Removal of Active Region Inflows Reveals a Weak Solar Cycle Scale Trend in the Near-surface Meridional Flow by Sushant S. Mahajan, Xudong Sun, Junwei Zhao

“…Using time–distance local helioseismology flow maps within 1 Mm of the solar photosphere, we detect inflows toward activity belts that contribute to solar-cycle scale variations in the near-surface meridional flow. …”
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A Statistical Analysis of Spiral-shaped Wave Patterns in Sunspot Umbrae by Juhyung Kang, Jongchul Chae, Jooyeon Geem

“…From the apparent radial speeds of the SWPs and a simple model of wave propagation, we infer that the SWPs may be generated between 2 and 11 Mm below the photosphere with a mean value of about 6 Mm.…”
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PROBING WOLF–RAYET WINDS: CHANDRA/HETG X-RAY SPECTRA OF WR 6 by Huenemoerder, David P., Gayley, K. G., Hamann, W.-R., Ignace, R., Nichols, Joy S., Oskinova, Lidia M., Pollock, A. M. T., Schulz, N. S., Shenar, T.

“…The presence of strong helium-like forbidden lines places the source of X-ray emission at tens to hundreds of stellar radii from the photosphere. Variability was present in X-rays and simultaneous optical photometry, but neither were correlated with the known period of the system or with each other. …”
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Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star by Arcavi, I, Howell, DA, Kasen, D, Bildsten, L, Hosseinzadeh, G, McCully, C, Wong, ZC, Katz, SR, Gal-Yam, A, Sollerman, J, Taddia, F, Leloudas, G, Fremling, C, Nugent, PE, Horesh, A, Mooley, K, Rumsey, C, Cenko, SB, Graham, ML, Perley, DA, Nakar, E, Shaviv, NJ, Bromberg, O, Shen, KJ, Ofek, EO, Cao, Y, Wang, X, Huang, F, Rui, L, Zhang, T, Li, W, Li, Z, Zhang, J, Valenti, S, Guevel, D, Shappee, B, Kochanek, CS, Holoien, TW-S, Filippenko, AV, Fender, R, Nyholm, A, Yaron, O, Kasliwal, MM, Sullivan, M, Blagorodnova, N, Walters, RS, Lunnan, R, Khazov, D, Andreoni, I, Laher, RR, Konidaris, N, Wozniak, P, Bue, B

“…The light curve has at least five peaks and remains bright for more than 600 days; the absorption lines show little to no decrease in velocity; and the radius of the line-forming region is more than an order of magnitude bigger than the radius of the photosphere derived from the continuum emission. These characteristics are consistent with a shell of several tens of solar masses ejected by the progenitor star at supernova-level energies a few hundred days before a terminal explosion. …”

Accretion dynamics and disk evolution in NGC 2264: a study based on the Corot photometric observations by Alencar, S, Teixeira, P, Guimaraes, M, McGinnis, P, Gameiro, J, Bouvier, J, Aigrain, S, Flaccomio, E, Favata, F

“…The percentage of AA Tau-like light curves decreases as the inner disk dissipates, from 40% +- 10% in systems with thick inner disks to 36% +- 16% in systems with anemic disks and none in naked photosphere systems. Indeed, 91% +- 29% of the CTTS with naked photospheres exhibit pure spot-like variability, while only 18% +- 7% of the thick disk systems do so, presumably those seen at low inclination and thus free of variable obscuration. …”

South African crustal fracture fluids preserve paleometeoric water signatures for up to tens of millions of years by Heard, A, Warr, O, Borgonie, G, Linage, B, Kuloyo, O, Fellowes, J, Magnabosco, C, Lau, M, Erasmus, M, Cason, E, van Heerden, E, Kieft, T, Mabry, J, Onstott, T, Lollar, B, Ballentine, C

“…Examples include fluids in the South African Kaapvaal craton which host chemolithoautotrophic microbial communities that survive independent of the photosphere, and billion-year-old fluids in the Canadian Shield, which preserve the Xe isotopic signature of an evolving early atmosphere. …”

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b by Bell, TJ, Crouzet, N, Cubillos, PE, Kreidberg, L, Piette, AAA, Roman, MT, Barstow, JK, Blecic, J, Carone, L, Coulombe, L, Ducrot, E, Hammond, M, Mendonça, JM, Moses, JI, Parmentier, V, Stevenson, KB, Teinturier, L, Zhang, M, Batalha, NM, Bean, JL, Benneke, B, Charnay, B, Chubb, KL, Demory, B, Tan, X, Taylor, J

“…The dayside is consistent with a cloudless atmosphere above the mid-infrared photosphere. Contrary to expectations from equilibrium chemistry but consistent with disequilibrium kinetics models, methane is not detected on the nightside (2σ upper limit of 1–6 ppm, depending on model assumptions). …”

A Blowout Jet Associated with One Obvious Extreme-ultraviolet Wave and One Complicated Coronal Mass Ejection Event by Miao, Yuhu, Liu, Yu, Li, Hong Bo, Shen, Yuan Deng, Yang, Shu Hong, Elmhamdi, Abouazza, Kordi, Ayman S., Abidin, Zamri Zainal

“…It is found that the triggering of the blowout jet was due to the emergence and cancellation of magnetic fluxes on the photosphere. During the rising stage of the jet, the EUV wave appeared just ahead of the jet top, lasting about 4 minutes and at a speed of 458-762 km s-1. …”

A Comprehensive Simulation of Solar Wind Formation from the Solar Interior: Significant Cross-field Energy Transport by Interchange Reconnection near the Sun by Haruhisa Iijima, Takuma Matsumoto, Hideyuki Hotta, Shinsuke Imada

“…Using an extended version of the three-dimensional radiative magnetohydrodynamic code RAMENS, we perform the first comprehensive simulation of the solar wind formation, starting from the wave excitation and the small-scale dynamo below the photosphere. The simulation satisfies various observational constraints as a slow solar wind emanating from the coronal hole boundary. …”
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Transport of Cosmic-Ray Electrons from 1 au to the Sun by Vahé Petrosian, Elena Orlando, Andrew Strong

“…Gamma rays are produced by cosmic-ray (CR) protons interacting with the particles at the solar photosphere and by CR electrons and positrons (CRes) via inverse Compton scattering of solar photons. …”
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Coronal Loop Heating by Nearly Incompressible Magnetohydrodynamic and Reduced Magnetohydrodynamic Turbulence Models by M. S. Yalim, G. P. Zank, M. Asgari-Targhi

“…The transport of waves and turbulence beyond the photosphere is central to the coronal heating problem. …”
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Proposed Resolution to the Solar Open Magnetic Flux Problem by C. Nick Arge, Andrew Leisner, Spiro K. Antiochos, Samantha Wallace, Carl J. Henney

“…The solar magnetic fields emerging from the photosphere into the chromosphere and corona are comprised of a combination of closed (field lines with both ends rooted at the Sun) and open (field lines with only one end at the Sun) fields. …”
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Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A by Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit

“…Transmission spectroscopy is a powerful tool to study exoplanet atmospheres, which can be affected by the ability of stellar photospheric heterogeneity to mimic or mask exoplanetary spectral signatures. …”
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Solar Chromospheric Heating by Magnetohydrodynamic Waves: Dependence on the Inclination of the Magnetic Field by Mayu Koyama, Toshifumi Shimizu

“…(b) The amount of the energy is enhanced toward 10 ^4 W m ^−2 , which is the energy required for heating in the chromospheric plage regions when the magnetic field is higher than 600 G and inclined more than 40°. (c) In the photosphere, the low-frequency component has much more power in the magnetic field inclined more and weaker than 400 G. …”
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Iron Isotope Constraints on the Structure of the Early Solar System by Yves Marrocchi, Maxime Piralla, François L. H. Tissot

“…In this scenario, the CI chondrites—a rare type of carbonaceous chondrites with chemical composition similar to that of the Sun’s photosphere—would sample a distinct source region than other carbonaceous chondrites, located beyond Saturn’s orbit. …”
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ON THE POSSIBLE EXISTENCE OF SUPERSTRONG MAGNETIC FIELDS IN A LIMB SOLAR FLARE by I. I. Yakovkin, V. G. Lozitsky

“…The Zeeman splitting of these emission peaks correspond to magnetic field strength in range 1300-2900 G at altitudes of 10–15 Mm above the level of the photosphere. Magnetic fields of ‘kilogauss’ range (up to 3200 G) were found for some locations also in post-peak phase of the flare. …”
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A SUPER-EDDINGTON, COMPTON-THICK WIND IN GRO J1655–40? by Rahoui, F., Buxton, M., Neilsen, Joseph M. G., Homan, Jeroen

“…Focusing on the X-ray continuum and the optical/infrared/UV spectral energy distribution, we argue that the unusual features of this "hypersoft state" are natural consequences of a super-Eddington Compton-thick wind from the disk: the optical/infrared blackbody represents the cool photosphere of a dense, extended outflow, while the X-ray emission is explained as Compton scattering by the relatively cool, optically thick wind. …”
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What can NuSTAR do for thermonuclear X-ray bursts? by Chenevez, Jerome, Tomsick, John A., Paerels, Frits, Christensen, Finn Erland, Chakrabarty, Deepto

“…The flux released during some strong bu rsts can temporarily exceed the Eddington limit, driving the neutron star photosphere to such large radii that heavy-element ashes of nuclear burning are ejected in the burst expansion wind. …”
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Super-Eddington Winds from Type I X-Ray Bursts by Yu, Hang, Weinberg, Nevin N.

“…This may explain why the photospheric radii of all superexpansion bursts show a transition after ≈1 s from a superexpansion () to a moderate expansion ().…”
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A Prograde, Low-Inclination Orbit for the Very Hot Jupiter WASP-3b by Tripathi, Anjali, Winn, Joshua Nathan, Johnson, John Asher, Howard, Andrew W., Halverson, Sam, Marcy, Geoffrey W., Holman, Matthew J., de Kleer, Katherine R., Carter, Joshua Adam, Esquerdo, G. A., Everett, Mark E., Cabrera, Nicole E.

“…This anomaly could represent the oc- cultation of material erupting from the stellar photosphere, although it is more likely to be an artifact caused by moonlight scattered into the spectrograph.…”
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