Results 41 to 50 of about 528 (133)
Reconstructing Historical Solar Indices for Predicting Past Space Weather Events
Space Weather, Volume 24, Issue 4, April 2026.Abstract Modeling and forecasting the near‐Earth space environment, specifically the thermosphere, is particularly important because it affects the motion of low‐Earth orbit objects through atmospheric drag. Solar indices such as F10.7, S10.7, M10.7, and Y10.7 are commonly used as inputs to ionospheric and thermospheric density models.
Poshan Belbase +4 more
wiley +1 more source
Photospheric Magnetic Field of the Sun: Two Patterns of the Longitudinal Distribution
Solar Physics, 2007 14 pages, 5 figures, 1 table; submitted to Solar Physics; 2 figures ...
Vernova, E. S. +2 more
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Mapping the Sun's upper photosphere with artificial neural networks
, 2021 We have developed an inversion procedure designed for high-resolution solar spectro-polarimeters, such as Hinode/SP or DKIST/ViSP. The procedure is based on artificial neural networks trained with profiles generated from random atmospheric stratifications for a high generalization capability. When applied to Hinode data we find a hot fine-scale network
Socas-Navarro, Hector +1 more
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Post‐Processing Probabilistic Forecasts of the Solar Wind by Data Mining Similar Scenarios
Space Weather, Volume 24, Issue 4, April 2026.Abstract The solar wind speed at Earth is one of the most important parameters regarding the effects of space weather on society. Thus far, most approaches for predicting the solar wind speed produce a single‐value time series without uncertainty, or utilize ensemble methods which require custom calibration development.
Daniel E. da Silva +3 more
wiley +1 more source
Searching for Rotational X‐Ray Modulation on TIC 277539431
Astronomische Nachrichten, Volume 347, Issue 3, March 2026.ABSTRACT TIC 277539431, a fast rotating M7 dwarf, was detected to host the highest latitude flare to date at 81°$$ {81}^{{}^{\circ}} $$. Magnetic activity like stellar flares occurring at high latitude indicate occurrence of coronal loops at these latitudes on fully‐convective M dwarfs. In contrast, sunspots usually occur below 30°$$ {30}^{{}^{\circ}} $
Desmond Dsouza +2 more
wiley +1 more source
Statistical equilibrium and photospheric abundance of silicon in the Sun and in Vega [PDF]
Astronomy & Astrophysics, 2001 Based on detailed non-LTE calculations, an updated determination of the abundance of silicon in the Sun and Vega is presented. The model atom includes neutral and singly ionized stages of silicon with 115 energy levels and 84 line transitions. Non-LTE eects are found to be quite small in the Sun.
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FLOWS OF MAGNETIC FIELD IN THE SUN’S PHOTOSPHERE
Proceedings of the 25th All-Russia Conference on Solar and Solar-Terrestrial Physics, 2021 E.S. Vernova, M.I. Tyasto, D.G. Baranov
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On the differences between plage and quiet sun in the solar photosphere
The Astrophysical Journal, 1992 Time sequences of interleaved observations of the continuum intensity, longitudinal magnetic field, vertical velocity in the midphotosphere, and the line-center intensity in Ni I 6768 A were obtained in an active-region plage and the surrounding relatively field-free area near disk center. Spacetime Fourier filtering techniques are used to separate the
Alan M. Title +5 more
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88th Annual Meeting of the Meteoritical Society 2026: Abstracts
Meteoritics &Planetary Science, Volume 61, Issue S1, Page S48-S551, August 2026.
wiley +1 more source
Тhе telescope for observation of the photosphere of the Sun [PDF]
Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, 2015 V. Efimenko, S. Kaminsky
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