2010/11/03 by M. Bazot, M. J. Ireland, Michael Ireland +38 · 101 citations
Physics and Astronomy · #Asteroseismology #Astro and Planetary Science #Astronomical and nuclear sciences #Astronomy #Astrophysics #Coronal mass ejection #Interferometry #Nuclear physics #Physics #Plasma #RADIUS #Solar mass #Solar radius #Solar wind #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201015679
published in Astronomy and Astrophysics 526, L4 (EDP Sciences) · 5 pages, 5 figures
openalex publication_date 2010/11/03 · arxiv created 2012/09/11 · arxiv updated 2015/06/11 · openalex created_date 2020/11/23 · openalex updated_date 2026/08/05
The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.