Multi-Wavelength Properties of the 2021 Periastron Passage of PSR B1259-63

Chernyakova, M.; Malyshev, D.; Soelen, B. van; O’Sullivan, Shane; Sobey, C.; Tsygankov, Sergey S.; Green, Jacob; Kirwan, Matthew; Santangelo, A.; Pühlhofer, G.; Monageng, I. M.

doi:10.3390/universe7070242

Cited by 24 publications

(36 citation statements)

References 37 publications

(28 reference statements)

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“…If ∆TS > 9, a cutoff is significantly preferred). This is consistent with the results reported in Chernyakova et al [9,14]. Using a power-law with exponentially cut-off model, the spectra index shows significant change between the 2014 and 2017 periastron.…”

Section: Resultssupporting

confidence: 92%

“…The main GeV flux peak appeared later and later in the last four periastron passages, as shown in Figure 3, occuring about 90 days after periastron in 2021. This delay pattern is consistent with the trend reported in Chang et al [11], and it is not being observed in any other energy bands [14]. Another feature of the light curves is that there are multiple bright flares during each periastron passage.…”

Section: Resultssupporting

confidence: 92%

“…A 95% confidence upper limit was calculated when PSR B1259-63 was not significantly detected (TS < 9). The results are consistent with those reported in the 0.1-10 GeV energy band in Chernyakova et al [14]. For a comparison to previous periastron passages, we re-analyzed all the Fermi-LAT data during its 2010, 2014 and 2017 periastron passages with the latest IRFs and the latest software package.…”

Section: Resultssupporting

confidence: 88%

“…Chang et al [11] also reported a time delay of the main GeV flare by comparing the three previous periastron passages (2010, 2014 and 2017). The most recent multi-wavelength observations which covered a period of more than 100 days around the 2021 periastron show substantial differences from the previously observed passages [14]. Besides the features in other energy bands, such as the weaker X-ray flux during peaks and the never before observed third X-ray peak, Chernyakova et al [14] also confirmed the delay of the GeV flare reported by Chang et al [11] in 2018.…”

Section: Introductionmentioning

confidence: 56%

“…It has a large field of view (about 20% of the sky) and has been scanning the sky continuously since August 2008. Fermi-LAT observed PSR B1259-63 during its periastron period in 2010 [16,17], 2014 [18], 2017 [11][12][13] and 2021 [14,[19][20][21].…”

Section: Observations and Data Analysismentioning

confidence: 99%

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Fermi-LAT Observation of PSR B1259-63 during Its 2021 Periastron Passage

et al. 2021

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PSR B1259-63 is a γ-ray binary system, where the compact object is a pulsar. The system has an orbital period of 1236.7 days and shows peculiar γ-ray flares (in 100 MeV–300 GeV) after its periastron time. We analyzed the Fermi-LAT observation of PSR B1259-63 during its latest periastron passage, as well as its previous three periastrons. The bright GeV flares started about 60 days after the periastron epoch in 2021. This delay is larger than that around the 2017 periastron and much larger than earlier periastrons. The delay of the GeV flux peak time in each periastron passage is apparent in our results. We discussed the possible origin of this delay and made a prediction of the GeV flux peak time in next periastron passage, based on observation of the previous delays.

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Section: Resultssupporting

confidence: 92%

Section: Resultssupporting

confidence: 92%

Section: Resultssupporting

confidence: 88%

Section: Introductionmentioning

confidence: 56%

Section: Observations and Data Analysismentioning

confidence: 99%

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Fermi-LAT Observation of PSR B1259-63 during Its 2021 Periastron Passage

et al. 2021

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Optical spectroscopy of the Be/black hole binary MWC 656 ‐ interaction of a black hole with a circumstellar disc

et al. 2022

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We present new spectroscopic observations of the Be/black hole binary MWC 656 obtained during the period 2015–2021. We measure the equivalent width of Hα (EWα), Hβ (EWβ$$ {EW}_{\beta } $$), and the distance between the peaks of Hα (normalΔVα$$ \Delta {V}_{\alpha } $$), Hβ (normalΔVβ$$ \Delta {V}_{\beta } $$), and FeII (normalΔVFeII$$ \Delta {V}_{\mathrm{FeII}} $$) lines. Combining new and old data, we find that: (1) the density of the circumstellar disc of MWC 656 (normalΔVα$$ \Delta {V}_{\alpha } $$ versus EWα$$ {EW}_{\alpha } $$ diagram) is similar to the Be stars. For the Be stars, we find the relation normalΔVβ=0.999normalΔVα+62.4$$ \Delta {V}_{\beta }=0.999\Delta {V}_{\alpha }+62.4 $$ km s−1, and the position of MWC 656 corresponds to the average behavior of the Be stars. This means that the presence of the black hole does not change the overall structure of the circumstellar disc; (2) the periodogram analysis indicates modulation of EWα$$ {EW}_{\alpha } $$ with a period 60.4±0.4$$ 60.4\pm 0.4 $$ days, which is identical to the binary orbital period. The maxima of EWα$$ {EW}_{\alpha } $$ and EWβ$$ {EW}_{\beta } $$ are around periastron (phase zero); (3) around orbital phase zero, normalΔVβ$$ \Delta {V}_{\beta } $$ and normalΔVFeII$$ \Delta {V}_{FeII} $$ decrease by about 30$$ 30 $$ km s−1. This suggests that we observe an increase of the circumstellar disc size induced by the periastron passage of the black hole and that the entire circumstellar disc pulsates with the orbital period with relative amplitude of 10–20%. The observations also indicate, that the reason for the black hole in MWC 656 to be in deep quiescence is a very low efficiency of accretion (∼2×10−6$$ \sim 2\times {10}^{-6} $$).

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Repeating fast radio burst 20201124A originates from a magnetar/Be star binary

et al. 2022

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Fast radio bursts (FRBs) are cosmic sources emitting millisecond-duration radio bursts. Although several hundreds FRBs have been discovered, their physical nature and central engine remain unclear. The variations of Faraday rotation measure and dispersion measure, due to local environment, are crucial clues to understanding their physical nature. The recent observations on the rotation measure of FRB 20201124A show a significant variation on a day time scale. Intriguingly, the oscillation of rotation measure supports that the local contribution can change sign, which indicates the magnetic field reversal along the line of sight. Here we present a physical model that explains observed characteristics of FRB 20201124A and proposes that repeating signal comes from a binary system containing a magnetar and a Be star with a decretion disk. When the magnetar approaches the periastron, the propagation of radio waves through the disk of the Be star naturally leads to the observed varying rotation measure, depolarization, large scattering timescale, and Faraday conversion. This study will prompt to search for FRB signals from Be/X-ray binaries.

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Multi-Wavelength Properties of the 2021 Periastron Passage of PSR B1259-63

Cited by 24 publications

References 37 publications

Fermi-LAT Observation of PSR B1259-63 during Its 2021 Periastron Passage

Fermi-LAT Observation of PSR B1259-63 during Its 2021 Periastron Passage

Optical spectroscopy of the Be/black hole binary MWC 656 ‐ interaction of a black hole with a circumstellar disc

Repeating fast radio burst 20201124A originates from a magnetar/Be star binary

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