from the typical presentation of myositis. Moreover, specific myositis antibodies were absent. Despite low CK, the clinical suspicion of myositis prompted an MRI scan of thigs, which confirmed active inflammation in the hip muscles. Another important aspect of this case was the initial positive urine PCR, which raised concerns about renal involvement—a serious complication of SLE. However, the resolution of this abnormality upon treating a concurrent UTI highlights the importance of re-evaluating initial findings and considering alternative explanations before proceeding with invasive procedures such as a renal biopsy. In summary, this case tells us the importance of a comprehensive and dynamic approach in the management of SLE. It illustrates the need for continuous monitoring, the utility of advanced imaging techniques in diagnosing myositis, and the cautious interpretation of laboratory results in the context of coexisting conditions. The patient’s favorable response to treatment also emphasizes the efficacy of current therapeutic strategies in controlling disease activity and preventing long-term complications Key learning points • Lupus flares can present with a wide range of symptoms, including musculoskeletal manifestations such as myositis. • The absence of typical markers, such as elevated CK and specific antibodies, should not rule out the possibility of myositis in lupus patients. • Prompt recognition and management of myositis in lupus flares are crucial to prevent further complications and improve patient outcomes. • Effective management of SLE often requires collaboration among various specialists. In this case, the involvement of the renal team was crucial for further evaluation and management, demonstrating the value of a coordinated care approach. In conclusion, this case highlights the complexity of lupus flares and the importance of considering myositis as a potential complication, even in the absence of typical markers. Early recognition and appropriate management are key to improving outcomes for patients with lupus-associated myositis.

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  • Rheumatology Advances in Practice
  • Nov 1, 2024
  • Shumaila Baloch + 1
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Variations of flare energy release behaviour and magnetic loop characteristics versus absolute stellar parameters

ABSTRACT In this paper, we examine how stellar flare activity varies with evolution stage, rotation period, and spectral type. To do this, we examine the distributions of the flare equivalent duration on a logarithmic scale, which we consider as an indicator of the maximum energy level that a star can reach in white-light flares. We conduct these analyses using two distinct statistical models of data obtained from white-light flare patrols of 33 stars. These models are the one-phase exponential association (OPEA) and cumulative flare frequency models. The results show that the value of the OPEA model parameter Plateau has a linear relationship with the stellar B – V colour index and the rotation period. In addition, it is shown that flare time-scales, and therefore the maximum magnetic loop height that stars can have, vary according to the evolutionary stage of the star. Finally, it is concluded that the cumulative flare frequency parameters of the stars are not as effective as the OPEA parameters at exhibiting these variations.

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  • Monthly Notices of the Royal Astronomical Society
  • Oct 25, 2024
  • E Yoldaş + 1
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Global and local dynamics of X-flare-producing active regions during solar cycle 25 peak phase

Context. The configuration of the longitudinally elongated region that active regions (ARs) cluster around, known as a toroid belt, has been shown to be an indicator of intense activity. In particular, complex ARs at locations in the north and/or south toroids tend to appear “tipped-away” with respect to each other. On the other hand, magnetic helicity has been used as an indicator of flare activity in ARs. Aims. As solar cycle (SC) 25 approaches its peak, a number of significant (X-class) flares have been produced. Here, we investigate the circumstances surrounding two of the most flare-prolific ARs of solar cycle 25, namely, ARs 13590 and 13514. Two aspects of the evolution of these ARs are investigated in this work: the global-scale magnetic toroid configuration and small-scale magnetic field morphology and topology – before, during, and after the onset of major flares. Methods. We studied the global morphology of the solar magnetic fields near intense flares in terms of the spatial distribution of ARs on magnetic fields synoptic maps. On AR scales, we analyzed the magnetic helicity accumulation, as well as its current-carrying and potential components. Results. Our results are consistent with major flare-prolific ARs from solar cycles 23 and 24. In particular, we observe a consistent dominance of current-carrying magnetic helicity at the time of major flares. The evolution of global magnetic toroids, indicating the occurrence of flare-prolific ARs in the tipped-away portion of the toroid, together with the local dynamics of complex ARs, could offer a few weeks of lead time to prepare for upcoming space weather hazards.

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  • Astronomy &amp; Astrophysics
  • Oct 25, 2024
  • B Raphaldini + 5
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Are There Local Dynamos Acting in Sunspot Regions?

In solar physics, a long-unanswered question is whether or not there are local dynamos acting in sunspot regions. Here we report an observed pattern of magnetic evolution that makes the sunspots alive with ample complexity and energy. This anomalous pattern manifests as peculiar bipolar magnetic emergences (BMEs), exhibiting the following characteristics: (1) the BMEs persistently appear beyond the penumbra, encircling the sunspot in an end-to-end configuration; (2) each BME gradually grows and separates its two polarities along an arc trajectory centered on the sunspot; (3) a circular brightening belt is manifested in the ultraviolet/extreme-ultraviolet radiations during the BMEs’ evolution; and (4) the sunspot regions with such an evolution pattern often exhibit vigorous solar activity, such as homogeneous major flares. The magnetic evolving pattern and relevant flare activity indicate the presence of a local dynamo, and we characterize it as a twisting-reconnecting dynamo.

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  • The Astrophysical Journal
  • Oct 24, 2024
  • Chunlan Jin + 3
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Association between depression and anxiety with the risk and flare of inflammatory bowel disease: a systematic review and meta-analysis.

Inflammatory bowel disease (IBD) is a chronic condition characterized by inflammation in the gastrointestinal tract. Previous studies have suggested a potential association between mental disorders, such as depression and anxiety, and the risk and flare of IBD. However, the findings have been inconsistent. This study aimed to conduct a systematic review and meta-analysis to assess the relationship between mental disorders and IBD. A comprehensive literature search was performed to identify relevant studies. Pooled odds ratios (ORs) and 95% confidence intervals (CIs) were calculated to determine the association between mental disorders and the risk and flare of IBD. Heterogeneity between studies was assessed using the I2 statistic. Sensitivity analysis was conducted to evaluate the stability of the results. A total of seven studies met the inclusion criteria and were included in the meta-analysis. The pooled results demonstrated a significant association between symptoms of depression at baseline and an increased risk of disease activity flare during longitudinal follow-up, with an OR of 1.69 (95% CI 1.34, 2.13). However, there was high heterogeneity between studies (I2 = 82%). Furthermore, patients who underwent surgery had a higher risk of disease activity flare (OR: 1.49, 95% CI 1.13, 1.95), and hospitalization was also identified as a contributing factor (OR: 1.22, 95% CI 1.10, 1.36). This meta-analysis provides evidence for a significant association between symptoms of depression and the risk of disease activity flare in IBD. However, the high heterogeneity observed between studies suggests the need for further research to explore potential moderators and underlying mechanisms. These findings highlight the importance of addressing mental health in the management and treatment of patients with IBD.

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  • Internal and emergency medicine
  • Oct 3, 2024
  • Guowei Gong + 3
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Separating states in astronomical sources using hidden Markov models: with a case study of flaring and quiescence on EV Lac

ABSTRACT We present a new method to distinguish between different states (e.g. high and low, quiescent and flaring) in astronomical sources with count data. The method models the underlying physical process as latent variables following a continuous-space Markov chain that determines the expected Poisson counts in observed light curves in multiple passbands. For the underlying state process, we consider several autoregressive processes, yielding continuous-space hidden Markov models of varying complexity. Under these models, we can infer the state that the object is in at any given time. The continuous state predictions from these models are then dichotomized with the help of a finite mixture model to produce state classifications. We apply these techniques to X-ray data from the active dMe flare star EV Lac, splitting the data into quiescent and flaring states. We find that a first-order vector autoregressive process efficiently separates flaring from quiescence: flaring occurs over 30 per cent–40 per cent of the observation durations, a well-defined persistent quiescent state can be identified, and the flaring state is characterized by higher plasma temperatures and emission measures.

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  • Monthly Notices of the Royal Astronomical Society
  • Sep 9, 2024
  • Robert Zimmerman + 3
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Quantifying the High Early Solar Cosmic-Ray Flux with Cosmogenic Neon Isotopes in Refractory Minerals

An enhancement in the activity of the early young Sun resulting in a high charged particle flux has been invoked to explain excesses in spallation-induced nuclides in primitive planetary materials. Astronomical observations of energetic outbursts of young stellar objects (YSOs) also support the idea of an active young Sun. However, the early solar cosmic-ray (SCR) flux has not been well constrained. Here we use measured concentrations of SCR-produced nuclides that formed and are preserved in meteoritical hibonite and spinel, some of the solar system’s oldest solids, and physical models for dust transport in the early protoplanetary disk to determine the magnitude of the early SCR flux. We focus our attention on cosmogenic neon, which cannot have been inherited from precursors and can only be produced in situ in solids. Our modeled effective exposure time to SCRs for these solids is very short, on the order of years. This indicates that the young Sun’s SCR flux recorded in refractory mineral hibonite was up to ∼7 orders of magnitude higher than the contemporary level. Our flux estimate is consistent with the >105× enhanced flux inferred from astronomical observations of greatly enhanced flare activities of YSOs.

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  • The Astrophysical Journal
  • Sep 1, 2024
  • Xin Yang + 2
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Time Series of Magnetic Field Parameters of Merged MDI and HMI Space-weather Active Region Patches as Potential Tool for Solar Flare Forecasting

Solar flare prediction studies have been recently conducted with the use of Space-Weather MDI (Michelson Doppler Imager on board Solar and Heliospheric Observatory) Active Region Patches (SMARPs) and Space-Weather HMI (Helioseismic and Magnetic Imager on board Solar Dynamics Observatory) Active Region Patches (SHARPs), which are two currently available data products containing magnetic field characteristics of solar active regions (ARs). The present work is an effort to combine them into one data product, and perform some initial statistical analyses in order to further expand their application in space-weather forecasting. The combined data are derived by filtering, rescaling, and merging the SMARP and SHARP parameters, which can then be spatially reduced to create uniform multivariate time series. The resulting combined MDI–HMI data set currently spans the period between 1996 April 4 and 2022 December 13, and may be extended to a more recent date. This provides an opportunity to correlate and compare it with other space-weather time series, such as the daily solar flare index or the statistical properties of the soft X-ray flux measured by the Geostationary Operational Environmental Satellites. Time-lagged cross correlation indicates that a relationship may exist, where some magnetic field properties of ARs lead the flare index in time. Applying the rolling-window technique makes it possible to see how this leader–follower dynamic varies with time. Preliminary results indicate that areas of high correlation generally correspond to increased flare activity during the peak solar cycle.

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  • The Astrophysical Journal
  • Sep 1, 2024
  • Paul A Kosovich + 10
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Proton Fluxes of Solar-Type Stars with Planetary Systems

Abstract The previously developed method for estimating of the parameters of proton fluxes from flare energies for the Sun has been applied to data on the flare activity of solar-type stars. The obtained results will be used to estimate the radiation situation in a stellar system containing exoplanets. In our analysis, we have used catalog data on flares of solar-type stars obtained from observations with Kepler telescope. The empirical relations between the energy of X-ray flares and the proton flux for the Sun have been extended to the case of stellar flares, similar to what has been done previously in the case of coronal mass ejections (CMEs). The used method has had limitations caused by the extension of the solar analogy to other stars as well as the uncertainties that have arisen when applying scaling methods. It has been found that the characteristic values of the proton flux for solar-type stars can be one order of magnitude higher than the estimates for the Sun. Prospects for the development of alternative methods for estimating proton fluxes in the vicinity of stars of late spectral types have been discussed (for example, by studying the behavior of Si IV and He II emission lines in the far ultraviolet range).

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  • Astronomy Reports
  • Sep 1, 2024
  • I S Savanov
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