The 35-day pulse evolution cycle of HER X-1

Details The 35-day pulse evolution cycle of HER X-1 The 35-day pulse evolution cycle of HER X-1

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt........12s&link_type=abstract

Ph.D. Thesis Washington Univ., Seattle, WA.

Astronomy and Astrophysics

Astrophysics

13

Accretion Disks, Precession, Pulsars, Pulsed Radiation, Stellar Radiation, Time Dependence, X Ray Binaries, Astrophysics, Ginga Satellite, Occultation, Pencil Beams, Radiation Distribution

Scientific paper

The pulse shape of the x-ray pulsar Her X-1 exhibits a systematic set of changes during its well known 35-day cycle. The pulse evolution is observed during the ten day long MAIN HIGH state and the five day long SHORT HIGH state and is currently a unique phenomena among the known x-ray pulsars. The pulse shape and its evolution have been observed with an extensive set of Ginga observations taken over the period 1988-1991. The core of the data set consists of a MAIN-SHORT-MAIN HIGH sequence in 1989 in which the evolution of the pulse during the SHORT HIGH state was observed for the first time. The phenomenology of the pulse evolution is documented and several new details have been found. Scaled differences between pairs of pulses are used to isolate the energy or time dependent components of the pulse and to follow the pulse evolution in a quantitative fashion. The existence of similar pulse component are found in the MAIN and SHORT HIGH states and used to align the pulse profiles in phase. The astrophysical interpretation of the pulse evolution cycle is considered. Significant difficulties are found with the observations if free precession of a neutron star with fixed beam pattern is the cause of the pulse evolution. An interpretation involving an occultation of the pulse emitting region around the neutron star by a tilted and precessing disk is favored. A large part of the observed pulse evolution of both the MAIN and SHORT HIGH state can be naturally explained with such an occultation if the beam pattern consists of a spectrally hard pencil beam and a softer fan beam that originates above the neutron star surface and is beamed in the direction antipodal to the pencil beam. The neutron star is also required to be highly inclined (approximately 45 percent) to the binary orbital axis and the radius of the inner disk must be small (less than or equal to 50 RNS).

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