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dc.contributor.authorAbbuhl, E.
dc.contributor.authorMutel, R.
dc.contributor.authorLynch, Christene
dc.contributor.authorGï Edel, M.
dc.identifier.citationAbbuhl, E. and Mutel, R. and Lynch, C. and Gï Edel, M. 2015. Radio Astrometry of The Close Active Binary Hr 5110. Astrophysical Journal. 811 (1): Article ID 33.

The close active binary HR 5110 was observed at six epochs over 26 days using a global very long baseline interferometry array at 15.4 GHz. We used phase referencing to determine the position of the radio centroid at each epoch with an uncertainty significantly smaller than the component separation. After correcting for proper motion and parallax, we find that the centroid locations of all six epochs have barycenter separations consistent with an emission source located on the KIV secondary, and not in an interaction region between the stars or on the F primary. We used a homogeneous power-law gyrosynchrotron emission model to reproduce the observed flux densities and fractional circular polarization. The resulting ranges of mean magnetic field strength and relativistic electron densities are of the order of 10 G and 105cm-3, respectively, in the source region.

dc.publisherInstitute of Physics Publishing
dc.titleRadio Astrometry of The Close Active Binary Hr 5110
dc.typeJournal Article
dcterms.source.titleAstrophysical Journal

Copyright © 2015. The American Astronomical Society. All rights reserved.

curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusOpen access

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