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[HTML][HTML] Flux emergence (theory)
Magnetic flux emergence from the solar convection zone into the overlying atmosphere is
the driver of a diverse range of phenomena associated with solar activity. In this article, we …
the driver of a diverse range of phenomena associated with solar activity. In this article, we …
[HTML][HTML] Sunspot modeling: from simplified models to radiative MHD simulations
M Rempel, R Schlichenmaier - Living Reviews in Solar Physics, 2011 - Springer
We review our current understanding of sunspots from the scales of their fine structure to
their large scale (global) structure including the processes of their formation and decay …
their large scale (global) structure including the processes of their formation and decay …
The Stagger-grid: A grid of 3D stellar atmosphere models-I. Methods and general properties
Aims. We present the Stagger-grid, a comprehensive grid of time-dependent, three-
dimensional (3D), hydrodynamic model atmospheres for late-type stars with realistic …
dimensional (3D), hydrodynamic model atmospheres for late-type stars with realistic …
Non-LTE oxygen line formation in 3D hydrodynamic model stellar atmospheres
The O i 777 nm lines are among the most commonly used diagnostics for the oxygen
abundances in the atmospheres of FGK-type stars. However, they form in conditions that are …
abundances in the atmospheres of FGK-type stars. However, they form in conditions that are …
Measuring precise radial velocities on individual spectral lines-III. Dependence of stellar activity signal on line formation temperature
K Al Moulla, X Dumusque, M Cretignier, Y Zhao… - Astronomy & …, 2022 - aanda.org
Context. To enable radial velocity (RV) precision on the order of~ 0.1 ms− 1 required for the
detection of Earth-like exoplanets orbiting solar-type stars, the main obstacle lies in …
detection of Earth-like exoplanets orbiting solar-type stars, the main obstacle lies in …
Three-dimensional simulations of near-surface convection in main-sequence stars-II. Properties of granulation and spectral lines
Context. The atmospheres of cool main-sequence stars are structured by convective flows
from the convective envelope that penetrate the optically thin layers and lead to structuring …
from the convective envelope that penetrate the optically thin layers and lead to structuring …
Spectral variability of photospheric radiation due to faculae–II. Facular contrasts for cool main-sequence stars
CM Norris, YC Unruh, V Witzke… - Monthly Notices of …, 2023 - academic.oup.com
Magnetic features on the surface of stars, such as spots and faculae, cause stellar spectral
variability on time-scales of days and longer. For stars other than the Sun, the spectral …
variability on time-scales of days and longer. For stars other than the Sun, the spectral …
The solar chromosphere at high resolution with IBIS-I. New insights from the Ca II 854.2 nm line
Context. The chromosphere remains a poorly understood part of the solar atmosphere, as
current modeling and observing capabilities are still ill-suited to investigating its fully 3 …
current modeling and observing capabilities are still ill-suited to investigating its fully 3 …
The magnetic connection between the convection zone and corona in the quiet Sun
WP Abbett - The Astrophysical Journal, 2007 - iopscience.iop.org
To understand the dynamic, magnetic, and energetic connection between the convectively
unstable layers below the visible surface of the Sun and the overlying solar corona, we have …
unstable layers below the visible surface of the Sun and the overlying solar corona, we have …
[HTML][HTML] GRB 161219B/SN 2016jca: A low-redshift gamma-ray burst supernova powered by radioactive heating
Since the first discovery of a broad-lined type Ic supernova (SN) with a long-duration gamma-
ray burst (GRB) in 1998, fewer than fifty GRB-supernovae (SNe) have been discovered. The …
ray burst (GRB) in 1998, fewer than fifty GRB-supernovae (SNe) have been discovered. The …