Hydrodynamic processes of angular momentum transport in the interior of a rotating massive hydrogen-burning star

Staritsin, E. I.

doi:10.1134/s106377370702003x

Cited by 9 publications

(17 citation statements)

References 7 publications

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“…The flux of hydrogen from the radiative turbulent envelope into the convective core has its maximum in the second half of the star's evolution along the main sequence [25]. The intensity of hydrodynamic transport processes in the non-convective layers of a star is determined by the momentum and Schmidt number in the turbulent radiative envelope [25,26], and can be different for stars of the same mass. For example, the mass of the chemically homogeneous region in the central part of the star during the second half of its main-sequence evolution is determined by the combined action of turbulent entrainment and shear turbulence, and can be different for stars of the same mass.…”

Section: Results Of the Computationsmentioning

confidence: 99%

Turbulent entrainment at the boundaries of the convective cores of main-sequence stars

Staritsin

2013

Astron. Rep.

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Abstract-Extra mixing of matter in stellar interiors at the boundaries of the convective cores of mainsequence stars is considered for the first time using the physical model of turbulent entrainment developed by Arnett and collaborators based on three-dimensional hydrodynamical simulations. The model takes into account the energy that goes into mixing the matter of the convective core and layers stable against convection located above the core. It is shown that the extent of the region of extra mixing expressed in units of the pressure scale height is not constant, and decreases as the star evolves along the main sequence. Adequate allowance for extra mixing at the boundaries of convective cores is necessary to clarify the relative importance of different mixing mechanisms in stellar interiors, as well as to determine stellar parameters using asteroseismlogy.

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Section: Results Of the Computationsmentioning

confidence: 99%

Turbulent entrainment at the boundaries of the convective cores of main-sequence stars

Staritsin

2013

Astron. Rep.

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“…The evolution of an isolated star with a mass of 16 M ⊙ and an angular momentum J in the range 0.92 × 10 52 − 3.69 × 10 52 erg • s was studied on the main sequence (Staritsin 2007). The inner part of a star with a mass of 10.7 M ⊙ contains 47% of the angular momentum of the star at J = 0.92×10 52 erg•s and 34% at J = 3.69 × 10 52 erg • s, when the hydrogen content in the convective core is the same as in the accretor.…”

Section: Discussionmentioning

confidence: 99%

“…Turbulent viscosity coefficients have been determined by Talon and Zahn (1997), Maeder (2003), and Mathis et al (2004). Equations ( 3) and ( 4) are solved along with equations of stellar structure and evolution (Staritsin 1999(Staritsin , 2005(Staritsin , 2007(Staritsin , 2014.…”

Section: Angular Momentum Transfer In the Accretormentioning

confidence: 99%

The Spin-up of a Star Gaining Mass in a Close Binary System on the Thermal Time Scale

Staritsin¹

2022

Res. Astron. Astrophys.

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We investigate the exchange of mass in a binary system as a channel through which a Be star can receive a rapid rotation. The mass-transfer phase in a massive close binary system in the Hertzsprung-gap is accompanied by the spinning up of the accreting component. We consider a case when the mass of the accreting component increases by 1.5 times. The component acquires mass and angular momentum while in a state of critical rotation. The angular momentum of the component increases by 50 times. Meridional circulation effectively transports angular momentum inside the component during the mass-transfer phase and during the thermal time scale after the end of the mass-transfer phase. As a result of mass transfer, the component acquires the rotation typical of classical Be stars.

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“…To solve Eq. ( 6), a difference scheme based on the integrointerpolation method (Samarskij & Popov 1992) was elaborated (Staritsin 1999(Staritsin , 2005(Staritsin , 2007. The method implies an integration of Eq.…”

Section: Transport Of Angular Momentummentioning

confidence: 99%

“…Be type stars exhibit the following properties: emission in the Balmer lines of hydrogen, excess radiation in the infrared part of the spectrum, and rapid rotation (Porter & Rivinius 2003). There are several channels by which a Be star can acquire a fast rotation: the process of star birth, the removal of angular momentum from the interior of an isolated star to the exterior during evolution along the main sequence (Meynet & Maeder 2005;Staritsin 2007Staritsin , 2009Ekstrom et al 2008;Granada & Haemmerle 2014;Gagnier et al 2019), mass and angular momentum exchange in a binary system in the Hertzsprung gap (Pols et al 1991;Portegies Zwart 1995;Van Bever & Vanbeveren 1997), or the merging of a pair of main sequence stars (Shao & Li 2014).…”

Section: Introductionmentioning

confidence: 99%

Asymmetric misfit nanotubes: Chemical affinity outwits the entropy at high-temperature solid-state reactions

Sreedhara

Hettler

Kaplan‐Ashiri

et al. 2021

Proc. Natl. Acad. Sci. U.S.A.

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Asymmetric two-dimensional (2D) structures (often named Janus), like SeMoS and their nanotubes, have tremendous scope in material chemistry, nanophotonics, and nanoelectronics due to a lack of inversion symmetry and time-reversal symmetry. The synthesis of these structures is fundamentally difficult owing to the entropy-driven randomized distribution of chalcogens. Indeed, no Janus nanotubes were experimentally prepared, so far. Serendipitously, a family of asymmetric misfit layer superstructures (tubes and flakes), including LaX-TaX2 (where X = S/Se), were synthesized by high-temperature chemical vapor transport reaction in which the Se binds exclusively to the Ta atoms and La binds to S atoms rather than the anticipated random distribution. With increasing Se concentration, the LaS-TaX2 misfit structure gradually transformed into a new LaS-TaSe2-TaSe2 superstructure. No misfit structures were found for xSe = 1. These counterintuitive results shed light on the chemical selectivity and stability of misfit compounds and 2D alloys, in general. The lack of inversion symmetry in these asymmetric compounds induces very large local electrical dipoles. The loss of inversion and time-reversal symmetries in the chiral nanotubes offers intriguing physical observations and applications.

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Hydrodynamic processes of angular momentum transport in the interior of a rotating massive hydrogen-burning star

Cited by 9 publications

References 7 publications

Turbulent entrainment at the boundaries of the convective cores of main-sequence stars

Turbulent entrainment at the boundaries of the convective cores of main-sequence stars

The Spin-up of a Star Gaining Mass in a Close Binary System on the Thermal Time Scale

Asymmetric misfit nanotubes: Chemical affinity outwits the entropy at high-temperature solid-state reactions

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