Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-19T05:34:48.470Z Has data issue: false hasContentIssue false
  • English
  • Français

Modelling Magnetar Behaviour with 3D Magnetothermal Simulations

Published online by Cambridge University Press:  27 February 2023

Davide De Grandis Open the ORCID record for Davide De Grandis [Opens in a new window] ,
Roberto Turolla ,
Roberto Taverna Open the ORCID record for Roberto Taverna [Opens in a new window] ,
Toby S. Wood  and
Silvia Zane
Davide De Grandis*
Affiliation:
Department of Physics and Astronomy, University of Padova, via Marzolo 8, I-35131 Padova, Italy Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Surrey, RH5 6NT, United Kingdom
Roberto Turolla
Affiliation:
Department of Physics and Astronomy, University of Padova, via Marzolo 8, I-35131 Padova, Italy Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Surrey, RH5 6NT, United Kingdom
Roberto Taverna
Affiliation:
Department of Physics and Astronomy, University of Padova, via Marzolo 8, I-35131 Padova, Italy
Toby S. Wood
Affiliation:
School of Mathematics and Statistics, Newcastle University, Newcastle upon Tyne, NE1 7RU, United Kingdom
Silvia Zane
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Surrey, RH5 6NT, United Kingdom
*
*email: [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.

The observational properties of isolated NSs are shaped by their magnetic field and surface temperature. They evolve in a strongly coupled fashion, and modelling them is key in understanding the emission properties of NSs. Much effort was put in tackling this problem in the past but only recently a suitable 3D numerical framework was developed. We present a set of 3D simulations addressing both the long-term evolution (≈ 104–106 yrs) and short-lived outbursts (≲ 1 yr). Not only a 3D approach allows one to test complex field geometries, but it is absolutely key to model magnetar outbursts, which observations associate to the appearance of small, inherently asymmetric hot regions. Even though the mechanism that triggers these phenomena is not completely understood, following the evolution of a localised heat injection in the crust serves as a model to study the unfolding of the event.

Keywords

neutron starsmagnetic fieldsnumerical methods
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 280 - 283
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Beznogov, M. V., Potekhin, A. Y., Yakovlev, D. G. 2001, Phys. Rep., 919:1–68. doi: 10.1016/j.physrep.2021.03.004.CrossRefGoogle Scholar
Coti Zelati, F., Rea, N., Pons, J. A., Campana, S., Esposito, P. 2018, MNRAS, 474(1):961–1017. doi: 10.1093/mnras/stx2679.CrossRefGoogle Scholar
De Grandis, D., Turolla, R., Wood, T. S., Zane, S., Taverna, R., Gourgouliatos, K. N. 2020, ApJ 903(1):40. doi: 10.3847/1538-4357/abb6f9.CrossRefGoogle Scholar
De Grandis, D., Taverna, R., Turolla, R., Gnarini, A., Popov, S. B., Zane, S., Wood, T. S. 2021, ApJ 914(2):118. doi: 10.3847/1538-4357/abfdac.CrossRefGoogle Scholar
Gourgouliatos, K, N., Cumming, A. 2014, Phys. Rev. Lett., 112(17):171101. doi: 10.1103/PhysRevLett.112.171101.CrossRefGoogle Scholar
Taverna, R., Turolla, R., Gonzalez Caniulef, D., Zane, S., Muleri, F., Soffitta, P. 2015, MNRAS, 454(3):3254–3266. doi: 10.1093/mnras/stv2168.CrossRefGoogle Scholar
Wood, T. S., Hollerbach, R. 2015, Phys. Rev. Lett., 114(19):191101. doi: 10.1103/PhysRevLett.114.191101.CrossRefGoogle Scholar
Yakovlev, D. G., Kaminker, A. D., Gnedin, O. Y., Haensel, P. 2001, Phys. Rep. 354(1-2):1–155. doi: 10.1016/S0370-1573(00)00131-9.CrossRefGoogle Scholar
Yakovlev, D. G., Kaminker, A. D., Potekhin, A. Y., Haensel, P. 2021 MNRAS 500(4):4491–4505. doi: 10.1093/mnras/staa3547.CrossRefGoogle Scholar