Hostname: page-component-586b7cd67f-dsjbd Total loading time: 0 Render date: 2024-11-23T17:46:21.899Z Has data issue: false hasContentIssue false
  • English
  • Français

Reversibility of Turbulent and Non-Collisional Plasmas: Solar Wind

Published online by Cambridge University Press:  24 September 2020

Belén Acosta Open the ORCID record for Belén Acosta [Opens in a new window] ,
Denisse Pastén Open the ORCID record for Denisse Pastén [Opens in a new window]  and
Pablo S. Moya Open the ORCID record for Pablo S. Moya [Opens in a new window]
Belén Acosta
Affiliation:
Departamento de Física, Facultad de Ciencias, Universidad de Chile, Las Palmeras 3425, Ñuñoa, Santiago emails: [email protected], [email protected], [email protected]
Denisse Pastén
Affiliation:
Departamento de Física, Facultad de Ciencias, Universidad de Chile, Las Palmeras 3425, Ñuñoa, Santiago emails: [email protected], [email protected], [email protected]
Pablo S. Moya
Affiliation:
Departamento de Física, Facultad de Ciencias, Universidad de Chile, Las Palmeras 3425, Ñuñoa, Santiago emails: [email protected], [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have studied turbulent plasma as a complex system applying the method known as Horizontal Visibility Graph (HVG) to obtain the Kullback-Leibler Divergence (KLD) as a first approach to characterize the reversibility of the time series of the magnetic fluctuations. For this, we have developed the method on Particle In Cell (PIC) simulations for a magnetized plasma and on solar wind magnetic time series, considering slow and fast wind. Our numerical results show that low irreversibility values are verified for magnetic field time series associated with Maxwellian distributions. In addition, considering the solar wind plasma, our preliminary results seem to indicate that greater irreversibility degrees are reached by the magnetic field associated with slow solar wind.

Keywords

Plasmasturbulencemethods: statistical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 363 - 366
Copyright
© International Astronomical Union 2020

References

Feldman, W.C., Asbridge, J.R., Bame, S.J., Gosling, J.T., 1976, J. Geophys. Res. 81, 5054.CrossRefGoogle Scholar
Krieger, A.S., Timothy, A.F., Roelof, E.C., 1973, Solar Phys. 29, 505.CrossRefGoogle Scholar
Lacasa, L., A. Nuñez, É. Roldán, J.M.R. Parrondo & B., Luque, 2012, Eur. Phys. J. B, 85: 217.CrossRefGoogle Scholar
Suyal, V., A., Prasad & H.P., Singh, 2014, Solar Phys, 289, 379–389.CrossRefGoogle Scholar
Thomas, J.A., & T.M., Cover, 2006, Elements of Information Theory, 2 ed., 19.Google Scholar
Viñas, A.F., P.S., Moya, R., Navarro, & J., Araneda, 2014, Phys. Plasmas, 21, 012902.CrossRefGoogle Scholar
Woo, R., Martin, J.M., 1997, Geophys. Res. Lett. 20, 2535.CrossRefGoogle Scholar