Zobrazeno 1 - 10
of 32
pro vyhledávání: '"Beeck, Benjamin"'
Autor:
Norris, Charlotte M., Unruh, Yvonne C., Witzke, Veronika, Solanki, Sami K., Krivova, Natalie A., Shapiro, Alexander I., Cameron, Robert, Beeck, Benjamin
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 our ability t
Externí odkaz:
http://arxiv.org/abs/2306.04669
Autor:
Norris, Charlotte M., Beeck, Benjamin, Unruh, Yvonne C., Solanki, Sami K., Krivova, Natalie A., Yeo, Kok Leng
Publikováno v:
A&A 605, A45 (2017)
Context. Stellar spectral variability on timescales of a day and longer, arising from magnetic surface features such as dark spots and bright faculae, is an important noise source when characterising extra-solar planets. Current 1D models of faculae
Externí odkaz:
http://arxiv.org/abs/1705.04455
Publikováno v:
A&A 595, A26 (2016)
On March 20, 2015, we obtained 159 spectra of the Sun as a star with the solar telescope and the FTS at the Institut f\"ur Astrophysik G\"ottingen, 76 spectra were taken during partial solar eclipse. We obtained RVs using $I_2$ as wavelength referenc
Externí odkaz:
http://arxiv.org/abs/1609.00535
Publikováno v:
A&A 581, A43 (2015)
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 qualitative
Externí odkaz:
http://arxiv.org/abs/1505.04744
Publikováno v:
A&A 581, A42 (2015)
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 the observa
Externí odkaz:
http://arxiv.org/abs/1505.04739
The solar photospheric magnetic field is highly structured owing to its interaction with the convective flows. Its local structure has a strong influence on the profiles of spectral lines not only by virtue of the Zeeman effect, but also through the
Externí odkaz:
http://arxiv.org/abs/1408.1802
The near-surface layers of cool main-sequence stars are structured by convective flows, which are overshooting into the atmosphere. The flows and the associated spatio-temporal variations of density and temperature affect spectral line profiles and t
Externí odkaz:
http://arxiv.org/abs/1308.4874
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 of the stellar atmospheres analogous to solar granulation. The flows have con
Externí odkaz:
http://arxiv.org/abs/1308.4873
We carried out 3D radiative magnetohydrodynamic simulations of the convective and magnetic structure in the surface layers (uppermost part of the convection zone and photosphere) of main-sequence stars of spectral types F3 to M2. The simulation resul
Externí odkaz:
http://arxiv.org/abs/1101.3848