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The Be/X-Ray System HDE 245770/A0535+26 in an Active Phase

Published online by Cambridge University Press:  23 September 2016

C. Bartolini
Affiliation:
Istituto Astronomico, Universita di Bologna, (Italy)
M. Burger
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, (Belgium)
E.L. van Dessel
Affiliation:
Royal Belgian Observatory, Uccle, (Belgium)
F. Giovannelli
Affiliation:
Istituto di Astrofisica Spaziale, CNR, Frascati, (Italy)
A. Guarnieri
Affiliation:
Istituto Astronomico, Universita di Bologna, (Italy)
C. de Loore
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, (Belgium)
A. Piccioni
Affiliation:
Istituto di Astrofisica Spaziale, CNR, Frascati, (Italy)

Extract

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The principal aim is to report on the sudden appearance and disappearance of (mainly) Fe II emission lines in the Be/X-ray system HDE 24-5770/ A0535+26, about 24 days before an X-ray outburst was observed. The system is characterized as an 09-7 Ille star of mass 20-25 M, accompanied by a neutron star (X-ray pulse period ≃104 s), with orbital period -110 d, eccentricity > 0.3; for a more complete description see Giovannelli et al. (1985) or de Loore et al. (1984). X-ray outbursts have been observed recurrently, obviously connected with periastron passage of the neutron star triggering gas infall onto it. The observed X-ray outbursts are of varied strength, from barely detectabl to 3 Crab units at peak (Nagase et al. (1982), Giovannelli et al. (1984)). A weak X-ray event took place on December 13, 1981.

Type
III. The Circumstellar Gas
Copyright
Copyright © Cambridge University Press 1987

References

Giovannelli, F. et al., 1984, in “X-ray Astronomy ‘84”, Oda, M. and Giacconi, R (eds.), p.205 Google Scholar
Giovannelli, F. et al., 1985, in “Multifrequency Behaviour of Galactic Accreting Sources”, Giovannelli, F. (ed.), p.284 Google Scholar
de Loore, C. et al., 1984, Astron.Astrophys. 141, 279 Google Scholar
Nagase, F. et al., 1982, Astrophys.J. 263, 814 Google Scholar