Catálogo de publicaciones - revistas

Compartir en
redes sociales

Título de Acceso Abierto

The Astrophysical Journal (ApJ)

Resumen/Descripción – provisto por la editorial en inglés

The Astrophysical Journal is an open access journal devoted to recent developments, discoveries, and theories in astronomy and astrophysics. Publications in ApJ constitute significant new research that is directly relevant to astrophysical applications, whether based on observational results or on theoretical insights or modeling.

Palabras clave – provistas por la editorial

astronomy; astrophysics

Disponibilidad

Institución detectada	Período	Navegá	Descargá	Solicitá
No detectada	desde jul. 1995 / hasta dic. 2023	IOPScience

Información

Tipo de recurso:

revistas

ISSN impreso

0004-637X

ISSN electrónico

1538-4357

Editor responsable

American Astronomical Society (AAS)

Idiomas de la publicación

inglés

País de edición

Reino Unido

Información sobre licencias CC

https://creativecommons.org/licenses/by/4.0/

Cobertura temática

Ciencias físicas

Tabla de contenidos

doi: 10.3847/1538-4357/ab2ad8

High-precision Asteroseismology in a Slowly Pulsating B Star: HD 50230

Tao Wu; Yan Li

<jats:title>Abstract</jats:title> <jats:p>The slowly pulsating B star HD 50230, which is in fact a hybrid B-type pulsator, has been observed by <jats:italic>CoRoT</jats:italic> for at least 137 days. Nearly equidistant period spacing patterns are found among eight modes that are extracted from the oscillation spectrum with more than 500 frequencies. However, it is thought to be most likely accidental by Szewczuk et al. In the present work, we analyze the eight modes in depth with the <jats:italic>χ</jats:italic> <jats:sup>2</jats:sup>-matching method. Based on the best-fitting model (model MA), we find that they can be well explained as sequences of consecutive dipolar (<jats:italic>l</jats:italic>, <jats:italic>m</jats:italic>) = (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 <jats:italic>χ</jats:italic> <jats:sup>2</jats:sup>-minimization models, we find that, for pure g-mode oscillations, the buoyancy radius, Λ<jats:sub>0</jats:sub>, can be precisely measured with the <jats:italic>χ</jats:italic> <jats:sup>2</jats:sup>-matching method between observations and calculations. It represents the “propagation time” of the g-mode from the stellar surface to the center. It is of Λ<jats:sub>0</jats:sub> = 245.78 ± 0.59 <jats:italic>μ</jats:italic>Hz with a precision of 0.24%. In addition, we also find that HD 50230 is a metal-rich (<jats:italic>Z</jats:italic> <jats:sub>init</jats:sub> = 0.034–0.043) star with a mass of <jats:italic>M</jats:italic> = 6.15–6.27 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>. It is still located in the hydrogen-burning phase with central hydrogen of <jats:italic>X</jats:italic> <jats:sub>C</jats:sub> = 0.298–0.316 (or <jats:inline-formula> <jats:tex-math> <?CDATA ${X}_{{\rm{C}}}={0.306}_{-0.008}^{+0.010}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab2ad8ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>); therefore, it has a convective core with a radius of <jats:italic>R</jats:italic> <jats:sub>cc</jats:sub> = 0.525–0.536 <jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub> (or <jats:inline-formula> <jats:tex-math> <?CDATA ${R}_{\mathrm{cc}}={0.531}_{-0.006}^{+0.005}\,{R}_{\odot }$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab2ad8ieqn2.gif" xlink:type="simple" /> </jats:inline-formula>). In order to interpret the structure of the observed period spacing pattern well, the convective core overshooting (<jats:italic>f</jats:italic> <jats:sub>ov</jats:sub> = 0.0175–0.0200) and the extra diffusion mixing (<jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}\,{D}_{\mathrm{mix}}=3.7\mbox{--}3.9$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab2ad8ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>) should be taken into account in theoretical models.</jats:p>