The Subluminous and Peculiar Type Ia Supernova PTF09dav by Sullivan, M, Kasliwal, M, Nugent, P, Howell, D, Thomas, R, Ofek, E, Arcavi, I, Blake, S, Cooke, J, Gal-Yam, A, Hook, I, Mazzali, P, Podsiadlowski, P, Quimby, R, Bildsten, L, Bloom, J, Cenko, S, Kulkarni, SR, Law, N, Poznanski, D

“…Helium shell detonation or deflagration on the surface of a CO white-dwarf can explain some of the features of PTF09dav, including the presence of Sc and the low photospheric velocities, but the observed Si and Mg are not predicted to be very abundant in these models. …”

Coronal Densities, Temperatures, and Abundances during the 2019 Total Solar Eclipse: The Role of Multiwavelength Observations in Coronal Plasma Characterization by Giulio Del Zanna, Jenna Samra, Austin Monaghan, Chad Madsen, Paul Bryans, Edward DeLuca, Helen Mason, Ben Berkey, Alfred de Wijn, Yeimy J. Rivera

“…EIS and AIR-Spec data indicate that the sulfur abundance (relative to silicon) is photospheric in both regions, confirming our previous results of the 2017 eclipse. …”
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Influence of magnetic reconnection on the eruptive catastrophes of coronal magnetic flux ropes by Quanhao Zhang, Quanhao Zhang, Quanhao Zhang, Xin Cheng, Rui Liu, Rui Liu, Rui Liu, Anchuan Song, Anchuan Song, Anchuan Song, Xiaolei Li, Xiaolei Li, Xiaolei Li, Yuming Wang, Yuming Wang, Yuming Wang

“…Further studies discovered that the catastrophe does not necessarily exist: The flux rope system with certain photospheric flux distributions could be non-catastrophic. …”
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Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna by Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein

“…The Zeeman effect has been routinely used to image and quantify the solar photospheric magnetic field (B). Such a direct measuring technique is not yet available for the corona (Lin et al. 2004). …”
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Evolution of Magnetic Fields and Energy Release Processes during Homologous Eruptive Flares by Suraj Sahu, Bhuwan Joshi, Avijeet Prasad, Kyung-Suk Cho

“…Over an interval of ≈ 44 hr, the photospheric magnetic field encompassing the three flares undergoes important phases of emergence and cancellation, together with significant changes near the polarity inversion lines within the flaring region. …”
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Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327 by Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo

“…Massive stars can present peculiar photospheric abundances that are unlikely to record the abundances of their former protoplanetary disks. …”
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Magnetar Giant Flare Origin for GRB 210410A? by Guo-Yu Li, Da-Bin Lin, Guo-Peng Li, Zhi-Lin Chen, Hai-Ming Zhang, Xiang-Gao Wang, En-Wei Liang

“…The radiation spectrum of GRB 210410A, similar to that of GRB 200415A, can be well fitted with a non-dissipative photospheric emission. However, GRB 210410A in the E _p, _z − L _iso plane is beyond the death line of cosmic GRBs for non-dissipated photospheric emission with a general initial size of the fireball. …”
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Data-driven Radiative Magnetohydrodynamics Simulations with the MURaM Code by Feng Chen, Mark C. M. Cheung, Matthias Rempel, Georgios Chintzoglou

“…The horizontal electric field that is derived from the full velocity and magnetic vectors is implemented at the photospheric (bottom) boundary to drive the induction equation. …”
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How Turbulent is the Magnetically Closed Corona? by James A. Klimchuk, Spiro K. Antiochos

“…The sheets form by various processes that do not involve a traditional turbulent cascade whereby energy flows losslessly through a continuum of spatial scales starting from the large scale of the photospheric driving. If such an inertial range is a defining characteristic of turbulence, then the magnetically closed corona is not a turbulent system. …”
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HYDROGEN LINES IN B-e STARS ENVELOPES by S. N. Udovichenko, E. I. Konchagina

“…The emission profiles of stars were obtained by subtracting from “A Be star atlas” photospheric line profiles which were computed from Kurucz models and corrected from gravity and rotation. …”
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Correlating Intrinsic Stellar Parameters with Mg ii Self-reversal Depths by Anna Taylor, Audrey Dunn, Sarah Peacock, Allison Youngblood, Seth Redfield

“…We quantify the sensitivity of the visible and near-infrared photometry to chromospheric and photospheric parameters. We find weak trends between Mg ii k self-reversal depth and age, rotation period, Mg ii luminosity, temperature, and mass. …”
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SN 2022oqm–A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material by Ido Irani, Ping Chen, Jonathan Morag, Steve Schulze, Avishay Gal-Yam, Nora L. Strotjohann, Ofer Yaron, Erez A. Zimmerman, Amir Sharon, Daniel A. Perley, J. Sollerman, Aaron Tohuvavohu, Kaustav K. Das, Mansi M. Kasliwal, Rachel Bruch, Thomas G. Brink, WeiKang Zheng, Alexei V. Filippenko, Kishore C. Patra, Sergiy S. Vasylyev, Yi Yang, Matthew J. Graham, Joshua S. Bloom, Paolo Mazzali, Josiah Purdum, Russ R. Laher, Avery Wold, Yashvi Sharma, Leander Lacroix, Michael S. Medford

“…After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s ^−1 , in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. …”
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Survey of Magnetic Field Parameters Associated with Large Solar Flares by Ting Li, Yanfang Zheng, Xuefeng Li, Yijun Hou, Xuebao Li, Yining Zhang, Anqin Chen

“…Here, we calculate the key magnetic field parameters within the area of high photospheric free energy density (HED region) for 323 ARs (217 C- and 106 M/X-flaring ARs), including total photospheric free magnetic energy density E _free , total unsigned magnetic flux Φ _HED , mean unsigned current helicity h _c , length of the polarity inversion lines L _PIL with a steep horizontal magnetic gradient, etc., and compare these with flare/coronal mass ejection (CME) properties. …”
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Understanding Sun-as-a-Star Variability of Solar Balmer Lines by S. Criscuoli, S. Marchenko, M. DeLand, D. Choudhary, G. Kopp

“…The fact that core and wings contribute in a similar manner to the variability, and current knowledge of Balmer-lines formation in stellar atmospheres, supports the notion that Balmer line core-to-wing ratio indices behave more like photospheric rather than chromospheric indices.…”
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Spectroscopic Study Of Light Curve And Physical Properties For SN2010jl by Adil N. Ayyash, Zeyad A. Saleh

“…Also, temperature of black body of SN2010jl during photospheric phase were calculated depending on data taken from optical spectrum curve and by applying special mathematical equation. …”
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The Influence of Chemi-Ionization and Recombination Processes on Spectral Line Shapes in Stellar Atmospheres by Mihajlov Anatolij A., Ignjatović Ljubinko M., Srécković Vladimir A., Dimitrijević Milan S.

“…The presented results are related to the photospheres of the Sun and some M red dwarfs, as well as weakly ionized layers of DB white dwarf atmospheres. …”
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On a limitation of Zeeman polarimetry and imperfect instrumentation in representing solar magnetic fields with weaker polarization signal by Pevtsov A.A., Liu Y., Virtanen I., Bertello L., Mursula K., Leka K.D., Hughes A.L.H.

“…This limitation stems from our ability to interpret the differing character of the Zeeman polarization signals which arise from the photospheric line-of-sight vs. the transverse components of the solar vector magnetic field, and is likely exacerbated by unresolved structure (non-unity fill fraction) as well as the disambiguation of the 180° degeneracy in the transverse-field azimuth. …”
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Search for high energy neutrinos from bright GRBs with ANTARES by Sanguineti M., Celli S., Turpin D.

“…In this paper two of most promising models of the GRB neutrino emission will be studied: the internal shock model and the photospheric model. No muons have been measured in space and time correlation with the selected GRBs and upper limits at 90% C.L. on the expected neutrino fluxes have been derived. …”
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Photometric Study on the Spot-Double Star XY Urase Majoris (I) by Woo-Baik Lee

“…Observational evidence for photospheric and chromospheric activities on the XY UMa are also discussed.…”
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MICROWAVE INDICATOR OF POTENTIAL GEOEFFECTIVENESS AND MAGNETIC FLUX-ROPE STRUCTURE OF A SOLAR ACTIVE REGION by A.V. Kudriavtseva, I.I. Myshyakov, A.M. Uralov, V.V. Grechnev

“…Calculation of the coronal magnetic field in a non-linear force-free approximation has revealed an extended structure consisting of interconnected magnetic flux ropes, located practically along the entire length of the main polarity separation line of the photospheric magnetic field. NLS is projected into the region of the strongest horizontal magnetic field, where the main energy of this structure is concentrated. …”
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