Period distributions in pulsating and binary stars

Quiroga, R. J.; Mello, J. C.

doi:10.1007/bf00643204

Cited by 2 publications

(3 citation statements)

References 10 publications

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“…To check the constancy of αβ Newt by using realistic stellar models, Claret & Giménez (1989) provided values of α and β for several grids of stellar evolutionary models. The availability of these formfactors allowed deeper investigations into the Jacobi dynamics of stellar evolution (Quiroga & Claret 1992a,b;Quiroga & Mello 1992;Quiroga & Cerqueira 1992). Unfortunately, due to limitations in the opacity tables available at that time, these stellar models only covered the pre main-sequence (PMS), the main sequence and only the first stages of the red giant branch.…”

Section: Introductionmentioning

confidence: 99%

The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II.

Claret

Hempel

2013

A&A

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Context. The Jacobi virial equation is a very powerful tool for exploring several aspects of the stellar internal structure and evolution. In a previous paper we have shown that the function αβ GR /Λ 0.9 (R) is constant (≈0.4) for pre main-sequence stars (PMS), white dwarfs (WD) and for some neutron star (NS) models, where α GR and β GR are the form-factors of the gravitational potential energy and of the moment of inertia. Aims. To investigate the structural evolution of another type of celestial bodies, we extend these calculations to gaseous planets. We also analyse the cases for which this function is not conserved during some stellar evolutionary phases. Concerning NS, we study the influence of the equation of state (EOS) on this function and refine the exponent of the auxiliary function Λ(R). We also present a macroscopic criterion of stability for these stars. Methods. Non-stop calculations from the PMS to the white dwarf cooling sequences were performed with the MESA code. The covered mass range was 0.1-1.7 M . We used the same code to compute models for gaseous planets with masses between 0.1-50 M J . Neutron star models were computed using two codes. The first one is a modified version of the NSCool/TOV subroutines. The second code is a plain TOV solver that allows one to use seven previously described EOS. The relativistic moment of inertia and gravitational potential energy were computed through a fourth-order Runge-Kutta method. Results. By analysing the internal structure of gaseous planets we show that the function αβ GR /Λ 0.8 (R) ≡ Γ(M, EOS) is conserved for all models during the whole planetary evolution and is independent of the planet mass. For the PMS to the white dwarf cooling sequences, we have found a connection between the strong variations of Γ(M, EOS) during the intermediary evolutionary phases and the specific nuclear power. A threshold for the specific nuclear power was found. Below this limit this function is invariant (≈0.4) for these models, i.e., at the initial and final stages (PMS and WD). For NS, we showed that the function Γ(M, EOS) is also invariant (≈0.4) and is independent of the EOS and of the stellar mass. Therefore, we confirm that regardless of the final products of the stellar evolution, NS or WD, they recover the initial value of Γ(M, EOS) ≈ 0.4 acquired at the PMS. Finally, we have introduced a macroscopic stability criterion for NS models based on the properties of the relativistic product αβ GR .

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Section: Introductionmentioning

confidence: 99%

The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II.

Claret

Hempel

2013

A&A

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“…На сегодняшний день подавляющее большинство работ, направленных на изучение особенностей распределений орбит малых тел Солнечной системы в пространстве возможных орбит, базируется на построении гистограмм численности (или же вероятности) по выбранному параметру [1][2][3][4]. Данный метод интуитив-но понятен и имеет свои преимущества, позволившие в свое время сделать ряд открытий, например, наличие люков Кирквуда в главном поясе астероидов и других особенностей, вызванных резонансными явлениями и соизмеримостями.…”

Section: Introductionunclassified

“…Данный метод интуитив-но понятен и имеет свои преимущества, позволившие в свое время сделать ряд открытий, например, наличие люков Кирквуда в главном поясе астероидов и других особенностей, вызванных резонансными явлениями и соизмеримостями. Более того, применив простые преобразования (удаление тренда, исключение нестационарных участков), можно получить остаточный ряд, который, согласно некоторым теориям и гипотезам [2][3][4], ISSN 2226-3780 должен содержать периодические составляющие на фоне шумов, что легко проверить, применив к данному ряду хорошо разработанные методы спектрального анализа равномерных рядов [5][6][7][8][9]. Под равномерностью ряда следует понимать то, что отсчеты его значений по изучаемому параметру делаются с одним и тем же шагом.…”

Section: Introductionunclassified

Spectral analysis of asteroids distribution on semimajor axis. LS-method

Черкас¹,

Kolomiets²,

Волощук³

2013

TAPR

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Розроблено математичний апарат для визначення напруженості електростатичних полів у багатошарових наночастинках. Це дає можливість визначити енергію, яка виділяється при дії лазерного випромінювання і може бути використано для лікування онкологічних захворювань.

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Period distributions in pulsating and binary stars

Cited by 2 publications

References 10 publications

The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II.

The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II.

Spectral analysis of asteroids distribution on semimajor axis. LS-method

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