Cyclotron spectroscopy of HU Aquarii

Details Cyclotron spectroscopy of HU Aquarii Cyclotron spectroscopy of HU Aquarii

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...402..201s&link_type=abstract

Astronomy and Astrophysics, v.402, p.201-209 (2003)

Astronomy and Astrophysics

Astrophysics

5

Accretion, Accretion Disks, Stars: Binaries: Eclipsing, Magnetic Fields, Stars: Individual: Hu Aqr

Scientific paper

We present the results of a combined analysis of low-resolution spectroscopy and high-speed optical photometry of the bright eclipsing polar HU Aqr, obtained in its high accretion state. Cyclotron harmonic emission in a field of B^simeq 34 MG became evident and could be traced through the whole optical bright phase. The cyclotron harmonics display an asymmetric motion as a function of phase which requires a certain forward tilt of the magnetic field lines in the emission region. The optical bright phase is more extended than the bright phase in soft X-rays suggesting a more extended emission region. Also, ingress into and egress from the optical eclipse last much longer in the optical than at X-ray wavelengths. These observations require the existence of an accretion arc with total extent of about 20°. The soft X-ray accretion spot is located at the far end of the arc, where the bulk of matter is accreted. The arc is likely to be more extended than the foot-line of field lines connecting to the ballistic accretion stream in a dipolar geometry. This together with the required tilt of the accreting field lines suggest a more complex magnetic geometry than a simple dipole.
Based on observations at the European Southern Observatory, Chile, at the ESO 1 m telescope and the ESO/MPG 2.2 m telescope in Max-Planck-time.

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