Long term radial velocity variations of the Sun as a star: The HARPS view
Texto completo
Figure
Documento similar
(2) The flux and radial-velocity variations observed for a line’s individual spectral features can be ex- plained in a model in which the maser spots form elongated chains or
Ultimately, as pointed out in the previous section, a long term observation of the position of the detected vehicles throughout a given video frame can yield a
Recent reports of long-term outcomes for radial shortening osteotomy in osteonecrosis early stage patients and for proximal row carpectomy (PRC) in advanced Kienböck’s disease
Radial velocity surveys are not biased against the discovery of brown dwarfs (de- fined here as object more massive than 13 M U?VXW ) as their perturbation on the parent stars
We find that the parameters of the model assumed for the radial profile of the rotational velocity, averaged over the considered lines of sight, are in agreement within two
of the subspace generated by the right singular vectors of the coefficient matrix, set up according to the entanglement classes which its generators belong to.. As a secondary
Over the last ten years, we have monitored about 1000 evolved stars for radial velocity variations in the search for low-mass companions under the Penn State – Torun Centre
2 we present the available observations and discuss the influence of the stellar ac- tivity on the radial velocity (RV) variation measurements. Sec- tion 3 shows the results of