Astronomy and Astrophysics – Astronomy
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.5705d&link_type=abstract
American Astronomical Society, 188th AAS Meeting, #57.05; Bulletin of the American Astronomical Society, Vol. 28, p.913
Astronomy and Astrophysics
Astronomy
Scientific paper
The High Speed Photometer (HSP) on the Hubble Space Telescope observed SS433 at 16 different epochs between 1993 May and November. Polarimetric observations were obtained in a 340 Angstroms FWHM bandpass centered at 2770 Angstroms; photometric observations were made in a bandpass extending between 1400 and 3000 Angstroms. The magnitude of the polarization in the UV is variable, reaching a maximum p >20%, a value as large as that observed in the radio, and unexpectedly larger than that observed in the visible. The mean position angle of the polarization in the UV is 90deg , again similar to the position angle of the polarization observed in the radio and orthogonal to the 0deg position angle observed in the visible. The position angle in the UV varies in phase with the 164 d period in a way similar to that observed in the radio. The polarized radiation we observe in the UV must be emitted from the precessing relativistic jets that ultimately produce the polarized radio emission rather than the scattering region producing the optical polarization. Gyro-synchrotron emission from the material moving at semi-relativistic velocity in the jets is a mechanism which can produce UV radiation with properties consistent with all the observations. SS433 would then be the first astronomical source known to emit gyro-synchrotron radiation at non-radio frequencies. Less than 1.2% of the flux from SS433 between 1400 and 3000 Angstroms is pulsed with a period between 200 mu s and 100 s at 164 d phase psi = 0.131, when the spectral line systems have their smaller maximal separation in radial velocity.
Boyd Patricia T.
Dolan James F.
Fabrika Sergei
Nelson Jonathan M.
Percival Will J.
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