A radio pulsar-B star binary in the small magellanic cloud

Kaspi, V. M.; Johnston, S.; Manchester, R. N.; Bailes, M.; Bell, J. F.; Bessell, M. S.; Lyne, A. G.; D’Amico, N.

doi:10.1063/1.45960

Cited by 4 publications

(8 citation statements)

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“…Using ROSAT PSPC data Finley et al (1992) showed that PSR 0656ϩ14 was pulsed at the radio period, and Ö gelman (1995) showed that the pulsed fraction varied over the 0.1-2.4 keV energy range nearing a pulsed fraction of 20% at the highest energies. Arzoumanian et al (1992), and Kaspi et al (1994). the pulsed fraction varied from 8% to 80% and settled to 40% at higher energies.…”

Section: Timingmentioning

confidence: 91%

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Heated Polar Caps in PSR 0656+14 and PSR 1055−52

Greiveldinger

Camerini

Fry

et al. 1996

The Astrophysical Journal

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We present new ASCA observations covering the 0.5-10 keV X-ray range of the cooling neutron star candidates PSR 0656ϩ14 and PSR 1055Ϫ52. Previous ROSAT observations had shown that two-component models, either two blackbodies or a blackbody plus a power-law, provided the best spectral fits to their X-ray emission. The combined ASCA and ROSAT spectrum of PSR 0656ϩ14 reveals two blackbody components with T 2 8 ϫ 10 5 K and T 2 1.5 ϫ 10 6 K and shows evidence that a power-law component is needed to account for higher energy photons. This three-component fit gives a reduced 2 that is half the value of a more conventional two component fit (1.3 as compared to 2.4). The fit to the combined spectrum for PSR 1055Ϫ52 yields a two-blackbody fit with T 2 8 ϫ 10 5 K and T 2 3.7 ϫ 10 6 K. Our results favor the existence of a hot polar cap in each of these pulsars with the ratio of the polar cap area to the neutron star surface area being 7 ϫ 10 Ϫ3 and 3 ϫ 10 Ϫ5 for PSR 0656ϩ14 and PSR 1055Ϫ52, respectively. The results are compared to models that make predictions of polar cap heating processes.

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Section: Timingmentioning

confidence: 91%

“…PSR 1055Ϫ52 was analyzed according to the ephemeris shown in Table 1 (Kaspi et al 1994). For the entire energy range, we determine that the 3 upper limit on the pulsed fraction is 87%.…”

Section: Timingmentioning

confidence: 99%

Heated Polar Caps in PSR 0656+14 and PSR 1055−52

Greiveldinger

Camerini

Fry

et al. 1996

The Astrophysical Journal

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“…Bell (1994) identified its optical companion as a 16th magnitude, 11 M ⊙ , B1 main‐sequence star. The orbital period (51 d) of PSR J0045‐7319 was found by Kaspi et al (1993) through the Doppler modulation of the pulse period.…”

Section: Temporal Properties Of Individual Sourcesmentioning

confidence: 99%

“… [1]: Kaspi et al (1993); [2]: Schmidtke & Cowley (2006); [3]: Coe et al (2005); [4]: McGowan et al (2008); [5]: Cowley & Schmidtke (2004); [6]: Schmidtke, Cowley & Udalski (2006); [7]: Schmidtke et al (2004); [8]: Edge (2005a); [9]: McGowan et al (2008); [10]: Schmidtke & Cowley (2005b); [11]: Schmidtke & Cowley (2007b); [12]: McGowan et al (2007); [13]: Edge et al (2005b); [14]: Coe et al (2009); [15]: Schurch et al (2009); [16]: Udalski & Coe (2008) …”

Section: Introductionmentioning

confidence: 99%

Very long-term optical variability of high-mass X-ray binaries in the Small Magellanic Cloud

Rajoelimanana

Charles

Udalski

2011

Monthly Notices of the Royal Astronomical Society

121

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We have studied the very long‐term temporal properties of the optical emission from Be X‐ray binaries (BeX) in the Small Magellanic Cloud (SMC) over a ∼16 yr baseline, using light curves from the MAssive Compact Halo Objects (MACHO) and Optical Gravitational Lensing Experiment (OGLE) data bases. All the BeX in our sample display superorbital variations, many of them quasi‐periodic on time scales of ∼200–3000 d. These long‐term variations are believed to be related to the formation and depletion of the circumstellar disc around the Be star, and we compare and contrast their behaviour with that of the Large Magellanic Cloud (LMC)’s prototypical BeX, A0538‐66. The great majority of sources show a correlation of outburst amplitude with brightness (the opposite to that seen in A0538‐66) although the amplitudes are mostly small (≤0.1 mag). We suggest this is an orbital inclination effect. In addition, we have also detected many of their optical orbital periodicities, visible as a series of precisely regular outbursts. Furthermore, the amplitude of these periodic outbursts can vary through the long‐term superorbital cycle, and we discuss mechanisms which can produce this effect, as well as examining an apparent correlation between these periodicities. As a by‐product of this variation survey we have compiled a list of all the reported SMC BeX orbital and superorbital periodicities at optical and X‐ray wavelengths.

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“…Bell (1994) identified its optical companion as a 16th magnitude, 11 M⊙, B1 main-sequence star. The orbital period (51 d) of PSR J0045-7319 was found by Kaspi et al (1993) through the Doppler modulation of the pulse period.…”

Section: Temporal Properties Of Individual Sourcesmentioning

confidence: 99%

Very Long-term Optical Variability of High Mass X-ray Binaries in the SMC

Rajoelimanana,

Charles,

Udalski

2010

Preprint

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We have studied the very long-term temporal properties of the optical emission from Be X-ray binaries (BeX) in the Small Magellanic Cloud over a ∼ 16 yr baseline, using light curves from the MACHO and OGLE databases. All the BeX in our sample display superorbital variations, many of them quasi-periodic on timescales of ∼ 200-3000 d. These long-term variations are believed to be related to the formation and depletion of the circumstellar disc around the Be star and we compare and contrast their behaviour with that of the LMC's prototypical BeX, A0538-66. The great majority of sources show a correlation of outburst amplitude with brightness (the opposite to that seen in A0538-66) although the amplitudes are mostly small ( 0.1 mag). We suggest this is an orbital inclination effect. In addition, we have also detected many of their optical orbital periodicities, visible as a series of precisely regular outbursts. Furthermore, the amplitude of these periodic outbursts can vary through the long-term superorbital cycle, and we discuss mechanisms which can produce this effect, as well as examining an apparent correlation between these periodicities. As a by-product of this variation survey we have compiled a list of all the reported SMC BeX orbital and superorbital periodicities at optical and X-ray wavelengths.

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A radio pulsar-B star binary in the small magellanic cloud

Cited by 4 publications

References 0 publications

Heated Polar Caps in PSR 0656+14 and PSR 1055−52

Heated Polar Caps in PSR 0656+14 and PSR 1055−52

Very long-term optical variability of high-mass X-ray binaries in the Small Magellanic Cloud

Very Long-term Optical Variability of High Mass X-ray Binaries in the SMC

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