Asteroseismic properties of solar-type stars observed with the NASA K2 mission: results from Campaigns 1-3 and prospects for future observations

Mikkel N. Lund, William J. Chaplin, Luca Casagrande, Víctor Silva Aguirre, Sarbani Basu, Allyson Bieryla, Jørgen Christensen-Dalsgaard, David W. Latham, Timothy R. White, Guy R. Davies, Daniel Huber, Lars A. Buchhave, Rasmus Handberg

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We present an asteroseismic analysis of 33 solar-type stars observed in short cadence during Campaigns (C) 1-3 of the NASA K2 mission. We were able to extract both average seismic parameters and individual mode frequencies for stars with dominant frequencies up to ~3300{\mu}Hz, and we find that data for some targets are good enough to allow for a measurement of the rotational splitting. Modelling of the extracted parameters is performed by using grid-based methods using average parameters and individual frequencies together with spectroscopic parameters. For the target selection in C3, stars were chosen as in C1 and C2 to cover a wide range in parameter space to better understand the performance and noise characteristics. For C3 we still detected oscillations in 73% of the observed stars that we proposed. Future K2 campaigns hold great promise for the study of nearby clusters and the chemical evolution and age-metallicity relation of nearby field stars in the solar neighbourhood. We expect oscillations to be detected in ~388 short-cadence targets if the K2 mission continues until C18, which will greatly complement the ~500 detections of solar-like oscillations made for short-cadence targets during the nominal Kepler mission. For ~30-40 of these, including several members of the Hyades open cluster, we furthermore expect that inference from interferometry should be possible.
Original languageEnglish
Article number124204
JournalPublications of the Astronomical Society of the Pacific
Issue number970
Publication statusPublished - 8 Nov 2016

Bibliographical note

17 pages, 15 figures, 4 tables; accepted for publication in PASP


  • astro-ph.SR


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