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X–ray/optical observations of A0535+26/HDE 245770 in quiescence

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Title: X–ray/optical observations of A0535+26/HDE 245770 in quiescence
Authors: Orlandini, M.1, Bartolini, C.2, Campana, S.3, Del Sordo, S.4, de Martino, D.5, Frontera, F.1, Guarnieri, A.2, Israel, G.6, Masetti, N.1, Palazzi, E.1, Piccioni, A.2, Santangelo, A.4, Stella, L.6
Source: Nuclear Physics B Proceedings Supplement. Jun2004, Vol. 132 Issue 1-3, p476-485. 10p.
Subjects: X-rays, Photometry, Stellar oscillations, Resonance
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 ∼0.5, 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 (kT∼1.2 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. [Copyright &y& Elsevier]
Copyright of Nuclear Physics B Proceedings Supplement is the property of Elsevier B.V. and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: X–ray/optical observations of A0535+26/HDE 245770 in quiescence
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  Data: <searchLink fieldCode="AR" term="%22Orlandini%2C+M%2E%22">Orlandini, M.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Bartolini%2C+C%2E%22">Bartolini, C.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Campana%2C+S%2E%22">Campana, S.</searchLink><relatesTo>3</relatesTo><br /><searchLink fieldCode="AR" term="%22Del+Sordo%2C+S%2E%22">Del Sordo, S.</searchLink><relatesTo>4</relatesTo><br /><searchLink fieldCode="AR" term="%22de+Martino%2C+D%2E%22">de Martino, D.</searchLink><relatesTo>5</relatesTo><br /><searchLink fieldCode="AR" term="%22Frontera%2C+F%2E%22">Frontera, F.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Guarnieri%2C+A%2E%22">Guarnieri, A.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Israel%2C+G%2E%22">Israel, G.</searchLink><relatesTo>6</relatesTo><br /><searchLink fieldCode="AR" term="%22Masetti%2C+N%2E%22">Masetti, N.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Palazzi%2C+E%2E%22">Palazzi, E.</searchLink><relatesTo>1</relatesTo><br /><searchLink fieldCode="AR" term="%22Piccioni%2C+A%2E%22">Piccioni, A.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Santangelo%2C+A%2E%22">Santangelo, A.</searchLink><relatesTo>4</relatesTo><br /><searchLink fieldCode="AR" term="%22Stella%2C+L%2E%22">Stella, L.</searchLink><relatesTo>6</relatesTo>
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  Data: <searchLink fieldCode="JN" term="%22Nuclear+Physics+B++Proceedings+Supplement%22">Nuclear Physics B Proceedings Supplement</searchLink>. Jun2004, Vol. 132 Issue 1-3, p476-485. 10p.
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  Data: <searchLink fieldCode="DE" term="%22X-rays%22">X-rays</searchLink><br /><searchLink fieldCode="DE" term="%22Photometry%22">Photometry</searchLink><br /><searchLink fieldCode="DE" term="%22Stellar+oscillations%22">Stellar oscillations</searchLink><br /><searchLink fieldCode="DE" term="%22Resonance%22">Resonance</searchLink>
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  Label: Abstract
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  Data: 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 ∼0.5, not varying with energy. There is a marginal detection (4σ) of a cyclotron resonance feature (CRF) at <f>118±20</f> 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 <f>Hα</f> and <f>Hβ</f> 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 (<f>kT∼1.2</f> 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. [Copyright &y& Elsevier]
– Name: AbstractSuppliedCopyright
  Label:
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  Data: <i>Copyright of Nuclear Physics B Proceedings Supplement is the property of Elsevier B.V. and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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        Value: 10.1016/j.nuclphysbps.2004.04.082
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      – SubjectFull: Stellar oscillations
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