Evolution of the optical and hard X-ray activity of AM Her in a season dominated by the high states

Original Article


The long-term activity of AM Her, the prototype of polars, consists of interchanging high and low states. This analysis uses the data from the BAT/Swift, MAXI/ISS, and AAVSO data archives (including long CCD \(V\)-band night series) for investigating the relation of the time evolution of intensities in the hard X-ray, medium/hard X-ray, and the optical bands on super-orbital timescale in a season dominated by the long high-state episodes. The observations mapped the relation of the cyclotron and bremsstrahlung luminosities in such episodes. Although an increase of intensity of the cyclotron emission is generally accompanied by a brightening of the bremsstrahlung component, this relation differs for the individual high-state episodes. These variations were accompanied by the large changes of the optical modulation. In my view, all of these variations suggest variations of the dimensions and structure of the cyclotron emitting region(s), not only the changes of the mass accretion rate. The activity during a decline (much less steep than the state transition) from an initial very bright peak can be explained by a gradual evolution of the conditions in stratified shock regions in a single high state episode. The observed behavior in the neighboring high-state episodes is also important for explaining the mechanisms which cause the low state between them. In the interpretation, some low-state episodes cause that AM Her develops a different accretion mode than the one before entering the low state. Each high-state episode is a complex phenomenon in the history of accretion in this system.


X-rays: binaries Radiation mechanisms: general Novae, cataclysmic variables Stars: individual (AM Her) 



This study was supported by grant 13-39464J provided by the Grant Agency of the Czech Republic. The public data from Swift/BAT transient monitor provided by the Swift/BAT team were used. This research has also made use of the Palermo BAT Catalogue and database operated at INAF-IASF Palermo. I also used public data from the MAXI data archive. I acknowledge the MAXI team for support. I also acknowledge with thanks the variable star observations from the AAVSO International Database (Massachusetts, USA) contributed by observers worldwide and used in this research.


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Copyright information

© Springer Science+Business Media Dordrecht 2016

Authors and Affiliations

  1. 1.Astronomical InstituteThe Czech Academy of SciencesOndřejovCzech Republic
  2. 2.Faculty of Electrical EngineeringCzech Technical University in PraguePragueCzech Republic

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