Nanostructure forming in soft magnetic Fe-P-Si-Mn-V and Fe-P-Si-Mn-V-C alloys upon annealing

Аносова, М. О.; Baldokhin, Yu. V.; Vavilova, V. V.; Korneev, V. P.; Palii, N. A.

doi:10.1134/s0036029511030037

Cited by 8 publications

(11 citation statements)

References 6 publications

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“…This is qualitatively the same as the results presented in Fig. 1 of Anosova & Orlov (1992). However, the systems in S 1 generally have a significantly hierarchical configuration, as is manifested by the obvious overdensity of the systems in S 1 near the point (0.5, 0).…”

Section: Characteristics Of Initial Systems With An Escape Detected Bsupporting

confidence: 87%

“…This reveals the fact that M903P is significantly more efficient in detecting escape systems with hierarchical configuration than those with non-hierarchical configuration. We know that, as an easy consequence of the energy integral, such a configuration is inevitable for any unbounded 3-body system with negative total energy, but, as is well known, it is also typical among systems with very long lifetime T L 1000τ c (e.g., Anosova & Orlov 1992). This is of practical interest because hierarchical configuration is typical among real triple stars (see the next section for further discussion).…”

Section: Characteristics Of Initial Systems With An Escape Detected Bmentioning

confidence: 92%

“…All of the systems mentioned in this section are randomly constructed using the process and the unit system described below (Agekian & Anosova 1967, 1968Anosova 1986Anosova , 1990Anosova & Orlov 1992).…”

Section: Sampling Systems and Aarseth's 3-body Codementioning

confidence: 99%

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Adapting Marchal's test of escape to real triple stars

Fu²,

Sun

2009

A&A

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Context. For a general N-body system, Marchal constructed an analytical test of escape, which uses only a one-dimensional projected motion state of the system at any given instant. This test is well adapted to identifying real, disintegrating small stellar systems, of which the full motion states are generally unavailable. However, to our knowledge, there has been no practical application of this test until the present-day. Aims. In this paper, we aim at adapting the above test to visual triple stars with estimable component masses and known kinematic data on the plane perpendicular to the line-of-sight. As illustrating examples, our goal is to identify disintegrating Hipparcos linear triple systems. Methods. The fundamental techniques of analytical geometry were used to adapt the test of escape to practical applications, and the Monte Carlo method used to cope with the unavoidable observational errors, so that the confidence probability of a real triple star disintegrating could be obtained. Results. A practical algorithm was designed to make full use of the two-dimensional kinematic data in testing usual visual triple stars. This algorithm is then applied to 24 Hipparcos linear triple systems with estimable component masses and the disintegration probability given. Conclusions.

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Section: Characteristics Of Initial Systems With An Escape Detected Bsupporting

confidence: 87%

Section: Characteristics Of Initial Systems With An Escape Detected Bmentioning

confidence: 92%

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Adapting Marchal's test of escape to real triple stars

Fu²,

Sun

2009

A&A

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“…The factor C(L) is needed to account for the fact that the lifetime of the system depends on the total angular momentum L (e.g. Valtonen 1974;Anosova & Orlov 1986). If we take q to be the physical sizes of the objects involved in the encounter, then equation (1) gives the collision probability for a resonant 1+2 interaction.…”

Section: Collision Probability For N =mentioning

confidence: 99%

Small-N collisional dynamics: pushing into the realm of not-so-small N

Leigh

Geller

2012

Monthly Notices of the Royal Astronomical Society

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In this paper, we study small‐N gravitational dynamics involving up to six objects. We perform a large suite of numerical scattering experiments involving single, binary and triple stars. This is done using the fewbody numerical scattering code, which we have upgraded to treat encounters involving triple stars. We focus on outcomes that result in direct physical collisions between stars, within the low angular momentum and high absolute orbital energy regime. The dependence of the collision probability on the number of objects involved in the interaction, N, is found for fixed total energy and angular momentum. Our results are consistent with a collision probability that increases approximately as N2. Interestingly, this is also what is expected from the mean free path approximation in the limit of very large N. A more thorough exploration of parameter space will be required in future studies to fully explore this potentially intriguing connection. This study is meant as a first step in an ongoing effort to extend our understanding of small‐N collisional dynamics beyond the three‐ and four‐body problems and into the realm of larger N.

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“…The system typically evolves via a series of close triple encounters (e.g. Anosova 1969;Szebehely 1972;Saslaw, Valtonen & Aarseth 1974;Valtonen 1975;Agekyan & Anosova 1983;Anosova & Orlov 1983, ⋆ E-mail: nleigh@amnh.org (NWCL), mshara@amnh.org, a-geller@northwestern.edu 1986,1994). Between each such event, one of the objects is temporarily ejected but remains bound to the three-body system.…”

Section: Introductionmentioning

confidence: 99%

When does a star cluster become a multiple star system? – I. Lifetimes of equal-mass small-Nsystems

Leigh

Shara

Geller

2016

Mon. Not. R. Astron. Soc.

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What is the difference between a long-lived unstable (or quasi-stable) multiple star system and a bona fide star cluster? In this paper, we present a possible framework to address this question, by studying the distributions of disruption times for chaotic gravitational encounters as a function of the number of interacting particles. To this end, we perform a series of numerical scattering experiments with the FEWBODY code, to calculate the distributions of disruption times as a function of both the particle number N and the virial coefficient k. The subsequent distributions are fit with a physically-motivated function, consisting of an initial exponential decay followed by a very slowly decreasing tail at long encounter times due to long-lived quasi-stable encounters. We find three primary features characteristic of the calculated distributions of disruption times. These are: (1) the system half-life increases with increasing particle number, (2) the fraction of long-lived quasi-stable encounters increases with increasing particle number and (3) both the system half-life and the fraction of quasistable encounters increase with decreasing virial coefficient. We discuss the significance of our results for collisional dynamics, and consider the extrapolation of our results to larger-N systems. We suggest that this could potentially offer a clear and unambiguous distinction between star clusters and (unstable or quasi-stable) multiple star systems. Although we are limited by very small-number statistics, our results tentatively suggest that (for our assumptions) this transition occurs at a critical particle number of order 100.

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Nanostructure forming in soft magnetic Fe-P-Si-Mn-V and Fe-P-Si-Mn-V-C alloys upon annealing

Cited by 8 publications

References 6 publications

Adapting Marchal's test of escape to real triple stars

Adapting Marchal's test of escape to real triple stars

Small-N collisional dynamics: pushing into the realm of not-so-small N

When does a star cluster become a multiple star system? – I. Lifetimes of equal-mass small-Nsystems

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