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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

SPB star HD 50230, in fact a hybrid B-type pulsator, has been observed byCoRoT least 137 days. A nearly equidistant period spacing pattern are foundamong 8 modes which are extracted from the oscillation spectrum with more than500 frequencies. However, it is thought to be most likely accidental bySzewczuk et al. (2014). In the present work, we analyze the 8 modes in depthwith the $\chi^2$-matching method. Based on the best fitting model (model MA),we find that they can be well explained as a sequences of consecutive dipolar$(l,~m)=(1,~0)$. The period discrepancies between observations and the bestfitting model are within 100 s except for the outlier which is up to 300 s.Based on the calculated CMMs, we find that, for pure g-mode oscillations, thebuoyancy radius $\Lambda_{0}$ can be precisely measured with the$\chi^2$-matching method between observations and calculations. It representsthe "Propagation time" of the g-mode from stellar surface to center. It is of$\Lambda_{0}=245.78\pm0.59~\mu$Hz with a precision of 0.24\%. In addition, wealso find that HD 50230 is a metal-rich ($Z_{\rm init}=0.034-0.043$) star witha mass of $M=6.15-6.27~{\rm M_{\odot}}$. It is still located onhydrogen-burning phase with central hydrogen $X_{\rm C}=0.298-0.316$ (or$X_{\rm C}=0.306^{+0.010}_{-0.008}$), therefore has a convective core with aradius of $R_{\rm cc}=0.525-0.536~{\rm R_{\odot}}$ (or $R_{\rmcc}=0.531^{+0.005}_{-0.006}~{\rm R_{\odot}}$). In order to well interpret thestructure of observed period spacing pattern, the convective core overshooting($f_{\rm ov}=0.0175-0.0200$) and the extra diffusion mixing ($\log D_{\rmmix}=3.7-3.9$) should be taken into account in theoretical models.

High-precision asteroseismology in Slowly Pulsating B star: HD 50230