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Power spectra of solar brightness variations at various inclinations

MPS-Authors

Nèmec,  N.-E.
ERC Starting Grant: Connecting Solar and Stellar Variabilities (SOLVe), Max Planck Institute for Solar System Research, Max Planck Society;

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Shapiro,  Alexander
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;
ERC Starting Grant: Connecting Solar and Stellar Variabilities (SOLVe), Max Planck Institute for Solar System Research, Max Planck Society;

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Solanki,  Sami K.
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

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Tagirov,  Rinat
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

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Cameron,  Robert H.
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

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Citation

Nèmec, N.-E., Shapiro, A., Krivova, N. A., Solanki, S. K., Tagirov, R., Cameron, R. H., et al. (2020). Power spectra of solar brightness variations at various inclinations. Astronomy and Astrophysics, 636: A43. doi:10.1051/0004-6361/202037588.


Cite as: http://hdl.handle.net/21.11116/0000-0006-53A5-2
Abstract
Context. Magnetic features on the surfaces of cool stars lead to variations in their brightness. Such variations on the surface of the Sun have been studied extensively. Recent planet-hunting space telescopes have made it possible to measure brightness variations in hundred thousands of other stars. The new data may undermine the validity of setting the sun as a typical example of a variable star. Putting solar variability into the stellar context suffers, however, from a bias resulting from solar observations being carried out from its near-equatorial plane, whereas stars are generally observed at all possible inclinations. Aims. We model solar brightness variations at timescales from days to years as they would be observed at different inclinations. In particular, we consider the effect of the inclination on the power spectrum of solar brightness variations. The variations are calculated in several passbands that are routinely used for stellar measurements. Methods. We employ the surface flux transport model to simulate the time-dependent spatial distribution of magnetic features on both the near and far sides of the Sun. This distribution is then used to calculate solar brightness variations following the Spectral And Total Irradiance REconstruction approach. Results. We have quantified the effect of the inclination on solar brightness variability at timescales down to a single day. Thus, our results allow for solar brightness records to be made directly comparable to those obtained by planet-hunting space telescopes. Furthermore, we decompose solar brightness variations into components originating from the solar rotation and from the evolution of magnetic features.