Tsallis maximum entropy distribution function for stellar rotational velocities in the Pleiades

Soares, B. B.; Carvalho, J. C.; Nascimento, J.-D. do; Medeiros, J. R. De

doi:10.1016/j.physa.2005.08.064

Cited by 16 publications

(32 citation statements)

References 30 publications

(29 reference statements)

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“…Nonextensivity was observed in the analysis of magnetic field at distant heliosphere associated to the solar wind observed by Voyager 1 and 2 (Burlaga & Viñas 2005;Burlaga & Ness 2009. The distribution of stellar rotational velocities in the Pleiades open cluster was found to be satisfactorily modeled by a q-Maxwellian distribution (Soares et al 2006). The problem of Jeans gravitational instability was considered according to nonextensive kinetic theory (Lima et al 2002).…”

Section: Nonextensive Statisticsmentioning

confidence: 97%

Nonextensive distributions of asteroid rotation periods and diameters

Betzler¹,

Borges

Novis³

2012

A&A

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Context. We investigate the distribution of asteroid rotation periods from different regions of the solar system and diameter distributions of near-Earth asteroids (NEAs). Aims. We aim to verify if nonextensive statistics satisfactorily describes the data. Methods. Light curve data were taken from the Planetary Database System (PDS) with Rel ≥ 2. We also considered the taxonomic class and region of the solar system. Data of NEA were taken from the Minor Planet Center. Results. The rotation periods of asteroids follow a q-Gaussian with q = 2.6 regardless of taxonomy, diameter, or region of the solar system of the object. The distribution of rotation periods is influenced by observational bias. The diameters of NEAs are described by a q-exponential with q = 1.3. According to this distribution, there are expected to be 994 ± 30 NEAs with diameters greater than 1 km.

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Section: Nonextensive Statisticsmentioning

confidence: 97%

Nonextensive distributions of asteroid rotation periods and diameters

Betzler¹,

Borges

Novis³

2012

A&A

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“…Although Deutsch (1970) claimed that the distribution of stellar rotational velocities follows a Maxwellian-Boltzmann law, a number of studies have shown a clear discrepancy between theory and observations, where observed distributions are not well fitted by a Gaussian or Maxwellian function (e.g., Wolff et al 1982;de Medeiros et al 1996). More recently, Soares et al (2006) have shown, based on an analysis of the rotation of low-mass stars in the Pleiades open cluster, that the question of the nature of the distribution of stellar rotational velocity is not simply a question of which mathematical function model is used. It depends on the statistical mechanics applied.…”

Section: Introductionmentioning

confidence: 99%

Non-Gaussian Statistics and Stellar Rotational Velocities of Main-Sequence Field Stars

Carvalho

Nascimento

Silva

et al. 2009

ApJ

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In this Letter, we study the observed distributions of rotational velocity in a sample of more than 16,000 nearby F and G dwarf stars, magnitude complete, and presenting high-precision V sin i measurements. We show that the velocity distributions cannot be fitted by a Maxwellian. In addition, an analysis based on both Tsallis and Kaniadakis power-law statistics is by far the most appropriate statistics and gives a very good fit. It is also shown that single and binary stars have similar rotational distributions. This is the first time, to our knowledge, that these two new statistics have been tested for the rotation of such a large sample of stars, pointing solidly to a solution of the puzzling problem of the function governing the distribution of stellar rotational velocity.

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“…The nature of the statistical laws controlling the distribution of different stellar physical parameters, in particular rotational and radial velocities, is not well established yet, in spite of a conventional practice which seeks explanations based on Gaussian and Maxwell-Boltzmann distribution or on analytical functions with no clear physical motivation. For instance, a preliminary study by Soares et al [1] shows that these functions cannot conveniently fit the observed distribution of projected rotational velocity of stars in the Pleiades stellar open cluster. In fact, the nature of such a distribution is better explained on the basis of a Tsallis maximum entropy distribution function.…”

Section: Introductionmentioning

confidence: 99%

“…Following the same procedure used by Soares et al [1] we study the behaviour of the distribution of radial velocity of stars located in 13 stellar open clusters. For such a purpose we have used the Tsallis Maximum Entropy distribution applied in the study of the observed rotational velocity distribution of the stars in the Pleiades cluster.…”

Section: Introductionmentioning

confidence: 99%