2009
DOI: 10.1051/0004-6361:200811396
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Phase-resolved spectroscopy of the accreting millisecond X-ray pulsar SAX J1808.4-3658 during the 2008 outburst

Abstract: Aims. We obtained phase-resolved spectroscopy of the accreting millisecond X-ray pulsar SAX J1808.4-3658 during its outburst in 2008 to find a signature of the donor star, constrain its radial velocity semi-amplitude (K 2 ), and derive estimates for the pulsar mass. Methods. Using Doppler images of the Bowen region, we find a significant (≥8σ) compact spot at a position where the donor star is expected. If this is a signature of the donor star, we measure K em = 248 ± 20 km s −1 (1σ confidence), which represen… Show more

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Cited by 14 publications
(20 citation statements)
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“…This is the case of Bowen fluorescence lines in LMXBs. It is interesting to compare J2215 with the accreting millisecond pulsars SAXJ1808.4-3658 and XTEJ1814-338, with Bowenline outburst K corrections of f K =0.90 and 0.81, respectively (Cornelisse et al 2009;Wang et al 2017 Horne & Schneider 1989) and we find f irr ∼50 (using the stellar parameters in Schmidt et al 1995). Similarly, we find f irr ∼140 for the PCEB NNSer, with a reported f K =0.88 (Balmer lines, Parsons et al 2010).…”
Section: A Broader Look At Irradiation: K Correction and Deep Heatingsupporting
confidence: 60%
“…This is the case of Bowen fluorescence lines in LMXBs. It is interesting to compare J2215 with the accreting millisecond pulsars SAXJ1808.4-3658 and XTEJ1814-338, with Bowenline outburst K corrections of f K =0.90 and 0.81, respectively (Cornelisse et al 2009;Wang et al 2017 Horne & Schneider 1989) and we find f irr ∼50 (using the stellar parameters in Schmidt et al 1995). Similarly, we find f irr ∼140 for the PCEB NNSer, with a reported f K =0.88 (Balmer lines, Parsons et al 2010).…”
Section: A Broader Look At Irradiation: K Correction and Deep Heatingsupporting
confidence: 60%
“…As can be seen, our fitting results are consistent with the analytical expectations. If K comp = 299±23 km s −1 instead, as reported by Cornelisse et al (2009), the M ns -i relation is expected to shift toward lower values. We explored this effect by fitting our model using K Bowen = 248 ± 20 km s −1 (Cornelisse et al 2009) as a prior.…”
Section: Influence Of the Companion Radial Velocitymentioning
confidence: 75%
“…If K comp = 299±23 km s −1 instead, as reported by Cornelisse et al (2009), the M ns -i relation is expected to shift toward lower values. We explored this effect by fitting our model using K Bowen = 248 ± 20 km s −1 (Cornelisse et al 2009) as a prior. As expected, we found similar results but noticeably i = 45 ± 5 • and M ns = 0.58 +0.20 −0.14 M ⊙ (both uncertainties are 1σ), which are both smaller than the values obtained using the Elebert et al (2009) measurement as the prior.…”
Section: Influence Of the Companion Radial Velocitymentioning
confidence: 75%
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