Results 181 to 190 of about 1,966 (233)

Horizontal and vertical exoplanet thermal structure from a JWST spectroscopic eclipse map. [PDF]

Nat Astron
Challener RC, Weiner Mansfield M, Cubillos PE, Piette AAA, Coulombe LP, Beltz H, Blecic J, Rauscher E, Bean JL, Benneke B, Kempton EM, Harrington J, Komacek TD, Parmentier V, Casewell SL, Iro N, Mancini L, Nixon MC, Radica M, Steinrueck ME, Welbanks L, Batalha NM, Caceres C, Crossfield IJM, Crouzet N, Désert JM, Molaverdikhani K, Nikolov NK, Palle E, Rackham BV, Schlawin E, Sing DK, Stevenson KB, Tan X, Turner JD, Zhang X.   +35 more
europepmc   +1 more source

Combined Surface Flux Transport and Helioseismic Far-Side Active Region Model (FARM). [PDF]

Sol Phys
Yang D, Heinemann SG, Cameron RH, Gizon L.   +3 more
europepmc   +1 more source

Computation and analysis of flow patterns in the solar photosphere.

, 1974
Richard G. Hendl
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Solar Photosphere

2020
The Sun is a G2V star with an effective temperature of 5780 K. As the nearest star to Earth and the biggest object in the solar system, it serves as a reference for fundamental astronomical parameters such as stellar mass, luminosity, and elemental abundances. It also serves as a plasma physics laboratory.
L. P. Chitta, H. N. Smitha, S. K. Solanki   +2 more
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Solar Filaments and Photospheric Network

Solar Physics, 2005
The locations of barbs of quiescent solar filaments are compared with the photospheric/chromospheric network, which thereby serves as a proxy of regions with enhanced concentrations of magnetic flux. The study covers quiet regions, where also the photospheric network as represented by flow converging regions, i.e., supergranular cell boundaries ...
Yong Lin, Jun Elin Wiik, Oddbjørn Engvold, Luc Rouppe Van Der Voort, Zoe A. Frank   +4 more
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Inhomogeneities in the solar photosphere

Solar Physics, 1969
A model of the solar photosphere incorporating a simple two-stream representation of granulation is found to give a small but significant improvement in the continuous radiation field over a homogeneous model. It is common to assume that the pressure does not vary with horizontal position; however, this assumption cannot be valid if the material is in ...
Thomas E. Margrave, Thomas L. Swihart
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Waves in the solar photosphere

Solar Physics, 1987
Time-sequences of line profile data have been subjected to a unique analysis which produces an amplitude and phase of the velocity and intensity at several line depths for each time sample and spatial point on the Sun. The data have been filtered to pass only the frequencies and spatial wavenumbers of the 5-min band.
Robin Stebbins, PhilipR. Goode
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Magnetic fields in the solar photosphere

Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, 2008
Recent high-resolution observations of the surface of the Sun have revealed the fine structure of a vast array of complex photospheric magnetic features. Observations of these magnetic field structures have already greatly enhanced our theoretical understanding of the interactions between magnetic fields and turbulent convection, and future ...
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Molecules in the solar photosphere

Solar Physics, 1969
A consideration of the dissociation equilibrium of diatomic molecules in the Utrecht Reference Photosphere leads us to conclude that SH, SiO, CS, HF and HCl may show up in enough concentrations in the solar atmosphere. The number above photosphere for these molecules is comparable with or more than that of MgH.
M. C. Pande, V. P. Gaur, B. M. Tripathi
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