Anticorrelation between X-ray luminosity and pulsed fraction in the Small Magellanic Cloud pulsar SXP 1323

Yang, Jun; Zezas, A.; Coe, M. J.; Drake, J. J.; Hong, Jae Sub; Laycock, S.; Wik, Daniel R.

doi:10.1093/mnrasl/sly085

Cited by 19 publications

(17 citation statements)

References 31 publications

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“…The small magellanic cloud (SMC) is a dwarf irregular galaxy near the Milky Way at a distance of about 62 kpc (Graczyk et al ; Scowcroft et al ). It contains a large and active population of X‐ray binaries (Christodoulou et al ; Coe & Kirk ; Galache et al ; Haberl & Sturm ; Klus et al ; Townsend et al ; Yang et al ; Yang et al ; Yang et al ). The most numerous HMXB species in current catalogs (Yang et al ) are Be‐HMXBs, where the companion is a Be star (Reig ).…”

Section: X‐ray Pulsars In the Small Magellanic Cloudmentioning

confidence: 99%

Evolution of high‐mass X‐ray binaries in the small magellanic cloud

et al. 2019

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To understand the progenitor of rotation-powered pulsars, we compare them with accreting High-Mass X-ray binary pulsars, (hereafter X-ray pulsars), in the small magellanic cloud. The diagram of spin period vs. period derivative shows that isolated neutron stars could be evolved from X-ray pulsars. The pulsars with long spin period might spin up to 0.001-1 s. The binary orbit is disrupted by a third body in the universe, and the binaries are detached. Therefore, some of the pulsars become isolated neutron stars.

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Section: X‐ray Pulsars In the Small Magellanic Cloudmentioning

confidence: 99%

Evolution of high‐mass X‐ray binaries in the small magellanic cloud

et al. 2019

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“…However, with the preferred 3C50, this behavior is not replicated. The energy-resolved PF behavior is, of course, dependent on the definition of PF used (see examples byYang et al 2018). For example, if we define PF as PF = (R Max − R Min )/(R Max + R…”

mentioning

confidence: 99%

RX J0529.8−6556: a BeXRB pulsar with an evolving optical period and out of phase X-ray outbursts

Treiber

Vasilopoulos

Bailyn

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We report the results of eROSITA and NICER observations of the June 2020 outburst of the Be/X-ray binary pulsar RX J0529.8−6556 in the Large Magellanic Cloud, along with the analysis of archival X-ray and optical data from this source. We find two anomalous features in the system’s behavior. First, the pulse profile observed by NICER during maximum luminosity is similar to that observed by XMM-Newton in 2000, despite the fact that the X-ray luminosity was different by two orders of magnitude. By contrast, a modest decrease in luminosity in the 2020 observations generated a significant change in pulse profile. Second, we find that the historical optical outbursts are not strictly periodic, as would be expected if the outbursts were triggered by periastron passage, as is generally assumed. The optical peaks are also not coincident with the X-ray outbursts. We suggest that this behavior may result from a misalignment of the Be star disc and the orbital plane, which might cause changes in the timing of the passage of the neutron star through the disc as it precesses. We conclude that the orbital period of the source remains unclear.

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“…The X-ray Multi-Mirror Mission (XMM-Newton) observation in 2003 has the longest exposure time. We used the standard procedure (see [20][21][22][23][24]) to extract the source. The folded light curve shows two double peaks and double troughs.…”

Section: Light Curves and Spectramentioning

confidence: 99%

TV Cassiopeiae with Chandra and XMM–Newton X-ray Observations

Yang

Drake

Wik

et al. 2019

Recent Progress in Relativistic Astrophysics

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TV Cassiopeia (TV Cas) is a well-known eclipsing Algol-type binary comprising a B9V primary and F7 IV secondary in an orbit with a period of 1.81 days, together with a purported low-mass companion in a wide orbit. Despite the considerable attention TV Cas has received in optical and UV bands, no X-ray analysis has been reported. Chandra has detected TV Cas six times and XMM–Newton observed it twice, all serendipitously during observations of the starburst galaxy IC 10. We have put all the X-ray data together to investigate its coronal morphology and spectral properties. We use the X-ray light curves and eclipses to probe the emitting geometry and the X-ray spectra at different epochs to investigate the activity mechanisms and test speculation that TV Cas undergoes significant mass transfer episodes.

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Anticorrelation between X-ray luminosity and pulsed fraction in the Small Magellanic Cloud pulsar SXP 1323

Cited by 19 publications

References 31 publications

Evolution of high‐mass X‐ray binaries in the small magellanic cloud

Evolution of high‐mass X‐ray binaries in the small magellanic cloud

RX J0529.8−6556: a BeXRB pulsar with an evolving optical period and out of phase X-ray outbursts

TV Cassiopeiae with Chandra and XMM–Newton X-ray Observations

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