High-precision asteroseismology in Slowly Pulsating B star: HD 50230. (arXiv:1907.04968v1 [astro-ph.SR])

<a href="http://arxiv.org/find/astro-ph/1/au:+Wu_T/0/1/0/all/0/1">Tao Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Yan Li</a>

SPB star HD 50230, in fact a hybrid B-type pulsator, has been observed by

CoRoT least 137 days. A nearly equidistant period spacing pattern are found

among 8 modes which are extracted from the oscillation spectrum with more than

500 frequencies. However, it is thought to be most likely accidental by

Szewczuk et al. (2014). In the present work, we analyze the 8 modes in depth

with 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 best

fitting 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, the

buoyancy radius $Lambda_{0}$ can be precisely measured with the

$chi^2$-matching method between observations and calculations. It represents

the “Propagation time” of the g-mode from stellar surface to center. It is of

$Lambda_{0}=245.78pm0.59~mu$Hz with a precision of 0.24%. In addition, we

also find that HD 50230 is a metal-rich ($Z_{rm init}=0.034-0.043$) star with

a mass of $M=6.15-6.27~{rm M_{odot}}$. It is still located on

hydrogen-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 a

radius of $R_{rm cc}=0.525-0.536~{rm R_{odot}}$ (or $R_{rm

cc}=0.531^{+0.005}_{-0.006}~{rm R_{odot}}$). In order to well interpret the

structure of observed period spacing pattern, the convective core overshooting

($f_{rm ov}=0.0175-0.0200$) and the extra diffusion mixing ($log D_{rm

mix}=3.7-3.9$) should be taken into account in theoretical models.

SPB star HD 50230, in fact a hybrid B-type pulsator, has been observed by

CoRoT least 137 days. A nearly equidistant period spacing pattern are found

among 8 modes which are extracted from the oscillation spectrum with more than

500 frequencies. However, it is thought to be most likely accidental by

Szewczuk et al. (2014). In the present work, we analyze the 8 modes in depth

with 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 best

fitting 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, the

buoyancy radius $Lambda_{0}$ can be precisely measured with the

$chi^2$-matching method between observations and calculations. It represents

the “Propagation time” of the g-mode from stellar surface to center. It is of

$Lambda_{0}=245.78pm0.59~mu$Hz with a precision of 0.24%. In addition, we

also find that HD 50230 is a metal-rich ($Z_{rm init}=0.034-0.043$) star with

a mass of $M=6.15-6.27~{rm M_{odot}}$. It is still located on

hydrogen-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 a

radius of $R_{rm cc}=0.525-0.536~{rm R_{odot}}$ (or $R_{rm

cc}=0.531^{+0.005}_{-0.006}~{rm R_{odot}}$). In order to well interpret the

structure of observed period spacing pattern, the convective core overshooting

($f_{rm ov}=0.0175-0.0200$) and the extra diffusion mixing ($log D_{rm

mix}=3.7-3.9$) should be taken into account in theoretical models.

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