A Near-half-century Simulation of the Solar Corona by Valentin Aslanyan, Karen A. Meyer, Roger B. Scott, Anthony R. Yeates

“…The simulation self-consistently reproduces decades of solar phenomena, varying in duration between rapid eruptions and the long-term solar cycles, from an input of observed active regions emerging at the photosphere. We have developed a geometric approach to use magnetic helicity to identify and localize the frequent eruptions that occur in the simulation. …”
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Optical Appearance of Eccentric Tidal Disruption Events by Fangyi (Fitz) Hu, Daniel J. Price, Ilya Mandel

“…Assuming electron scattering opacity, this material would be visible as a ∼100 au photosphere at ∼10 ^4 K, in line with observations of candidate TDEs.…”
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Accretion shock stability on a dynamically heated YSO atmosphere with radiative transfer by de Sá Lionel, Chièze Jean-Pierre, Stehlé Chantal, Matsakos Titos, Ibgui Laurent, Lanz Thierry, Hubeny Ivan

“…Theory and simulations predict Quasi-Periodic Oscillations of shocks which develop in magnetically driven accretion funnels connecting the stellar disc to the photosphere of Young Stellar Objects (YSO). X-ray observations however do not show evidence of the expected periodicity. …”
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Study on the relation of the solar coronal rotation with magnetic field structures by N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, S. Zheng

“…Furthermore, this study presents an explanation for the inconsistent results for the coronal rotation issue among the previous studies, and also reveals the reason why the coronal atmosphere rotates faster than the lower photosphere.…”
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Studying the relationship of localization parameters of solar sources of magnetic clouds with their characteristics and substorm activity by Barkhatov N.A., Revunova E.A., Romanov R.V., Barkhatova O.M., Revunov S.E.

“…We propose a method for determining location and orientation of extended solar sources of magnetic clouds, using coronagraph data and SOHO EIT/MDI images of the photosphere. To estimate the probability of formation of magnetic clouds, we use a simple cylindrical force-free model. …”
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Magnetic Fields in the Solar Convection Zone by Fan Yuhong

“…Thus the magnetic fields need to traverse the entire convection zone before they reach the photosphere to form the observed solar active regions. …”
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The Evolution of Research on Abundances of Solar Energetic Particles by Donald V. Reames

“…On average, gradual SEP events give us a measure of element abundances in the solar corona, which differ from those in the photosphere as a classic function of the first ionization potential (FIP) of the elements, distinguishing ions and neutrals. …”
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GRB 220304A: Another Gamma-Ray Burst Dominated by Thermal Radiation by Jia-Ming Chen, Zhao-Yang Peng

“…It is reminiscent of GRB 090902B, a special GRB with photosphere radiation characteristics. Then, we perform spectral analysis using the Planck function (blackbody, BB) and the multicolor BB model. …”
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Solar Flares: Magnetohydrodynamic Processes by Kazunari Shibata, Tetsuya Magara

“…The evolution toward the onset of a flare is rather quasi-static when free energy is accumulated in the form of coronal electric current (field-aligned current, more precisely), while the dissipation of coronal current proceeds rapidly, producing various dynamic events that affect lower atmospheres such as the chromosphere and photosphere. Flares manifest such rapid dissipation of coronal current, and their theoretical modeling has been developed in accordance with observations, in which numerical simulations proved to be a strong tool reproducing the time-dependent, nonlinear evolution of a flare. …”
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Causal relationships between eruptive prominences and coronal mass ejections by B. Filippov, S. Koutchmy

“…A twisted flux rope is held by the tension of field lines of photospheric sources until parameters of the system reach critical values and a catastrophe happens. …”
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Transitions in the cloud composition of hot Jupiters by Parmentier, V, Fortney, JJ, Showman, AP, Morley, CV, Marley, MS

“…The cold trapping of cloud species below the photosphere naturally produces such a transition and predicts similar transitions for other condensates, including TiO. …”

On the tidal interaction of a solar-type star with an orbiting companion: Excitation of g mode oscillation and orbital evolution by Terquem, C, Papaloizou, J, Nelson, R, Lin, D

“…We compute the torque exerted on the star by a companion in circular orbit, and determine the potentially observable magnitude of the tidally induced velocity at the stellar photosphere. These calculations are compared with the results obtained by assuming that a very small frequency limit can be taken in order to calculate the tidal response (equilibrium tide). …”

Weak seasonality on temperate exoplanets around low-mass stars by Tan, X

“…At the infrared emission level in the photosphere, the relative amplitudes of thermal flux and temperature perturbations are negligible, and their phase lags are closed to −90° for Jupiter-like planets around very low mass stars. …”

Pulsation-induced Spectroscopic Variability of IRAS Z02229+6208 by Laimons Začs, Kārlis Puķı̄tis

“…Strong and broad CN red system lines, blueshifted up to 9.4 km s ^−1 relative to the stellar photosphere, are seen near the light minimum. Near the light maxima, the molecular features are weak and most of them are in emission, e.g., broad emissions in the CN red system (0,0) lines are seen. …”
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Model Constraints Based on the IceCube Neutrino Nondetection of GRB 221009A by Shunke Ai, He Gao

“…We find that, at least for this specific burst, the dissipative photosphere model could be ruled out in a large parameter space. …”
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Processes and mechanisms governing the initiation and propagation of CMEs by B. Vršnak

“…Special attention is paid to 3-dimensional (3-D) topology of the magnetic field structures, particularly to aspects related to the concept of semi-toroidal flux-rope anchored at both ends in the dense photosphere and embedded in the coronal magnetic arcade. …”
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Episodes of Molecular Emission in the Optical Spectrum of IRAS 22272+5435 by Kārlis Puķı̄tis, Laimons Začs, Julius Sperauskas

“…It is proposed that the observed emissions originate within few stellar radii above the photosphere.…”
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Coronal Field Geometry and Solar Wind Speed by Ivan Berezin, Andrey Tlatov

“…The second input parameter for the WSA model is the great circle distance from the base of the open magnetic field line in the photosphere to the boundary of the corresponding coronal hole (DCHB). …”
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Comparing results of real-scale time MHD modeling with observational data for first flare M 1.9 in AR 10365 by Borisenko Alexey Vasilevich, Podgorny Igor Maksimovich, Podgorny Alexander Igorevich

“…However, apparently due to small disturbance, propagating from the photosphere, sufficient magnetic energy was not accumulated in this configuration, so the NoRH does not show the flare source of emission at the frequency 17 GHz in the place, where this singular line is situated.…”
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Synoptic solar observations of the Solar Flare Telescope focusing on space weather by Hanaoka Yoichiro, Sakurai Takashi, Otsuji Ken’ichi, Suzuki Isao, Morita Satoshi

“…Data for the brightness, Doppler signal, and magnetic field information of the photosphere and the chromosphere are obtained. In addition to monitoring dynamic phenomena like flares and filament eruptions, we can track the evolution of the magnetic fields that drive them on the basis of these data. …”
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