To obtain cm/s precision, stellar surface magneto-convection must be disentangled from observed radial velocities (RVs). In order to understand and remove the convective signature, we create Sun-as-a-star model observations based on a 3D magnetohydrodynamic solar simulation. From these Sun-as-a-star model observations, we find several line characteristics are correlated with the induced RV shifts. The aim of this campaign is to feed directly into future high precision RV studies, such as the search for habitable, rocky worlds, with forthcoming spectrographs such as ESPRESSO.
|Title of host publication||Proceedings of the 18th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun: Lowell Observatory|
|Number of pages||8|
|Publication status||Published - 11 Aug 2014|
Bibliographical note6 pages, 3 figures; presented at the 18th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CoolStars18); to appear in the proceedings of Lowell Observatory (9-13 June 2014), edited by G. van Belle & H. Harris. Updated with correct y-axis units on righthand plot in figure 3
Cegla, H. M., Watson, C. A., Shelyag, S., & Mathioudakis, M. (2014). Understanding Astrophysical Noise from Stellar Surface Magneto-Convection. In Proceedings of the 18th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun: Lowell Observatory (pp. 567-574) http://www2.lowell.edu/workshops/coolstars18/articles/070-Cegla+_CS18.pdf