The abundances of heavy elements in BL138 – red giant of local group fornax dwarf spheroidal galaxy by V.F. Gopka, A.V. Yushchenko, V.A. Yushchenko, A.V. Shavrina, S.M. Andrievsky, Y. Jeong, E.P. Shereta

“…The analysis of these abundances and also previously published investigation of BL138 allowed claiming that the distribution of abundances is different from that in the solar photosphere. The signs of r-process in the abundance pattern of BL138 are not important. …”
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Our dynamic sun: 2017 Hannes Alfvén Medal lecture at the EGU by E. Priest, E. Priest

“…A small-scale dynamo may also be operating near the surface of the Sun, generating magnetic fields that thread the lowest layer of the solar atmosphere, the turbulent photosphere. Above the photosphere lies the highly dynamic fine-scale chromosphere, and beyond that is the rare corona at high temperatures exceeding 1 million degrees K. …”
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Investigations of the MnI 539.47 nm and MnI 542.04 nm lines in solar plages by Vince Ištvan I., Gopasyuk O., Gopasyuk S., Vince Oliver I.

“…We observed the MnI 539.47 nm and 542.04nm line profiles in the quiet photosphere and plage regions in 1998 and 2001, and measured the full widths at half maximum, equivalent widths and depths of these profiles. …”
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A Bright First Day for Tidal Disruption Events by Xiaoshan Huang, Shane W. Davis, Yan-fei Jiang

“…The average gas temperature at this photospheric surface is a few × 10 ^4 K, roughly consistent with inferred prepeak photosphere properties for some optical TDEs. …”
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The Van Hoof Effect over the Blazhko Cycle by Merieme Chadid

“…We investigate the differential motion between the upper and lower photosphere and between the photosphere and high atmosphere in the RR Lyr star. …”
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The Three Regimes of Atmospheric Evaporation for Super-Earths and Sub-Neptunes by Darius Modirrousta-Galian, Jun Korenaga

“…The second regime applies to planets with lower internal temperatures, so a radiative region forms, but the photosphere still remains outside the Bondi radius. …”
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Element abundance and the physics of solar energetic particles by Donald V. Reames

“…Thus, SEPs provide a measurement of element abundance in the solar corona, distinct from solar wind, and may even better define the photosphere for some elements.…”
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The abundances of heavy elements in the atmosphere of hyades giant 6 Tauri by V. F. Gopka

“…Comparison of synthetic spectrum of the б Tauri photosphere and high quality spectral atlas of this star permit us to identify absorption lines of iron and heavy elements Z ≥ 30 in the observed spectrum. …”
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Magnetic Structure of Sunspots by Juan M. Borrero, Kiyoshi Ichimoto

“…We start by offering a brief description of tools that are most commonly employed to infer the magnetic field in the solar atmosphere with emphasis in the photosphere of sunspots. We then address separately the global and local magnetic structure of sunspots, focusing on the implications of the current observations for the different sunspots models, energy transport mechanisms, extrapolations of the magnetic field towards the Corona, and other issues.…”
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THE ABUNDANCES OF SOME HEAVY ELEMENTS IN THE ATMOSPHERE OF γ TAURI by A. V. Yushchenko, V. F. Gopka

“…Comparison of synthetic spectrum of the γ Tauri photosphere and high quality spectral atlases of this star permit us to identify absorption lines of rubidium, indium, disprosium, erbium, osmium in the observed spectra. …”
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Asymmetric Twisting of Coronal Loops by Gabriele Cozzo, Paolo Pagano, Antonino Petralia, Fabio Reale

“…The bright solar corona entirely consists of closed magnetic loops rooted in the photosphere. Photospheric motions are important drivers of magnetic stressing, which eventually leads to energy release into heat. …”
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Outflowing Helium from a Mature Mini-Neptune by Michael Zhang, Fei Dai, Jacob L. Bean, Heather A. Knutson, Federica Rescigno

“…Here W _avg is the equivalent width of the helium absorption, and ρ _XUV is the density of the planet within the XUV photosphere, but the correlation is similarly strong if we use the optical photosphere. …”
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Spatial and temporal variations of Ca II K line profile shapes in different structures of solar chromosphere. I. Features of individual profiles by Turova I.P., Grigoryeva S.A., Ozhogina O.A.

“…There are, however, structures which begin to differ at the level of the photosphere and continue to differ in the chromosphere. …”
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Disentangling the Planet from the Star in Late-Type M Dwarfs: A Case Study of TRAPPIST-1g by Wakeford, HR, Lewis, NK, Fowler, J, Bruno, G, Wilson, TJ, Moran, SE, Valenti, J, Batalha, NE, Filippazzo, J, Bourrier, V, Hörst, SM, Lederer, SM, de Wit, J

“…We find that TRAPPIST-1 is a 0.08 M ∗, 0.117 R ∗, M8V star with a photospheric effective temperature of 2400 K, with ∼35% 3000 K spot coverage and a very small fraction, <3%, of ∼5800 K hot spot. …”
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Pengamatan dan Analisa Sunspot di Stasion Pengamatan Matahari Haurngombong Tanjungsari by Sinambela, Wilson

“…Sunspot adalah noda hitam yang terdapat pada permukaan matahari (photosphere), yang merupakan salah satu phenomena aktivitas matahari yang dapat dilihat secara visual dengan bantuan fillter cahaya putih. …”
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Magnetic Fields in the Solar Convection Zone by Yuhong Fan

“…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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Re-evaluating hot Jupiter WASP-12b: An update by Tanaka Ichi, Hansen Brad M.S., Barman Travis, Crossfield Ian J.M., Kodama Tadayuki

“…We show that this new spectrum is still consistent with a featureless blackbody, indicating a nearly isothermal photosphere on the planet's day side. Thus the ensemble of occultation measurements for WASP-12b is still insufficient to constrain the planet's atmospheric composition.…”
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Propagation Properties of Sunspots Umbral Oscillations in Horizontal and Vertical Directions by Wei Wu, Jiang-tao Su, Jie Chen, Xiao-shuai Zhu, Robert Sych

“…We speculate that oscillations in two of the umbrae have a common origin in the sub-photosphere, resulting in a stronger correlation (>30%). …”
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Artificial Intelligence Assisted Inversion (AIAI): Quantifying the Spectral Features of 56Ni of Type Ia Supernovae by Xingzhuo Chen, Lifan Wang, Lei Hu, Peter J. Brown

“…The neural networks are applied to derive the mass of ^56 Ni in velocity ranges above the photosphere for a sample of 124 well-observed SNe Ia in the TARDIS model context. …”
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Disentangling the Planet from the Star in Late-Type M Dwarfs: A Case Study of TRAPPIST-1g by Wakeford, HR, Lewis, NK, Fowler, J, Bruno, G, Wilson, TJ, Moran, SE, Valenti, J, Batalha, NE, Filippazzo, J, Bourrier, V, Hörst, SM, Lederer, SM, de Wit, J

“…We find that TRAPPIST-1 is a 0.08 M ∗, 0.117 R ∗, M8V star with a photospheric effective temperature of 2400 K, with ∼35% 3000 K spot coverage and a very small fraction, <3%, of ∼5800 K hot spot. …”
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