2015/02/11 by Joanne Breitfelder, J. Breitfelder, P. Kervella +12 · 25 citations
Physics and Astronomy · #Amplitude #Angular diameter #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Cepheid variable #Interferometry #Optics #Parallax #Photometry (optics) #Physics #Radial velocity #Stars #Stellar, planetary, and galactic studies #astro-ph.IM #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201425171
published in Astronomy and Astrophysics 576, A64 (EDP Sciences) · 8 pages, 6 figures, accepted in A&A
openalex publication_date 2015/02/11 · arxiv created 2015/03/17 · arxiv updated 2015/06/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
Context. The distance of pulsating stars, in particular Cepheids, are commonly measured using the parallax of pulsation technique. The different versions of this technique combine measurements of the linear diameter variation (from spectroscopy) and the angular diameter variation (from photometry or interferometry) amplitudes, to retrieve the distance in a quasi-geometrical way. However, the linear diameter amplitude is directly proportional to the projection factor (hereafter p-factor), which is used to convert spectroscopic radial velocities (i.e., disk integrated) into pulsating (i.e., photospheric) velocities. The value of the p-factor and its possible dependence on the pulsation period are still widely debated.