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RX J0524+42: A New Asynchronous Magnetic CV

Published online by Cambridge University Press:  12 April 2016

Robert Schwarz ,
A. D. Schwope ,
A. Staude ,
T. Urrutia ,
A. Rau  and
G. Hasinger
Robert Schwarz
Affiliation:
Universitäts-Sternwarte, Geismarlandstr. 11, 37083 Göttingen, Germany
A. D. Schwope
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
A. Staude
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
T. Urrutia
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
A. Rau
Affiliation:
Max-Planck Institut für extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany
G. Hasinger
Affiliation:
Max-Planck Institut für extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany

Abstract

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Extensive optical photometry of the canditate magnetic CV RX J0524+42 has uncovered three persistent periods at 157, 146 and 136 minutes, which are the manifestation of the orbital motion of the system, the white dwarf spin and a possible side-band period of the latter. Depending on the interpretation of the 146 or the 136 minute period as the spin period, the system is an asynchronous by 7% or 14% (1 – PSpin/Porb), and therefore intermediate between the near-synchronous polars (< 2%) and the two DQ Her stars with long spin periods (EX Hya and V1025 Cen). Sampling the data over the beat period of 1.4 or 0.7 days reveals a prominent double-humped modulation on the spin period for certain fractions of the beat cycle. The phasing of this modulation strongly suggests that either pole switching onto two diametrically opposed accretion sites, or pole migration is operating in this system. With a period right within the period gap, RX J0524+42 is a key object for MCV evolution: it might be the first transition object between the DQ and AM Her subclasses where the white dwarf is currently in the process of synchronisation.

Type
Part 4. Asynchronous Systems
Information
International Astronomical Union Colloquium , Volume 190: Magnetic Cataclysmic Variables , 2004 , pp. 230 - 236
Copyright
Copyright © Astronomical Society of the Pacific 2004

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