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Modelling the radio pulses of an ultracool dwarf

Yu, S. and Hallinan, G. and Doyle, J. G. and MacKinnon, A. L. and Antonova, A. and Kuznetsov, A. and Golden, A. and Zhang, Z. H. (2011) Modelling the radio pulses of an ultracool dwarf. Astronomy and Astrophysics, 525 . Art. No. A39. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20140205-153242329

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Abstract

Context. Recently, unanticipated magnetic activity in ultracool dwarfs (UCDs, spectral classes later than M7) has emerged from a number of radio observations. The highly (up to 100%) circularly polarized nature and high brightness temperature of the emission have been interpreted as requiring an effective amplification mechanism of the high-frequency electromagnetic waves − the electron cyclotron maser instability (ECMI). Aims. We aim to understand the magnetic topology and the properties of the radio emitting region and associated plasmas in these ultracool dwarfs, interpreting the origin of radio pulses and their radiation mechanism. Methods. An active region model was built, based on the rotation of the UCD and the ECMI mechanism. Results. The high degree of variability in the brightness and the diverse profile of pulses can be interpreted in terms of a large-scale hot active region with extended magnetic structure existing in the magnetosphere of TVLM 513-46546. We suggest the time profile of the radio light curve is in the form of power law in the model. Combining the analysis of the data and our simulation, we can determine the loss-cone electrons have a density in the range of 1.25 × 10^(5)−5 × 10^5 cm^-3 and temperature between 10^7 and 5 × 10^7 K. The active region has a size <1 R_Jup, while the pulses produced by the ECMI mechanism are from a much more compact region (e.g. ~0.007 R_Jup). A surface magnetic field strength of ≈7000 G is predicted. Conclusions. The active region model is applied to the radio emission from TVLM 513-46546, in which the ECMI mechanism is responsible for the radio bursts from the magnetic tubes and the rotation of the dwarf can modulate the integral of flux with respect to time. The radio emitting region consists of complicated substructures. With this model, we can determine the nature (e.g. size, temperature, density) of the radio emitting region and plasma. The magnetic topology can also be constrained. We compare our predicted X-ray flux with Chandra X-ray observation of TVLM 513-46546. Although the X-ray detection is only marginally significant, our predicted flux is significantly lower than the observed flux. Further multi-wavelength observations will help us better understand the magnetic field structure and plasma behavior on the ultracool dwarf.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201015580DOIArticle
http://www.aanda.org/articles/aa/abs/2011/01/aa15580-10/aa15580-10.htmlPublisherArticle
http://arxiv.org/abs/1009.1548arXivDiscussion Paper
Additional Information:© 2010 ESO. Article published by EDP Sciences. Received 13 August 2010; Accepted 8 September 2010. Published online 30 November 2010. The Armagh Observatory is supported by a grant from the Northern Ireland Dept. of Culture Arts and Leisure. G.H. and A.G. gratefully acknowledge the support of Science Foundation Ireland (grant No. 07/RFP/PHYF553). A.K., S.Y.U. & J.G.D. thank the Leverhulme Trust for support. AA gratefully acknowledges the support of the Scientific Research Fund of “St. Kl. Ohridski” University of Sofia (grant No. 80/2009 and 138/2010). A.L.M. & S.Y.U. thank M. Aschwanden for providing the quasi-linear diffusion code of ECMI. SYU thanks Gavin Ramsay for his comments and also thanks Eamon Scullion for discussions. We also thank the UK Science and Technology Facilities Council for support via a Visitor grant. We gratefully thank the referee for his/her suggestions and comments.
Funders:
Funding AgencyGrant Number
Northern Ireland Department of Culture, Arts and Leisure (DCAL)UNSPECIFIED
Science Foundation Ireland07/RFP/PHYF553
Leverhulme TrustUNSPECIFIED
University of Sofia Scientific Research Fund80/2009
University of Sofia Scientific Research Fund138/2010
Science and Technology Facilities Council (STFC) Visitor GrantUNSPECIFIED
Subject Keywords:magnetic fields; radio continuum: stars; stars: low-mass; brown dwarfs; polarization; masers
Record Number:CaltechAUTHORS:20140205-153242329
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140205-153242329
Official Citation:Modelling the radio pulses of an ultracool dwarf S. Yu, G. Hallinan, J. G. Doyle, A. L. MacKinnon, A. Antonova, A. Kuznetsov, A. Golden and Z. H. Zhang A&A 525 A39 (2011) DOI: http://dx.doi.org/10.1051/0004-6361/201015580
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43679
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:05 Feb 2014 23:55
Last Modified:05 Feb 2014 23:55

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