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Title:
VLBI observations of a radio flare of Circinus X-1
Authors:
Preston, R. A.; Morabito, D. D.; Wehrle, A. E.; Jauncey, D. L.; Batty, M. J.; Haynes, R. F.; Wright, A. E.; Nicolson, G. D.
Affiliation:
AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AD(Commonwealth Scientific and Industrial Research Organization, Div. of Radiophysics, Epping, New South Wales, Australia), AE(Commonwealth Scientific and Industrial Research Organization, Div. of Radiophysics, Epping, New South Wales, Australia), AF(Commonwealth Scientific and Industrial Research Organization, Div. of Radiophysics, Epping, New South Wales, Australia), AG(Commonwealth Scientific and Industrial Research Organization, Div. of Radiophysics, Epping, New South Wales, Australia), AH(South African Council for Scientific and Industrial Research, National Institute for Telecommunications Research, Johannesburg, Republic of South Africa)
Publication:
Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 268, May 1, 1983, p. L23-L26. (ApJL Homepage)
Publication Date:
05/1983
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Binary Stars, Flare Stars, Microwave Emission, Radio Sources (Astronomy), Very Long Base Interferometry, X Ray Sources, Angular Resolution, Gas Expansion, Radiant Flux Density, Stellar Mass Accretion, Variable Stars
DOI:
10.1086/184022
Bibliographic Code:
1983ApJ...268L..23P

Abstract

VLBI 2.3 GHz observations of a strong radio flare of the binary star system Circinus X-1 indicate a radio source flaring component angular size of 0.0015-0.015 arcsec. This is equivalent to a linear size of 15-150 AU at the 10 kpc distance of Circinus X-1, although interstellar medium scattering may have enlarged the apparent angular source size. Since the radio source quiescent component, observed prior to the flare, had an angular size greater than 0.2 arcsec (equivalent to more than 2000 AU at 10 kpc), the quiescent radio emission comes from a region much larger than that proposed in recent models for Circinus X-1. The quiescent component appears to be variable on a time scale of years, and is probably fueled by the Circinus X-1 binary system.

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