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Cyclotron resonance scattering features observed in the spectra of some X-raypulsars show significant changes of the line energy with the pulsar luminosity.At high luminosities, these variations are often associated with the onset andgrowth of the accretion column, which is believed to be the origin of theobserved emission and of the cyclotron lines. However, this scenario inevitablyimplies large gradient of the magnetic field strength within the line-formingregion, which makes the formation of the observed line-like featuresproblematic. Moreover, the observed variation of the cyclotron line energy ismuch smaller than could be anticipated for the corresponding luminositychanges. We argue here that a more physically realistic situation is that thecyclotron line forms when the radiation emitted by the accretion column isreflected from the neutron star surface, where the gradient of the magneticfield strength is significantly smaller. We develop here the reflection modeland apply it to explain the observed variations of the cyclotron line energy ina bright X-ray pulsar V 0332+53 over a wide range of luminosities.

A reflection model for the cyclotron lines in the spectra of X-ray pulsars