We present the result of three BeppoSAX observations of the X-ray binary pulsar A0535+26 in its quiescent state. The source is quite well detected up to 200 keV (6σ detection in the stronger observation). No Iron line is detected in the MECS data (3σ upper limit on its equivalent width of 150 eV). There is evidence of a soft excess below 2 keV. Pulsation is detected in all energy bands up to 10 keV, with a pulsed fraction of not, vert, similar0.5, not varying with energy. There is a marginal detection (4σ) of a cyclotron resonance feature (CRF) at 118±20 keV in the PDS spectrum. During the BeppoSAX observations HDE 245770, the optical counterpart to A0535+26, was monitored spectroscopically and photometrically. These observations show that the Hα and Hβ lines previously observed in absorption returned in emission, indicating that the Be disk formed again. The presence of pulsation and a CRF is a clear indication that accretion onto the polar caps is occurring, and that the propeller mechanism is leaking. The presence of a soft excess could be explained either in terms of thermal emission (kTnot, vert, similar1.2 keV) from the neutron star surface, as observed in other accreting X–ray pulsars, or in terms of an overabundance of Mg in the circumstellar matter.
X-ray/optical observations of A0535+26/HDE 245770 in quiescence
FRONTERA, Filippo;
2004
Abstract
We present the result of three BeppoSAX observations of the X-ray binary pulsar A0535+26 in its quiescent state. The source is quite well detected up to 200 keV (6σ detection in the stronger observation). No Iron line is detected in the MECS data (3σ upper limit on its equivalent width of 150 eV). There is evidence of a soft excess below 2 keV. Pulsation is detected in all energy bands up to 10 keV, with a pulsed fraction of not, vert, similar0.5, not varying with energy. There is a marginal detection (4σ) of a cyclotron resonance feature (CRF) at 118±20 keV in the PDS spectrum. During the BeppoSAX observations HDE 245770, the optical counterpart to A0535+26, was monitored spectroscopically and photometrically. These observations show that the Hα and Hβ lines previously observed in absorption returned in emission, indicating that the Be disk formed again. The presence of pulsation and a CRF is a clear indication that accretion onto the polar caps is occurring, and that the propeller mechanism is leaking. The presence of a soft excess could be explained either in terms of thermal emission (kTnot, vert, similar1.2 keV) from the neutron star surface, as observed in other accreting X–ray pulsars, or in terms of an overabundance of Mg in the circumstellar matter.I documenti in SFERA sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
