Bimodal brightness oscillations in models of young binary systems

T. V. Demidova, N. Ya. Sotnikova, V. P. Grinin

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Abstract

We consider a model for the cyclic activity of young binary stars that accrete matter from the remnants of a protostellar cloud. If the orbit of such a binary system is inclined at a small angle to the line of sight, then the streams of matter and the density waves excited in the circumbinary disk can screen the primary component of the binary from the observer. To study these phenomena by the SPH (smoothed particle hydrodynamics) method, we have computed grids of hydrodynamic models for binary systems based on which we have constructed the light curves as a function of the orbital phase. The main emphasis is on investigating the properties of the brightness oscillations. Therefore, the model parameters were varied within the following ranges: the component mass ratio q = M 2/M 1 = 0.2-0.5 and the eccentricity e = 0-0.7. The parameter that defined the binary viscosity was also varied. We adopted optical grain characteristics typical of circumstellar dust. Our computations have shown that bimodal oscillations
Original languageEnglish
Number of pages8
JournalAstronomy Letters
Volume36
Issue number6
DOIs
StatePublished - 2010

Keywords

  • young
  • binary systems
  • early accretion
  • hydrodynamics

Cite this

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title = "Bimodal brightness oscillations in models of young binary systems",
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Bimodal brightness oscillations in models of young binary systems. / Demidova, T. V.; Sotnikova, N. Ya.; Grinin, V. P.

In: Astronomy Letters, Vol. 36, No. 6, 2010.

Research output: Contribution to journalArticleResearchpeer-review

TY - JOUR

T1 - Bimodal brightness oscillations in models of young binary systems

AU - Demidova, T. V.

AU - Sotnikova, N. Ya.

AU - Grinin, V. P.

PY - 2010

Y1 - 2010

N2 - We consider a model for the cyclic activity of young binary stars that accrete matter from the remnants of a protostellar cloud. If the orbit of such a binary system is inclined at a small angle to the line of sight, then the streams of matter and the density waves excited in the circumbinary disk can screen the primary component of the binary from the observer. To study these phenomena by the SPH (smoothed particle hydrodynamics) method, we have computed grids of hydrodynamic models for binary systems based on which we have constructed the light curves as a function of the orbital phase. The main emphasis is on investigating the properties of the brightness oscillations. Therefore, the model parameters were varied within the following ranges: the component mass ratio q = M 2/M 1 = 0.2-0.5 and the eccentricity e = 0-0.7. The parameter that defined the binary viscosity was also varied. We adopted optical grain characteristics typical of circumstellar dust. Our computations have shown that bimodal oscillations

AB - We consider a model for the cyclic activity of young binary stars that accrete matter from the remnants of a protostellar cloud. If the orbit of such a binary system is inclined at a small angle to the line of sight, then the streams of matter and the density waves excited in the circumbinary disk can screen the primary component of the binary from the observer. To study these phenomena by the SPH (smoothed particle hydrodynamics) method, we have computed grids of hydrodynamic models for binary systems based on which we have constructed the light curves as a function of the orbital phase. The main emphasis is on investigating the properties of the brightness oscillations. Therefore, the model parameters were varied within the following ranges: the component mass ratio q = M 2/M 1 = 0.2-0.5 and the eccentricity e = 0-0.7. The parameter that defined the binary viscosity was also varied. We adopted optical grain characteristics typical of circumstellar dust. Our computations have shown that bimodal oscillations

KW - young

KW - binary systems

KW - early accretion

KW - hydrodynamics

U2 - 10.1134/S1063773710060058

DO - 10.1134/S1063773710060058

M3 - Article

VL - 36

JO - Astronomy Letters

JF - Astronomy Letters

SN - 1063-7737

IS - 6

ER -