Swift/XRT monitoring of the supergiant fast X-ray transient IGR J18483-0311 for an entire orbital period

P. Romano, L. Sidoli, L. Ducci, G. Cusumano, V. La Parola, C. Pagani, K. L. Page, Jamie A. Kennea, David Nelson Burrows, N. Gehrels, V. Sguera, A. Bazzano

Research output: Contribution to journalArticle

27 Citations (Scopus)

Abstract

IGR J18483-0311 is an X-ray pulsar with transient X-ray activity, belonging to the new class of high-mass X-ray binaries called supergiant fast X-ray transients. This system is one of the two members of this class, together with IGR J11215-5952, where both the orbital (18.52 d) and spin period (21 s) are known. We report on the first complete monitoring of the X-ray activity along an entire orbital period of a supergiant fast X-ray transient. These Swift observations, lasting 28 d, cover more than one entire orbital phase consecutively. They are a unique data set, which allows us to constrain the different mechanisms proposed to explain the nature of this new class of X-ray transients. We applied the new clumpy wind model for blue supergiants developed by Ducci et al. to the observed X-ray light curve. Assuming an eccentricity of e = 0.4, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from 10 18 g to 5 × 10 21 g.

Original languageEnglish (US)
Pages (from-to)1564-1569
Number of pages6
JournalMonthly Notices of the Royal Astronomical Society
Volume401
Issue number3
DOIs
StatePublished - Jan 1 2010

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orbitals
monitoring
x rays
clumps
eccentricity
pulsars
light curve
accretion

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Romano, P. ; Sidoli, L. ; Ducci, L. ; Cusumano, G. ; La Parola, V. ; Pagani, C. ; Page, K. L. ; Kennea, Jamie A. ; Burrows, David Nelson ; Gehrels, N. ; Sguera, V. ; Bazzano, A. / Swift/XRT monitoring of the supergiant fast X-ray transient IGR J18483-0311 for an entire orbital period. In: Monthly Notices of the Royal Astronomical Society. 2010 ; Vol. 401, No. 3. pp. 1564-1569.
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Romano, P, Sidoli, L, Ducci, L, Cusumano, G, La Parola, V, Pagani, C, Page, KL, Kennea, JA, Burrows, DN, Gehrels, N, Sguera, V & Bazzano, A 2010, 'Swift/XRT monitoring of the supergiant fast X-ray transient IGR J18483-0311 for an entire orbital period', Monthly Notices of the Royal Astronomical Society, vol. 401, no. 3, pp. 1564-1569. https://doi.org/10.1111/j.1365-2966.2009.15789.x

Swift/XRT monitoring of the supergiant fast X-ray transient IGR J18483-0311 for an entire orbital period. / Romano, P.; Sidoli, L.; Ducci, L.; Cusumano, G.; La Parola, V.; Pagani, C.; Page, K. L.; Kennea, Jamie A.; Burrows, David Nelson; Gehrels, N.; Sguera, V.; Bazzano, A.

In: Monthly Notices of the Royal Astronomical Society, Vol. 401, No. 3, 01.01.2010, p. 1564-1569.

Research output: Contribution to journalArticle

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T1 - Swift/XRT monitoring of the supergiant fast X-ray transient IGR J18483-0311 for an entire orbital period

AU - Romano, P.

AU - Sidoli, L.

AU - Ducci, L.

AU - Cusumano, G.

AU - La Parola, V.

AU - Pagani, C.

AU - Page, K. L.

AU - Kennea, Jamie A.

AU - Burrows, David Nelson

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AU - Sguera, V.

AU - Bazzano, A.

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N2 - IGR J18483-0311 is an X-ray pulsar with transient X-ray activity, belonging to the new class of high-mass X-ray binaries called supergiant fast X-ray transients. This system is one of the two members of this class, together with IGR J11215-5952, where both the orbital (18.52 d) and spin period (21 s) are known. We report on the first complete monitoring of the X-ray activity along an entire orbital period of a supergiant fast X-ray transient. These Swift observations, lasting 28 d, cover more than one entire orbital phase consecutively. They are a unique data set, which allows us to constrain the different mechanisms proposed to explain the nature of this new class of X-ray transients. We applied the new clumpy wind model for blue supergiants developed by Ducci et al. to the observed X-ray light curve. Assuming an eccentricity of e = 0.4, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from 10 18 g to 5 × 10 21 g.

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