Benjamin Beeck
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View article: Spectral variability of photospheric radiation due to faculae – II. Facular contrasts for cool main-sequence stars
Spectral variability of photospheric radiation due to faculae – II. Facular contrasts for cool main-sequence stars Open
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 signatures of faculae are poorly understood, limiting ou…
View article: Spectral variability of photospheric radiation due to faculae II: Facular contrasts for cool main-sequence stars
Spectral variability of photospheric radiation due to faculae II: Facular contrasts for cool main-sequence stars Open
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 signatures of faculae are poorly understood, limiting ou…
View article: The influence of convective blueshift on radial velocities of F, G, and K stars
The influence of convective blueshift on radial velocities of F, G, and K stars Open
Context. Apparent radial velocity (RV) signals induced by stellar surface features such as spots and plages can result in a false planet detection or hide the presence of an orbiting planet. Our ability to detect rocky exoplanets is curren…
View article: Publisher’s Note: Solar Irradiance Variability is Caused by the Magnetic Activity on the Solar Surface [Phys. Rev. Lett. <b>119</b>, 091102 (2017)]
Publisher’s Note: Solar Irradiance Variability is Caused by the Magnetic Activity on the Solar Surface [Phys. Rev. Lett. <b>119</b>, 091102 (2017)] Open
This corrects the article DOI: 10.1103/PhysRevLett.119.091102.
View article: Solar Irradiance Variability is Caused by the Magnetic Activity on the Solar Surface
Solar Irradiance Variability is Caused by the Magnetic Activity on the Solar Surface Open
The variation in the radiative output of the Sun, described in terms of solar irradiance, is important to climatology. A common assumption is that solar irradiance variability is driven by its surface magnetism. Verifying this assumption h…
View article: Estimates of Active Region Area Coverage through Simultaneous Measurements of the He i λλ 5876 and 10830 Lines
Estimates of Active Region Area Coverage through Simultaneous Measurements of the He i λλ 5876 and 10830 Lines Open
Simultaneous, high-quality measurements of the neutral helium triplet features at 5876 Å and 10830 Å in a sample of solar-type stars are presented. The observations were made with ESO telescopes at the La Silla Paranal Observatory under pr…
View article: Radial velocity observations of the 2015 Mar. 20 eclipse
Radial velocity observations of the 2015 Mar. 20 eclipse Open
\n Spectroscopic observations of a solar eclipse can provide unique information for solar\n and exoplanet research; the huge amplitude of the Rossiter-McLaughlin (RM) effect during\n solar eclipse and the high precision of solar radial vel…
View article: Radial velocity observations of the 2015 Mar 20 eclipse - A benchmark Rossiter-McLaughlin curve with zero free parameters
Radial velocity observations of the 2015 Mar 20 eclipse - A benchmark Rossiter-McLaughlin curve with zero free parameters Open
On March 20, 2015, we obtained 159 spectra of the Sun as a star with the solar telescope and the FTS at the Institut für Astrophysik Göttingen, 76 spectra were taken during partial solar eclipse. We obtained RVs using $I_2$ as wavelength r…
View article: Modelling The Spectral Contrasts Of Stellar Faculae.
Modelling The Spectral Contrasts Of Stellar Faculae. Open
Facular contrasts are an important parameter in modelling stellar variability and exoplanet transits. The ultimate goal of this work will be to model the contrasts of faculae for different spectral types and thus improve the modelling of s…
View article: MESA meets MURaM
MESA meets MURaM Open
Context. Space-based observations of solar-like oscillators have identified large numbers of stars in which many individual mode frequencies can be precisely measured. However, current stellar models predict oscillation frequencies that ar…
View article: MESA meets MURaM: Surface effects in main-sequence solar-like oscillators computed using three-dimensional radiation hydrodynamics simulations
MESA meets MURaM: Surface effects in main-sequence solar-like oscillators computed using three-dimensional radiation hydrodynamics simulations Open
... [C]urrent stellar models predict oscillation frequencies that are systematically affected by simplified modelling of the near-surface layers. We use three-dimensional radiation hydrodynamics simulations to better model the near-surface…
View article: The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems
The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems Open
When a planet transits its host star, it blocks regions of the stellar surface from view; this causes a distortion of the spectral lines and a change in the line-of-sight (LOS) velocities, known as the Rossiter-McLaughlin (RM) effect. Sinc…
View article: Three-dimensional simulations of near-surface convection in main-sequence stars
Three-dimensional simulations of near-surface convection in main-sequence stars Open
\n Context. The convective envelopes of cool main-sequence stars harbour magnetic fields with a complex global and local structure. These fields affect the near-surface convection and the outer stellar atmospheres in many ways and are resp…
View article: Three-dimensional simulations of near-surface convection in main-sequence stars
Three-dimensional simulations of near-surface convection in main-sequence stars Open
Context. Magnetic fields affect the local structure of the photosphere of stars. They can considerably influence the radiative properties near the optical surface, flow velocities, and the temperature and pressure profiles. This has an imp…
View article: Three-dimensional simulations of near-surface convection in main-sequence stars
Three-dimensional simulations of near-surface convection in main-sequence stars Open
The convective envelopes of cool main-sequence stars harbour magnetic fields with a complex global and local structure. These fields affect the near-surface convection and the outer stellar atmospheres in many ways and are responsible for …
View article: Three-dimensional simulations of near-surface convection in main-sequence stars. IV. Effect of small-scale magnetic flux concentrations on centre-to-limb variation and spectral lines
Three-dimensional simulations of near-surface convection in main-sequence stars. IV. Effect of small-scale magnetic flux concentrations on centre-to-limb variation and spectral lines Open
Magnetic fields affect the local structure of the photosphere of stars. They can considerably influence the radiative properties near the optical surface, flow velocities, and the temperature and pressure profiles. We aim at understanding …
View article: Three-dimensional simulations of near-surface convection in main-sequence stars. III. The structure of small-scale magnetic flux concentrations
Three-dimensional simulations of near-surface convection in main-sequence stars. III. The structure of small-scale magnetic flux concentrations Open
The convective envelopes of cool main-sequence stars harbour magnetic fields with a complex global and local structure. These fields affect the near-surface convection and the outer stellar atmospheres in many ways and are responsible for …