A method to deconvolve stellar rotational velocities

Michel Curé, Diego F. Rial, Alejandra Christen, Julia Cassetti

Research output: Contribution to journalArticlepeer-review

11 Scopus citations

Abstract

Aims. Rotational speed is an important physical parameter of stars, and knowing the distribution of stellar rotational velocities is essential for understanding stellar evolution. However, rotational speed cannot be measured directly and is instead the convolution between the rotational speed and the sine of the inclination angle v sin i. Methods. We developed a method to deconvolve this inverse problem and obtain the cumulative distribution function for stellar rotational velocities extending the work of Chandrasekhar & Münch (1950, ApJ, 111, 142) Results. This method is applied: a) to theoretical synthetic data recovering the original velocity distribution with a very small error; and b) to a sample of about 12.000 field main-sequence stars, corroborating that the velocity distribution function is non-Maxwellian, but is better described by distributions based on the concept of maximum entropy, such as Tsallis or Kaniadakis distribution functions. Conclusions. This is a very robust and novel method that deconvolves the rotational velocity cumulative distribution function from a sample of v sin i data in a single step without needing any convergence criteria.

Original languageEnglish
Article numberA85
JournalAstronomy and Astrophysics
Volume565
DOIs
StatePublished - May 2014
Externally publishedYes

Keywords

  • Methods:analytical
  • Methods:data analysis
  • Methods:numerical
  • Methods:statistical
  • Stars:fundamental parameters
  • Stars:rotation

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