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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/ab93d0

Early Evolution of Disk, Outflow, and Magnetic Field of Young Stellar Objects: Impact of Dust Model

Y. Tsukamoto; M. N. Machida; H. Susa; H. Nomura; S. Inutsuka

<jats:title>Abstract</jats:title> <jats:p>The formation and early evolution of low-mass young stellar objects (YSOs) are investigated using three-dimensional non-ideal magnetohydrodynamics simulations. We investigate the evolution of YSOs up to <jats:inline-formula> <jats:tex-math> <?CDATA $\sim {10}^{4}\,\mathrm{yr}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab93d0ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> after protostar formation, at which protostellar mass reaches <jats:inline-formula> <jats:tex-math> <?CDATA $\sim 0.1{M}_{\odot }$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab93d0ieqn2.gif" xlink:type="simple" /> </jats:inline-formula>. We particularly focus on the impact of the dust model on the evolution. We found that a circumstellar disk is formed in all simulations, regardless of the dust model. Disk size is approximately 10 au at the protostar formation epoch, and it increases to several tens of au at <jats:inline-formula> <jats:tex-math> <?CDATA $\sim {10}^{4}\,\mathrm{yr}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab93d0ieqn3.gif" xlink:type="simple" /> </jats:inline-formula> after protostar formation. The disk mass is comparable to the central protostellar mass, and gravitational instability develops. In simulations with small dust sizes, the warp of the pseudodisk develops <jats:inline-formula> <jats:tex-math> <?CDATA $\sim {10}^{4}\,\mathrm{yr}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab93d0ieqn4.gif" xlink:type="simple" /> </jats:inline-formula> after protostar formation. The warp strengthens magnetic braking in the disk and decreases disk size. Ion-neutral drift can occur in the infalling envelope when the typical dust size is <jats:inline-formula> <jats:tex-math> <?CDATA $a\gtrsim 0.2\,\mu {\rm{m}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab93d0ieqn5.gif" xlink:type="simple" /> </jats:inline-formula> and the protostar (plus disk) mass is <jats:inline-formula> <jats:tex-math> <?CDATA $M\gtrsim 0.1{M}_{\odot }$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab93d0ieqn6.gif" xlink:type="simple" /> </jats:inline-formula>. The outflow activity is anticorrelated to the dust size, and the strong outflow appears with small dust grains.</jats:p>