Broad relativistic iron emission line observed in SAX J1808.4–3658
Broad relativistic iron emission line observed in SAX J1808.4–3658
During the 2008 September-October outburst of the accreting millisecond pulsar SAX J1808.4–3658, the source was observed by both Suzaku and XMM-Newton approximately 1 day apart. Spectral analysis reveals a broad relativistic Fe K? emission line which is present in both data sets, as has recently been reported for other neutron star low-mass X-ray binaries. The properties of the Fe K line observed during each observation are very similar. From modeling the Fe line, we determine the inner accretion disk radius to be 13.2 ± 2.5 GM c–2. The inner disk radius measured from the Fe K line suggests that the accretion disk is not very receded in the hard state. If the inner disk (as measured by the Fe line) is truncated at the magnetospheric radius this implies a magnetic field strength of ~3 × 108 G at the magnetic poles, consistent with other independent estimates.
L21-L25
Cackett, E. M.
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Altamirano, D.
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Patruno, A.
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Miller, J. M.
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Reynolds, M.
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Linares, M.
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Wijnands, R.
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2009
Cackett, E. M.
db500756-c971-444b-9677-4ee742b2dac5
Altamirano, D.
d5ccdb09-0b71-4303-9538-05b467be075b
Patruno, A.
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Miller, J. M.
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Reynolds, M.
240b47f0-77d7-43c8-947f-dcc0518f8608
Linares, M.
cea3a79a-1831-4a7f-be41-3bf3b7b25383
Wijnands, R.
382893ee-0e03-45e3-9321-db8b9fc74914
Cackett, E. M., Altamirano, D., Patruno, A., Miller, J. M., Reynolds, M., Linares, M. and Wijnands, R.
(2009)
Broad relativistic iron emission line observed in SAX J1808.4–3658.
The Astrophysical Journal Letters, 694 (1), .
(doi:10.1088/0004-637X/694/1/L21).
Abstract
During the 2008 September-October outburst of the accreting millisecond pulsar SAX J1808.4–3658, the source was observed by both Suzaku and XMM-Newton approximately 1 day apart. Spectral analysis reveals a broad relativistic Fe K? emission line which is present in both data sets, as has recently been reported for other neutron star low-mass X-ray binaries. The properties of the Fe K line observed during each observation are very similar. From modeling the Fe line, we determine the inner accretion disk radius to be 13.2 ± 2.5 GM c–2. The inner disk radius measured from the Fe K line suggests that the accretion disk is not very receded in the hard state. If the inner disk (as measured by the Fe line) is truncated at the magnetospheric radius this implies a magnetic field strength of ~3 × 108 G at the magnetic poles, consistent with other independent estimates.
Text
0901.3142v2.pdf
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Published date: 2009
Organisations:
Astronomy Group, Physics & Astronomy
Identifiers
Local EPrints ID: 358797
URI: http://eprints.soton.ac.uk/id/eprint/358797
ISSN: 2041-8205
PURE UUID: 93622a90-1a4f-4230-a0a5-0ec2987bde4d
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Date deposited: 14 Oct 2013 13:20
Last modified: 16 Nov 2024 02:46
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Contributors
Author:
E. M. Cackett
Author:
A. Patruno
Author:
J. M. Miller
Author:
M. Reynolds
Author:
M. Linares
Author:
R. Wijnands
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