English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Context: We present 31.2 days of nearly continuous MOST photometry of theroAp star 10Aql. Aims:The goal was to provide an unambiguous frequencyidentification for this little studied star, as well as to discuss the detectedfrequencies in the context of magnetic models and analyze the influence of themagnetic field on the pulsation. Methods: Using traditional Fourier analysistechniques on three independent data reductions, intrinsic frequencies for thestar are identified. Theoretical non-adiabatic axisymmetric modes influenced bya magnetic field having polar field strengths Bp = 0-5kG were computed tocompare the observations to theory. Results: The high-precision data allow usto identify three definite intrinsic pulsation frequencies and two othercandidate frequencies with low S/N. Considering the observed spacings, only one(50.95microHz) is consistent with the main sequence nature of roAp stars. Thecomparison with theoretical models yields a best fit for a 1.95Msun modelhaving solar metallicity, suppressed envelope convection, and homogenous heliumabundance. Furthermore, our analysis confirms the suspected slow rotation ofthe star and sets new lower limits to the rotation period (Prot>1 month) andinclination (i>30\pm10deg.). Conclusions:The observed frequency spectrum is notrich enough to unambiguously identify a model. On the other hand, the modelshardly represent roAp stars in detail due to the approximations needed todescribe the interactions of the magnetic field with stellar structure andpulsation. Consequently, errors in the model frequencies needed for the fittingprocedure can only be estimated. Nevertheless, it is encouraging that modelswhich suppress convection and include solar metallicity, in agreement withcurrent concepts of roAp stars, fit the observations best.

MOST photometry of the roAp star 10 Aql