SMALL SOLAR FLARES AND LOCAL POLARITY INVERSION LINES OF THE LONGITUDINAL MAGNETIC FIELD OF THE ACTIVE REGION by A.V. Borovik, A.A. Zhdanov

“…Using photospheric data and data on the longitudinal magnetic field from the SDO satellite, as well as observations in the Hα line from GONG ground stations, we have studied the flare activity of the NOAA 12673 sunspot group, which in September 2017 produced the largest X9.3 class flare in the last decade. …”
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Damping of visco-resistive Alfven waves in solar spicules by Z Fazel, H Ebadi

“…In other words, with these assumptions, Alfven waves may transfer the photospheric energy to the corona during timescales corresponding to the observed lifetimes of spicules. …”
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Hot Stars With Hot Jupiters Have High Obliquities by Winn, Joshua Nathan, Fabrycky, Daniel C., Albrecht, Simon H., Johnson, John Asher

“…Alternatively, we speculate that hot-Jupiter systems begin with a wide range of obliquities, but the photospheres of cool stars realign with the orbits due to tidal dissipation in their convective zones, while hot stars cannot realign because of their thinner convective zones. …”
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Chemical Composition of the RS CVN-Type Star 29 Draconis by Barisevičius G., Tautvaišienė G., Berdyugina S., Chorniy Y., Ilyin I.

“…Photospheric parameters and chemical composition are determined for the single-lined chromospherically active RS CVn-type star 29 Draconis (HD 160538). …”
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A New Insight into the Linear Theory of Magnetoacoustic Waves in the Homogeneous Flux Tubes with an Abrupt Boundary by Naga Varun Yelagandula

“…An important and interesting issue is brought to notice in the standard linear theory of the magnetoacoustic waves in the homogeneous magnetic flux tubes with an abrupt magnetic boundary, which are representative of the coronal, chromospheric, and photospheric loops of the solar atmosphere. It is shown that the dispersion relation given for the magnetoacoustic waves of such flux tubes by the linear standard theory is generally inapplicable because it does not take into account the electrodynamic boundary condition and the applicability is only restricted to the case β = 0, where β is the usual plasma parameter given by the ratio of the thermodynamic gas pressure to the magnetic pressure. …”
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LS IV — 14°116 : A Time-Resolved Spectroscopic Study by Martin Pamela, Jeffery C. Simon

“…We are currently exploring ways in which to resolve the photospheric motion as a function of optical depth.…”
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Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT by Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj

“…The elemental abundances during the evolution of the microflare are also studied and observed to drop toward photospheric values at the flare peak time, compared to coronal values during the rise and decay phase. …”
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Overstable Convective Modes in a Polytropic Stellar Atmosphere by Bradley W. Hindman, Rekha Jain

“…We suggest that such coupling might enhance the photospheric visibility of a subset of the Sun’s g modes.…”
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On the Origin of Persistent Radio and X-ray Emission from Brown Dwarf TVLM 513-46546 by Alexander Stepanov, Valery Zaitsev

“…It is shown that the source of ≈1 keV X-ray emission is not the entire corona of the brown dwarf, but a population of several hundreds of coronal magnetic loops, with 10 MK plasma heated upon dissipation of the electric current generated by the photospheric convection. Unlike models, which assume a large-scale magnetic structure of the microwave source, our model suggests that the microwave radiation comes from hundreds of magnetic loops quasi-uniformly distributed over the dwarf’s surface. …”
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SN2017ein: bolometric light curve and physical parameters by P.S. Tadjimuratov, D. Mirzakulov

“…Further, we used reconstructed bolometric values to estimate physical parameters using simple one-component models for photospheric and nebular phases. Fitting the models to reconstructed quasi-bolometric light curve allows us to estimate physical parameters. …”
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Hα AND Hβ PROFILE VARIATIONS IN THE SPECTRA OF THE STAR 55 CYG by Y. M. Maharramov

“…We revealed that the structures of photospheric (CII, HeI etc.) absorption line profiles, as well as Hβ line, their radial velocities and equivalent widths are variable.  …”
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The transition region above sunspots by Hui Tian, Tanmoy Samanta, Jingwen Zhang

“…Abstract Over decades, sunspots and their fine structures have been studied in detail at the photospheric level with different ground-based telescopes, as the surface of the Sun primarily emits light in the visible wavelengths. …”
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Chemical Composition of the RS CVn-Type Star Lambda Andromedae by Tautvaišienė G., Barisevičius G., Berdyugina S., Chorniy Y., Ilyin I.

“…Photospheric parameters and chemical composition are determined for the single-lined chromospherically active RS CVn-type star λ And (HD 222107). …”
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NICER Observes a Secondary Peak in the Decay of a Thermonuclear Burst from 4U 1608–52 by Jaisawal, Gaurava K, Chenevez, Jérôme, Bult, Peter, in’t Zand, Jean JM, Galloway, Duncan K, Strohmayer, Tod E, Güver, Tolga, Adkins, Phillip, Altamirano, Diego, Arzoumanian, Zaven, Chakrabarty, Deepto, Coopersmith, Jonathan, Gendreau, Keith C, Guillot, Sebastien, Keek, Laurens, Ludlam, Renee M, Malacaria, Christian

“…Our analysis suggests that the dip and secondary peak are not related to photospheric expansion, varying circumstellar absorption, or scattering. …”
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TYPE I X-RAY BURSTS FROM THE NEUTRON-STAR TRANSIENT XTE J1701–462 by Lin, Dacheng, Altamirano, Diego, Homan, Jeroen, Wijnands, Rudy, Belloni, Tomaso M., Remillard, Ronald A

“…The last two of the three bursts show photospheric radius expansion, from which we estimate the distance to the source to be 8.8 kpc with a 15% uncertainty. …”
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Three-dimensional MHD simulation of the 2008 December 12 coronal mass ejection: from the Sun to Interplanetary space by Zhang Man, Feng Xue Shang, Yang Li Ping

“…The background solar wind is obtained by using a splitting finite-volume scheme based on a six-component grid system in spherical coordinate, with Parker’s one-dimensional solar wind solution and measured photospheric magnetic fields as the initial values. A spherical plasmoid is superposed on the realistic ambient solar wind to study the 12 December 2008 coronal mass ejection event. …”
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Possibilities and problems of solar magnetic field observations for space weather forecast by Demidov M.L.

“…Due to lack of opportunities to observe magnetic fields directly in the corona, the almost only source of various models for quantitative calculation of heliospheric parameters are daily magnetograms measured in photospheric lines and synoptic maps derived from these magnetograms. …”
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A review of the quantitative links between CMEs and magnetic clouds by P. Démoulin

“…Making such a link more quantitative is challenging since it requires a relation between very different kinds of magnetic field measurements: (i) photospheric magnetic maps, which are observed from a distant vantage point (remote sensing) and (ii) in-situ measurements of MCs, which provide precise, directly measured, magnetic field data merely from one-dimensional linear samples. …”
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“Twhirleds”: Spun and whirled affordances controlling multimodal mobile-ambient environments with reality distortion and synchronized lighting to preserve intuitive alignment by Michael Cohen, Rasika Ranaweera, Bektur Ryskeldiev, Tomohiro Oyama, Aya Hashimoto

“…Orientation of a twirled device can be metered, and with a communications infrastructure, this streamed azimuthal data can be used to modulate various distributed, synchronous, multimodal displays, including panoramic and photospherical imagery, diffusion of pantophonic and periphonic auditory soundscapes, and mixed virtuality scenes featuring avatars and props animated by real-world twirling. …”
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Solar Wind Modeling with the Alfvén Wave Solar atmosphere Model Driven by HMI-based Near-real-time Maps by the National Solar Observatory by Nishtha Sachdeva, Ward B. Manchester IV, Igor Sokolov, Zhenguang Huang, Alexander Pevtsov, Luca Bertello, Alexei A. Pevtsov, Gabor Toth, Bart van der Holst, Carl J. Henney

“…We explore the performance of the Alfvén Wave Solar atmosphere Model with near-real-time (NRT) synoptic maps of the photospheric vector magnetic field. These maps, produced by assimilating data from the Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory, use a different method developed at the National Solar Observatory (NSO) to provide a near contemporaneous source of data to drive numerical models. …”
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